I Scientific Highlights(April 2005 - March 2006)

1. Numerous luminous buried AGNs in ultraluminous infrared galaxies ………………………………………… IMANISHI et al.
2. Photospheric and Chromospheric Vector Magnetograph Systems Installed into the
Solar Flare Telescope ………………………………………………………………… HANAOKA, Flare Telescope Team
3. Preflare Nonthermal Emission Observed in Microwaves and Hard X-Rays ………………………………………… ASAI et al.
4. The Unique Type Ib Supernova 2005bf: A WN Star Explosion Model for Peculiar
Light Curves and Spectra…………………………………………………………………………………TOMINAGA et al.
5. Same-Beam Differential VLBI Technology Using Two Satellites of the SELENE Spacecraft …………………………LIU et al.
6. The Relation between the Two-Point and Three-Point Correlation Functions in the
Nonlinear Gravitational Clustering Regime………………………………………………………………KOYAMA, YANO
7. Observational Pursuit for Population III Star …………………………………………………………………… NAGAO et al.
8. Metallicity Evolution of Active Galactic Nuclei ………………………………………………………………… NAGAO et al.
9. One Solar Cycle Observations of Prominence Activities Using the Nobeyama
Radioheliograph 1992-2004…………………………………………………………………………………SHIMOJO et al.
10. Discovery of an Extrasolar Planet HD149026 b with a Large Core ………………………………………………… SATO et al.
11. Local Gravity From Lunar Prospector Tracking Data: Results for Mare Serenitatis ………………………… GOOSSENS et al.
12. Metal Abundances of Meteoroids in Meteor Showers: Leonids vs Geminid …………………………………… KASUGA et al.
13. Observations of Star-forming Galaxies at z ~ 3 with ESO VLT: Escape Fractionof Ionizing Photons and Stellar Populations ……………………………………………………………………IWATA et al.
14. Three-Dimensional Motion of Plasmas Associated with a Coronal Mass Ejection
Observed with NOrikura Green-line Imaging System (NOGIS)……………………………………………… SUZUKI et al.
15. Three-Mirror Anastigmat Telescope Design for an ELT ………………………………………………………… NARIAI, IYE
16. SMA Observations of Submm Bright Galaxies at High-z …………………………………………………………………IONO
17. A Coronagraphic Search for Brown Dwarfs and Planets around Nearby Stars ……………………………… NAKAJIMA et al.
18. Morphological Classification of Galaxies using Photometric Parameters: theConcentration index versus the Coarseness parameter ……………………………………………………YAMAUCHI et al.
19. Dense and Warm Molecular Gas Observations of NGC 6240 with the Nobeyama
Millimeter Array and the RAINBOW Interferometer …………………………………………………… NAKANISHI et al.
20. Clustering of Lyman Break Galaxies at z＝4 and 5 in The Subaru Deep Field:
Luminosity Dependence of The Correlation Function Slope ……………………KASHIKAWA and Subaru Deep Field team
21. Discovery of HE 1327-2326, the most iron-deficient star known ………………………………………………………… AOKI
22. Sulfur and Zinc Abundances of Galactic Disk/Halo Stars : Application of Extensive
Detailed Non-LTE Calculations …………………………………………………………………………… TAKEDA et al.
23. Rotating Molecular Gas Associated with a Silhouette Disk at the Center of the Radio Galaxy 3C 31 …………… OKUDA et al.
24. Installation of Seismic Attenuation System (SAS) to Gravitational Wave Detector TAMA300 ……………… FUJIMOTO et al.
25. Development of a laser interferometric high-precision angle sensor for the JASMINE satellite………………………ARAI et al.
26. Velocity Drift of Water Maser Features of NGC 4258 ………………………………………………………YAMAUCHI et al.
27. Nobeyama Millimeter Array Observations of GRB 030329: a Decay of Afterglow with
Bumps and Molecular Gas in the Host Galaxy ……………………………………………………………… KOHNO et al.
28. A 385-500 GHz Sideband-separating (2SB) SIS Mixer Based on a Waveguide Split-Block Coupler ……… KAMIKURA et al.
29. Phoenicids in 1956 Revisited ………………………………………………………………………………WATANABE et al.
30. Size Distribution of Faint Jovian L4-Trojan Asteroids ………………………………………………YOSHIDA, NAKAMURA
31. Near-Infrared Imaging Survey of Bok Globules: Density Structure ……………………………………………KANDORI et al.
32. Extremely high-velocity gas in a merging galaxy Arp 220 revealed with ammonia
absorption lines………………………………………………………………………………………………TAKANO et al.
33. Discovery of Circumstellar Disk around a Massive Protostar by the Subaru Telescope …………………………… JIANG et al.
34. Observations of Giant Silhouette Envelope Object M17-SO1 ………………………………………………………SAKO et al.
35. Forthcoming Launch of the SOLAR-B Spacecraft ……………………………………………………… KATSUKAWA et al.

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36. Expanding Radio Lobe Revealed by VSOP Observations ……………………………………………………… ASADA et al.
37. Near-infrared deep imaging of Subaru Supe Deep Field using Adaptive Optics…………………………………MINOWA et al.
38. Reverberation Measurements of the Inner Radius of the Dust Torus in Nearby
Seyfert 1 Galaxies……………………………………………………………………………………… SUGANUMA et al.
39. Compilation and Publication of Union Catalog for Books and Materials on Japanese
Astronomy before Meiji Era …………………………………………………………………………… NAKAMURA, ITO
40. First fringe measurement of `OHANA……………………………………………………………………………PERRIN et al.
41. Combination of Nulling Interferometer and Modified Pupil for Observations of Exo-Planet ……………… NISHIKAWA et al.
187
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42. Development of Re- Os nucleo-cosmochronometer for r-process in supernovae ……………………… HAYAKAWA et al.
43. Sensitivity of R-Process Nucleosynthesis in Supernovae and GRBs to the LightElement Nuclear Reactions………………………………………………………………………………… SASAQUI et al.
44. Neutrino-Effects on R-Process Nucleosynthesis in Black-Hole Formation………………………………………SASAQUI et al.
45. Primordial magnetic field constrained from CMB anisotropies……………………………………………… YAMAZAKI et al.
46. Supernova Neutrino Nucleosynthesis of Light Elements with Neutrino Oscillations ………………………… YOSHIDA et al.

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Numerous luminous buried AGNs in ultraluminous infrared galaxies
IMANISHI, Masatoshi(Division of Optical and Infrared Astronomy, NAOJ)

DUDLEY, C. C.
(Naval Research Laboratory)

MALONEY, P. R.
(University of Colorado)
Ultraluminous infrared galaxies (ULIRGs) radiate very large
12
luminosities (L＞10 L ) as infrared dust emission, and thus mustpossess extremely powerful energy sources hidden behind dust.
The cosmic infrared background emission, the sum of dustobscured activity in the universe, is dominated by high-redshift
ULIRGs. Thus, distinguishing whether the energy sources of the
ULIRG population are dominated by nuclear fusion inside stars(starbursts) or by active mass accretion onto supermassive
blackholes with M＞107M (AGN), is important to understanding
the history of star formation and supermassive blackhole growth in
the universe.
If luminous AGNs (=actively mass accreting supermassive
blackholes) are present hidden behind dust in a torus geometry,
their signatures are easily detectable thorough optical
spectroscopy, because a large amount of AGN’s radiation escapes
along the torus axis and produces the so-called narrow line
regions. However, since nuclear regions of ULIRGs are very
dusty, AGNs resident in the majority of ULIRGs may be deeply
buried in dust along all sightlines. Although such buried AGNs are
elusive, it is fundamental to detect them and quantitatively
determine their energetic importance. For these purposes, it isinevitable to observe at wavelengths of low dust extinction. One ofsuch wavelengths is thermal infrared 3-4μm. Dust extinction at 3-4
μm is as low as that at 5-13μm. Furthermore, starburst and AGN
emission are clearly distinguishable based on the spectral shapes;
A starburst always shows strong 3.3μm Polycyclic Aromatic
Hydrocarbon (PAH) emission, while if the equivalent width of the
3.3μm 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 [1]. Finally, in a starburst,
the energy sources and dust should be spatially well mixed, while
the energy source is more centrally concentrated than thesurrounding dust in a buried AGN. In the former case (starburst),
there are upper limits to the optical depths of dust absorption
features at 3-4μm, but they can be large in the latter case (buried
AGN) [2].
We have performed systematic infrared 3-4μm spectroscopy,
using Subaru IRCS, of nearby ULIRGs with no obvious AGN
signatures in the optical, to search for elusive buried AGNs anddetermine their energetic importance (Fig. 1). We obtained thefollowing main conclusions [3]. (1) Buried AGN signatures were
found in roughy half of the observed ULIRGs, and in a muchlarger fraction of ULIRGs classified optically as LINERs than
HII-regions. (2) Buried AGNs in ULIRGs showed larger dust
extinction along our sightline than AGNs obscured by torusshaped dust (optical Seyferts). Since the dust covering factor islarger in the former, this means that the total amount of nuclear
dust around buried AGNs are systematically larger than that in
optical Seyferts. (3) Buried AGN signatures were detected in
ULIRGs with both warm and cool far-infrared colors. The larger

amount of nuclear dust around buried AGNs (see above item 2)
can naturally produce cooler far-infrared colors than AGNs
surrounded by torus-shaped dust (which often show warm farinfrared colors).

Figure1: Examples of infrared 3-4μm spectra of ULIRGs. The abscissa isobserved wavelength inμm. The ordinate is flux in Fλ(10−16 W−2−1
cm μm ). (a) A ULIRG diagnosed to be starburst dominated,because of large equivalent width 3.3μm PAH emission. (b) A
ULIRG dominated by a luminous buried AGN. No PAH emission
and strong absorption features at 3.4μm by bare carbonaceous dust
and at 3.05μm by ice-covered dust are found. (c) A ULIRG withstarburst and buried AGN composite. A low equivalent width PAH
emission and strong dust absorption features are detected.

References[1] Imanishi, M., Dudley, C. C.: 2000, ApJ, 545, 701.
[2] Imanishi, M., Maloney, P. R.: 2003, ApJ, 588, 165.
[3] Imanishi, M., et al.: 2006, ApJ, 637, 114.

3

Photospheric and Chromospheric Vector Magnetograph Systems
Installed into the Solar Flare Telescope
HANAOKA, Yoichiro, Flare Telescope Team
(Solar Observatory, NAOJ)
Active phenomena in the solar atmosphere are governed by themagnetic field, and therefore, the magnetic field information is
critically important to study them. The photospheric vector
magnetic field data have been used for this purpose, and the Solar
Flare Telescope (Fig. 1) has carried out the imaging polarimetry
observation of the photosphere since its construction. On the other
hand, actual energy release sites in various active phenomena arein layers in the solar atmosphere much higher than thephotosphere. Particularly, the information of the chromosphericvector magnetic field is very important to study the active
phenomena as well as the photospheric one. However, polarization
signals in the chromospheric lines, particularly lines formed in the
middle and the upper chromosphere, are very weak. Therefore, it
has been rather difficult to measure the vector magnetic fieldstrengths in the middle/upper chromosphere.
To achieve high sensitivity in the polarization measurement todetect weak polarization signals, we need to reduce the crosstalkcaused by the seeing effect, which is the largest source of spurious
polarization signals, and also we need to integrate photons to
reduce the statistical error. We have developed a polarimeterconsisting of ferroelectric liquid crystals (FLC), which can be
driven at high frequencies, and a high-speed CCD camera (about−1
500 frames s ). The combination of this polarimeter and the realtime data processing system enabled us to measure thepolarization signals with the sensitivity of the order of 10−4, whichmeets the requirement for measuring the chromospheric vector
magnetic field.
We made two sets of the polarimeters, and installed them into
the Solar Flare Telescope for the photospheric observation in the
Fe I 6303 line and the chromospheric observation in the Ha line,
respectively. The new polarimeter for the Fe I 6303 observation
improved the sensitivity of the polarimetry for the photospherevery much, and furthermore, we started the regular chromosphericvector magnetograph observation in the Ha line. We have realized
simultaneous observation of the vector magnetic fields in thephotosphere and the chromosphere.
Sample polarization maps in Fe I 6303 and Ha are shown in
Figure 2. Contours show the circular polarization signals, whichcorrespond to the longitudinal magnetic field, and green sticks
show the linear polarization signals, which correspond to thetransverse magnetic field. Such data are now open on our WWW
page.

Figure1: The current configuration of the Solar Flare Telescope.

References[1] Hanaoka, Y.: 2005, ESA SP-596, 57, 1.

Figure2: Sample polarization maps taken in the Fe I 6303 line and the Haline simultaneously. The position of the field of view is shown in theinset solar image at the top-right corner.

4

Preflare Nonthermal Emission Observed in Microwaves
and Hard X-Rays
ASAI, Ayumi, NAKAJIMA, Hiroshi*, SHIMOJO, Masumi(Nobeyama Solar Radio Observatory, NAOJ)

WHITE, Stephen M.

HUDSON, Hugh S., and LIN, Robert P.

(Maryland University)(UC Berkeley)

Figure1: Spatial distribution of the emission sources. The left and middle
panels show a TRACE EUV (195 Å) image. The right panel shows
the positions of the flare ribbons (dark gray regions) and the flare
loops (light gray). The overlaid contour images are the NoRH 34
GHz brightness temperature (white in the middle and black in theright panels) and the RHESSI 25 - 40 keV intensity (gray).

We examined in detail nonthermal emissions in the preflarephase of the X4.8 flare that occurred on 2002 July 23 spatially,
temporally, and spectroscopically [1]. Nonthermal emissions, thatare often observed in hard X-rays (HXRs),c-rays, and microwaves
at the beginning of a solar flare, are generated from accelerated
particles, and are associated with intense energy release processes.
Understanding of the particle acceleration mechanism has been
one of the most important and the most difficult problems in solar
physics. On the other hand, it is also interesting to study preflare
activity, since this may hold the key for understanding how totrigger the catastrophic energy release of the flare. Even in the
preflare stage of a solar flare, some energy release process isprobably occurring at a low level, although the energy release ismuch milder. It is not widely accepted that nonthermal particles
are present in significant numbers prior to the impulsive phase of aflare; rather, it is common to speak of preflare heating implying
thermal behavior. Therefore, at least in terms of the explosivenessof energy release, the impulsive phase seems to be distinguishedfrom the preflare phase.
We analyzed the flare, and found sufficient emissions both in
HXRs and in microwaves that can be candidates for nonthermal
emissions during the preflare phase. Especially, this is the firstimaging observation of preflare nonthermal emission in
microwaves. The microwave (17 GHz and 34 GHz) data obtainedwith NoRH1 at Nobeyama Solar Radio Observatory and the hard
2
X-ray data taken with RHESSI clearly showed nonthermalfeatures in the preflare phase. We focus on the nonthermal
emissions of the preflare phase. First, the GOES temperature
rapidly increases. This is often observed in a preflare phase, andthe emissions are thought to be thermal. After some short delay,
the microwave and HXR emissions starts to rise. In Figure 1 we
present the spatial features during this phase. A microwave source
appears at the top of the post flare loops that connect the flare

Figure2: Top left: a TRACE EUV image of the flare. The black solid line
illustrates the position of the slit line. Top right: time slice image
obtained with the TRACE images along the slit line. The horizontal
and the vertical axes are time (UT), and the space along the slit,
respectively. Bottom: NoRH 17 GHz light curve.

ribbons. The spectral index of the microwave emission source (a)is about −3.0, which implies that this source is emitting
nonthermal-gyrosynchrotron radiation. An HXR source also
appears at this site, although apparently slightly higher than the
microwave emission source. On the other hand, we can also see
3
footpoint sources that are located on the TRACE flare ribbons
both in the microwaves and in the HXRs. The energy releaseprobably occurs in the corona, some part of which is deposited at
the footpoints to produce the EUV brightenings. The HXR
emissions from the flare ribbon are thought to be generated bythick-target emission by nonthermal electrons. This is evidence forthe existence of the nonthermal particles in this phase. Just after
the phase, we found a faint ejection in the TRACE EUV images,
which was followed by the fast energy release process occured in
the impulsive phase (see Fig. 2).
Our results indicate that the process in the preflare phase,
which leads to fast magnetic reconnection and a violent energy
release, also releases enough amount of energy with the rightconditions to accelerate particles to nonthermal energies. Thissuggests that the energy release mechanism in the preflare phaseof a typical flare may be accompanied by particle acceleration,although it is much milder than that in the impulsive phase, andtherefore hardly detected in flares smaller than this event.
References[1] Asai, A., et al.: 2006, PASJ, 58, L1.

1

Nobeyama Radioheliograph
Reuven Ramaty High Energy Solar Spectroscopic Imager
3
Transition Region and Coronal Explorer*A former professor of NAOJ
2

5

The Unique Type Ib Supernova 2005bf: A WN Star Explosion
Model for Peculiar Light Curves and Spectra
TOMINAGA, Nozomu, TANAKA, Masaomi, NOMOTO, Ken’ichi, UMEDA, Hideyuki(School of Science, University of Tokyo)

MAZZALI, P. A.

DENG, J.

MAEDA, Keiichi(Istituto Nazionale di Astrofisica-OATs)(NAOC)(Graduate School of Arts and Science, University of Tokyo)

MODJAZ, M., HICKEN, M., CHALLIS, P., KIRSHNER, R. P., WOOD-VASEY, W. M.,
BLAKE, C. H., SZENTGYORGYI, A., FALCO, E. E.
(CfA)

BLOOM, J. S.

SKRUTSKIE, M. F.

(University of California)(University of Virginia)

INADA, Naohisa, MINEZAKI, Takeo, YOSHII, Yuzuru(Institute of Astronomy, School of Science, University of Tokyo)

KAWABATA, Koji S.

IYE, Masanori(Hiroshima Astrophysical Science Center, Hiroshima University)(Optical and Infrared Astronomy Division, NAOJ)ANUPAMA, G. C., SAHU, D. K., and PRABHU, T. P.
(Indian Institute of Astrophysics)

Figure1: The bolometric light curve constructed from UBVRIJHK-band LCs
is compared with synthetic light curves are shown for normal(dashed) and enhanced c-ray escape (solid) models.

We report a WN star explosion model for the unique type Ib
supernova (SN) 2005bf that has peculiar light curves (LCs, Fig. 1) andspectra (Fig. 2) [1]. This event is an important SN to understanddifferences between Type Ib and Ic SNe.
This SN showed unique features: the LC had two maxima, anddeclined rapidly after the second maximum [2], while the spectra
showed strengthening He lines whose velocity increased with time.
The double-peaked LC can be reproduced by a double-peaked 56Ni
distribution, with most 56Ni at low velocity and a small amount at highvelocity. The rapid post-maximum decline requires a large fraction of
the c-rays to escape from the 56Ni-dominated region, possibly becauseof low-density “holes”. The presence of Balmer lines in the spectrum
suggests that the He layer of the progenitor was substantially intact.
Increasing c-ray deposition in the He layer due to enhanced c-ray
escape from the 56Ni-dominated region may explain both the delayed
6

Figure2: Spectra of SN 2005bf (thick lines: 2005 April 13 - FLWO; May 4 HCT; May 16 - Subaru Telescope) compared to the synthetic spectra(dashed lines) computed with the model that has (M/M ,51
E/10 erg)＝(7, 1.3).

strengthening and the increasing velocity of the He lines.
The SN has massive ejecta (~ 6−7M ), normal kinetic energy(~ 1.0−1.5×1051 ergs), high peak bolometric luminosity (~ 5×1042
erg s−1) for an epoch as late as ~ 40 days, and a large 56Ni mass(~ 0.32M ). These properties, and the presence of a small amount of H
suggest that the progenitor was initially massive (M ~ 25−30M ) andhad lost most of its H envelope, possibly a WN star.
References[1] Tominaga, N., et al.: 2005, ApJ, 633, L97.
[2] Anupama, G. C., et al.: 2005, ApJ, 631, L125.

Same-Beam Differential VLBI Technology
Using Two Satellites of the SELENE Spacecraft
LIU, Qinghui, MATSUMOTO, Koji, KIKUCHI, Fuyuhiko, PING, Jinsong, ASARI, Kazuyoshi
TSURUTA, Seiitsu, HANADA, Hideo, KAWANO, Nobuyuki(RISE Project Office, NAOJ)
The Japanese SELENE project consists of a main satellite witha polar orbit of 100km, a relay sub-satellite (Rstar) with 2400-100km, and a VLBI sub-satellite (Vstar) with 800-100 km. The highdegree lunar gravity field in the far side will be directly observed
for the first time by 4-way Doppler tracking of the main satellite
via Rstar, and the low-degree gravity fields especially near the rim
will be more precisely observed by differential VLBI of the two
sub satellites.
Rstar and Vstar only transmit three-pair carriers of 2212, 2218,
2287 MHz in S-band and one-pair carriers of 8456 MHz in Xband, and the difference in phase delay between Rstar and Vstar
will be obtained from the relation between correlation phase andfrequency of four carriers. In this case, the difference in correlation
phase at each frequency has to be estimated without 2πnambiguity, for which some strict conditions such as the error ofcorrelation phase in S-band σs lower than 4.3˚ and the error ofdifferenced total electron contents (∆Ds) in ionosphere along thesignal propagation paths less than 0.23 TECU are necessary.
In order to resolve the 2πn ambiguity problem, we propose a
new VLBI technique, called same-beam differential VLBI, in
which Rstar and Vstar are observed simultaneously by the same
beam of the receiving antenna. In this case, the influence of
atmosphere, ionosphere and receivers can be nearly canceled in
the difference of correlation phases.
In this paper, we estimate the chance of same-beam differential
VLBI observation by using simulating orbits of Rstar and Vstar,and find that it is about 80 percent paths of all. We also estimate
the errors of atmosphere, ionosphere and receivers, and give
methods for decreasing these errors. As shown in Table 1, phaseerrors in the receiver are lower than 1˚. Phase fluctuations causedby thermal noise are 0.7˚ for S-band and 1.1˚ for X-band. Phasevariations in main beam of receiving antenna can be compensatedto 1.7˚ by using a formula determined by the least square method.
Difference in delay time caused by measurement error of TEC in
ionosphere is lower than 5 ps and Ds can be measured from X-and
S-band correlation phases with an accuracy of 0.07 TECU.
Difference in delay time caused by the measurement error of water
vapor in atmosphere is less than 3 ps and phase fluctuations areless than 0.7˚ RMS for S-band and 2.8˚ for X-band estimated fromthe 26 m baseline VLBI observation results. Influence of phasecharacteristic of transmitting antenna and rotation of satellites canbe reduced to 0.02˚ by using a low pass filter.
As shown in Table 2, we estimated that σs＜3.1˚, σx ＜5.2˚,
and ∆Ds＜0.1 TECU by considering the influence of two satellites
or two stations. In addition, the different error of the predicted
geometric delay between Rstar and Vstar ∆τs can be estimatedwith an accuracy of 1 ns by using range and Doppler
measurements. The difference ∆τx−∆τs mainly originated inionosphere and difference in positions of the S-band and X-band
antennas is less than 0.0082 ns.
These results show that the conditions for removing 2πnambiguity are satisfied by using the same-beam differential VLBI.

Using this new technique, difference in delay time can be obtainedwith an accuracy of several ps, and the relative position between
Rstar and Vstar can be determined with a very high accuracy oftens cm.

Figure1: Concept of the same-beam differential VLBI observation for
SELENE project.

Error source
ReceiverAtmosphere
Receiving antenna
Thermal noise
Transmitting antenna
Root sum squarephase error
（°
σ
s ）

phase error
（°
σ
x ）

1
0.7
1.7
0.7
0.02
2.2

1
2.8
1.7
0.7 , 1.1
0.02
3.7

Table1: Errors of differences in correlation phase of S-band and X-band in thesame-beam VLBI of SELENE.

°°

Table2: ∆Ds, ∆τs, ∆τx−∆τs, σs, σx in the same-beam VLBI of SELENE.

References[1] Liu, Q., et al.: 2006, IEICE, J89-B, 602-617.

7

The Relation between the Two-Point and Three-Point Correlation
Functions in the Nonlinear Gravitational Clustering Regime
KOYAMA, Hiroko

YANO, Taihei(Waseda University)(JASMINE Project Office, NAOJ)

We have studied the relation between the two-point and thethree-point correlation functions in the nonlinear gravitational
clustering regime. Under a scaling hypothesis for the bispectrum,
as well as for the power spectrum, we have derived a new formula
regarding the three-point correlation function,ζ, in the nonlinear
regime as follows,(3m＋4w−2ε)/(2m＋2w)

ζ〜ξ

(1)

where,ξ, m, w are the two-point correlation function, the powerindex of the power spectrum in the nonlinear regime, the numberof spatial dimensions, respectively. The parameter ε, relatied with
the information of the three-point correlation, is the minimum
value of some power indexes for correlations of some waves, andone of which is the power index of the Fourier-phase correlation,a. The Fourier phase in the bispectrum is described asi(φkt＋φk’t＋φ−kt−k’t)＜e−ai(φk＋φk’＋φ−k−k’)＞∝t ＜e＞(2)

The value of a represents the vihaviour of the phasecorrelation. According to the value of a, there remain two
characteristic possibilities for the evolution of the phases of theFourier modes: they remain correlated (if a＝0) or tend to become
uncorrelated (if a positive) in the strongly nonlinear regime.
We have also checked the behaviour of the relation between
the two-point and three-point correlation funcitons using
numerical simulations in a one-dimensional Einstein de Sittermodel.
Figure 1 shows the power spectrum in the nonlinear
gravitational regime where we have chosen the initial power index−0.75. From the Fourier transform,
1. It can be fitted by P (k)＝∝k−0.25. Figure 2 shows the bispectrum inthe 2PCF obeys ξ(r)∝rthe nonlinear regime when the power spectrum is expressed as in
Figure 1. It is obvious that the bispectrum is well fitted by B (k, 2k)−1.5∝k . This value of the index, −1.5, is nearly equal to 2m〜−2×2m(−0.75) ＝−1.5. Accordingly, B (k, 2k)∝k coresponds to theexpression (1) with the relationε＝−m/2. In other words, this2
result seems to agree with the hierarchical assumptionζ∝ξ .
References[1] Koyama, H., Yano, T.: 2005, ApJ, 624, 1.

8

Figure1: Power spectrum P (k). We have chosen the initial power spectrum as
the power law with index n＝1 The power index of the power
spectrum in the non-linear regime is fitted to −0.75.

Figure2: The bispectrum in the nonlinear regime when the power spectrum isexpressed as in Fig.1. The dashed line shows a power law with apower index of −1.5.

Observational Pursuit for Population III Stars
NAGAO, Tohru

MAIOLINO, R.

(NAOJ / INAF)(INAF--Roma)

MOTOHARA, Kentaro(University of Tokyo)

MARCONI, A.

MURAYAMA, Takashi

KASHIKAWA, Nobunari(INAF--Arcetri)(Tohoku University)(NAOJ)

MALKAN, M. A.

TANIGUCHI, Yoshiaki

OHTA, Kouji(UCLA)(Ehime University)(Kyoto University)

Population III stars are the stars created by pristine gas withprimordial elemental abundance ratios. Their properties have been
extensively investigated theoretically, and now it is recognizedthat the initial-mass function of population III stars could extend
up to a few hundreds M . Currently no population III stars havebeen discovered observationally so far, although massive
population III stars likely contribute to the cosmic reionization andmetal enrichment in the early universe. Therefore, we are now
promoting a project aiming to discover massive population III
stars in galaxies at high redshift (z＞6), where the massive
population III stars may still be in survival.
Galaxies hosting population III stars are expected to show an
extremely large Lya equivalent width and strong HeIIλ1640
emission, caused by hard ionizing radiation from population III
stars. Therefore, efficient surveys for Lya emitting galaxies(LAEs) with a large equivalent width are required. We thus
developed a new selection method to select LAEs with a large
equivalent width in a wide redshift range 6.0＜ z ＜6.5 byutilizing broad-band and narrow-band photometric data. Applying
this new method to the very deep and wide multi-band data of the
Subaru Deep Field ([1], [2]), we selected some candidates andconfirmed that three of them are indeed LAEs with a large restframe equivalent width (EW0 (Lya) ≥ 100Å; z＝6.03, 6.04, 6.33;[3], [4]; Fig. 1).
In order to investigate whether such LAEs contain a significant
number of massive population III stars or not, we tried to observe
their redshifted HeIIλ1640 emission by using Subaru/OHS, that
can achieve the deepest spectroscopic limiting flux in JH-band
among any ground-based instruments (Subaru common-use
program S05A-086). We carried out an ultra-deep JH-band
spectroscopy for a LAE with EW0 (Lya)＝130Å, with 42 ksec
exposure time (Fig. 2). Although we obtained only an upper limiton the HeIIλ1640 flux, we found that the star-formation in this
LAE is not dominated by population III stars and that this kind ofobservations can give some constraints on model parameters intheories of population III stars [5].
We are now carrying out additional observations for finding
new high-z LAEs with a large Lya equivalent width, selected by
our new selection method (Subaru common-use program S06A053). We are now also preparing additional near-infrared ultradeep spectroscopic observations aiming to discover population III
stars in such high-z LAEs through HeIIλ1640 emission.
References[1] Kashikawa, N., et al.: 2004, PASJ, 56, 1011.
[2] Taniguchi, Y., et al.: 2005, PASJ, 57, 165.
[3] Nagao, T., et al.: 2004, ApJ, 613, L9.
[4] Nagao, T., et al.: 2005, ApJ, 634, 142.
[5] Nagao, T., et al.: 2005, ApJ, 631, L5.

Figure1: Optical spectra of two LAEs selected by our new selection method
to pick up LAEs with large Lya equivalent width emission, obtainedwith Keck/DEIMOS [4]. Total exposure times are ~2 hours for each
LAE. Thanks to high wavelength resolution R ~ 3600, an
asymmetric profile that is expected for Lya emission is clearly seenfor each spectrum. Redshift and the rest-frame equivalent width are
6.03 and 6.04, and 94Å and 236Å, respectively. The latter is the
LAE with the largest Lya equivalent width spectroscopicallyconfirmed so far.

Figure2: JH-band spectrum of a LAE with EW0 (Lya)＝130Å obtained by 42
ksec observation using Subaru/OHS [5]. The expected wavelengthof the redshifted HeIIλ1640 emission of the target object is marked
by the black cross. Three very strong continuum features (one ispositive, and two are negative) are seen, which are the spectra of thereference star observed simultaneously with the main target.

9

Metallicity Evolution of Active Galactic Nuclei
NAGAO, Tohru

MAIOLINO, R.

MARCONI, A.

(NAOJ / INAF)(INAF--Roma)(INAF--Arcetri)

Active galactic nuclei (AGNs) are very energetic objects
releasing huge radiation from a compact region at a galactic
center. Thanks to their high luminosity, we can observe themrather easily even at high-z universe. Since we can estimate gas
metallicity of emission-line regions in AGNs through spectral
analysis, AGNs have been investigated as a tracer of metallicity
evolution of galaxies from high-z to the local universe. In
particular, broad-line regions (BLRs) that reside at r ＜1 pc fromthe nucleus have been intensively studied up to now. Such studies
have revealed that the more luminous and/or the higher redshift
AGNs tend to have the higher metallicity. However, we may see
more luminous AGNs at higher redshift due to observationalbiases.
To solve this problematic situation, we analyzed ＞5000
spectra of AGNs taken from the SDSS database and examinedthem as independent functions of luminosity and redshift (Fig. 1).
We then found that the BLR metallicity is strongly correlated with
the AGN luminosity positively while that is independent ofredshift at a given luminosity, at 2.0＜ z ＜4.5 (Fig. 2, [1]). In
order to interpret this result in terms of chemical evolutionarymodels of galaxies, it should be considered whether the BLR
located very close to the nucleus really traces properties of wholeof galaxies. We therefore investigated the dependences ofmetallicity on the luminosity and redshift also for narrow-line
1−3pc). Although NLR metallicity isregions (NLRs; r ~ 10generally estimated by using NV emission, this emission line
becomes too weak when the metallicity is low (ZNLR＜Z ) andthus only upper limits on the NV flux have been obtained formany high-z AGNs with NLR emission (type-2 AGNs). We thus
developed a new metallicity diagnostic diagram that does not
require the NV flux based on our intensive photoionization model
calculations. Applying this new diagnostic diagram on available
NLR data, we found that also the NLR metallicity strongly
correlated with the AGN luminosity positively while that is
independent of redshift at a given luminosity (Fig. 3, [2]). Since
the spatial extent of NLRs is comparable with that of their hostgalaxies, our results are highly insightful to discuss the metallicity
evolution of AGNs in terms of galaxy evolutionary models.
Now we are carrying out a new observational program toinvestigate NLR metallicity at higher redshift, z＞3, with
VLT/FORS [30 hours (period 76, priority C) and 36 hours (period
77, priority 77) have been already allocated for this program]. We
are also proposing a new observational project to Subaru, toinvestigate BLR metallicity of low-luminosity AGNs at highredshift. All of the observational insights should be summarized
and discussed in terms of galaxy evolutionary models in order tounderstand the metallicity evolution of AGNs and galaxies. To
conduct such a study, we are now preparing a hybrid model
considering both galaxy chemical evolutionary models andphotoionization models for emission-line regions [3].
References[1] Nagao, T., et al.: 2006, A&A, 447, 157.
[2] Nagao, T., et al.: 2006, A&A, 447, 863.
[3] Maiolino, R., et al.: 2006, astro-ph/0603261.

10

Figure1: Composite spectrum of AGNs made of 643 spectra at 2.0＜z＜2.5
and with −24.5＞MB＞−25.5, taken from the SDSS Data Release
2 database [1]. Although the S/N of individual spectra is low, we canmeasure even weak emission lines accurately by using composite
spectra.

Figure2: BLR metallicity-sensitive flux ratio, NV/CIV, of SDSS AGNs as
functions of the AGN luminosity (left) and of the redshift (right) [1].

Figure3: New NLR metallicity diagnostic diagram developed by us [2].
Model grids shown here are for the nH = 102cm−3 case. Although themodels depend on the gas density and thus the absolute values of
NLR metallicity cannot be estimated by this diagram, we candiscuss the relative evolution or dependence of the NLR metallicity.
The dependences of metallicity on the redshift and the AGN
luminosity are examined in the left and the right panels, respectively.
Thin bars denote the RMS’s of the data distribution, and thick bars
denote the estimated errors on the averaged values. A systematic
shift of the data on the diagram is seen in the right panel.

One Solar Cycle Observations of Prominence Activities
Using the Nobeyama Radioheliograph 1992-2004
SHIMOJO, Masumi, ASAI, Ayumi, NAKAJIMA, Hiroshi*, SHIBASAKI, Kiyoto(Nobeyama Solar Radio Observatory, NAOJ)

YOKOYAMA, Takaaki(University of Tokyo)
We developed a detection method for prominence activities
based on 17 GHz images observed with NoRH, and applied themethod to 12 yr of observations at NoRH. As a result, we detected
785 prominence activities, and found the following properties of
the activities [1]:1) The variation in the number of the prominence activities issimilar to that of sunspots during one solar cycle. The prominence
activities also have a dip around the solar maximum, like thesunspot number.
2) There are differences between the peak times of prominence
activities and sunspots. The first peak of prominence activities is
one year earlier than that of sunspots. The second peak time ofprominence activities is delayed by one year from that of sunspots
by one year.
3) The frequency distribution as a function of the magnitude ofprominence activities in each phase of the solar cycle shows apower-law distribution. The power-law index of the distributions
does not change, except around the solar minimum. At the solar
minimum, the power-law index decreases from −2.6 to −3.7.
The averaged power-law index is −2.8.
4) The number of prominence activities has a dependence on
latitude, and numerous prominence activities occur in the active
region belt. On the other hand, the average magnitude ofprominence activities is independent of the latitude.
5) During the rise phase of the solar cycle, the locations of thehigh-latitude prominence activities migrate to the pole region. The
poleward migration is similar to the motion of magnetic flux
expanding from the active regions of early Cycle 23 to the poleregion.
6) After the magnetic polarity reversal around the poles, thelocation of the prominence activities in the northern hemisphereslowly migrates to the equator. On the other hand, the prominence
activities in the southern hemisphere continue at a high-latitude
region until the decay phase of the solar cycle.
In this paper, we do not mention the difference between
prominence eruption and prominence disappearance, since we do
not classify the prominence activities based on the direction of the
motion here. The future study is to measure the direction and thevelocity of prominences, and to investigate the relationshipbetween these phenomena and the solar cycle.
References[1] Shimojo, M., et al.: 2006, PASJ, 58, 85-92.

Figure1: Upper panel: Butterfly diagram of the prominence activities. The
plus marks present the prominence activities. Lower panel: Gray
scale shows the magnetogram observed by Kitt Peak Facilities,
National Solar Observatory. Middle panel: The butterfly diagram ofthe prominence activities is plotted on the magnetogram. The black
dashed lines on the upper panel and the red dashed line on the
middle panel indicate the dormant period of the NoRH observation.
The red dashed line on the lower panel presents dormant period forthe changing system in Kitt Peak/NSO.

*A former professor of NAOJ

11

Discovery of an Extrasolar Planet HD149026 b with a Large Core
SATO, Bun’ei

IDA, Shigeru(Okayama Astrophysical Observatory, NAOJ)(Tokyo Institute of Technology)

TOYOTA, Eri

Debra, A. Fischer(Kobe University)(San Francisco State University)

Greg Laughlin(University of California at Santa Cruz)

N2K Consortium
About 30 “hot Jupiters”, extrasolar planets orbiting close tocentral stars, have been discovered by Doppler and Transit
technique. Such short-period planets have high probability oftransit, can be good tracers of multiple planet systems, and give
deep insights into understanding of formation and evolution of
extrasolar planets. Especially, transiting ones are highly importantbecause they can provide rich information on radius, density,internal structure, and atmosphere of extrasolar planets. However,among 9 transiting planets currently known, only 3 of them weredetected around bright enough (V＜10) stars for high-precision
photometry and spectroscopy.
Since 2004, we have established an international consortium(N2K) among Subaru (Japan), Keck (USA), and Magellan (Chile)aiming to search for hot Jupiters. We plan to survey 2000 solartype stars for the next 3 years and to discover more than 60 hot
Jupiters and several transiting ones. We have already screened
about 750 stars, discovered 4 new hot Jupiters, and identified
about 45 planet candidates.
HD149026 b is a “hot Saturn” discovered by Subaru and Keckobservations [1]. Firstly Subaru/HDS found the star showing
significant radial velocity variations and then Keck confirmed its
orbital parameters to be P＝2.88 days and K1＝43.3ms−1 (Fig. 1).
After that, Fairborn observatory (USA) succeeded in detecting thetransit of its orbiting planet (Fig. 2), whose radius is 0.73RJUP (0.86
RSAT), orbital inclination is 85°, and mass is 0.36 MJUP (1.2 MSAT).
The mean density is derived to be about 1.7 times larger than thatof the Saturn. Models for this planet suggest the presence of a 70
M (MEARTH) core composed of elements heavier than hydrogenand helium (Fig. 3). Existence of such a large core prefers the“core accretion” scenario to the “disk instability” one as theformation mechanism of giant planets, although it may be difficult
to form cores massive than 30M within the conventional “coreaccretion” model. Several scenarios including a giant impact
between two isolation-mass embryos are now being discussed [2].
References[1] Sato, B., et al.: 2005, ApJ, 633, 465.
[2] Ikoma, M., et al.: 2006, ApJ, 650, 1150.

Figure2: Photometric transits of HD149026 detected by Fairborn
Observatory.

Figure1: Radial velocity variations in HD149026 detected by Subaru and
Keck.

12

Figure3: Interior models of HD149026b (left) and Jupiter (right). Central darkgrey regions express solid cores.

Local Gravity From Lunar Prospector Tracking Data:
Results for Mare Serenitatis
GOOSSENS, Sander

VISSER, Pieter(NAOJ / DEOS)(DEOS)

HEKI, Kosuke

AMBROSIUS, Boudewijn(Hokkaido University)(DEOS)Up to this date, the lunar gravity field has mainly been
expressed by a global spherical harmonical representation, despite
the lack of tracking data over the far side of the Moon. Such a
representation requires regularisation, which greatly affects thecomplete final solution, for both the far and near side. To extract
the wealth of information on the near side present in tracking dataof the Lunar Prospector spacecraft, regional representations
become of interest. Here, a high-resolution gravity anomaly
solution for Mare Serenitatis, one of the large mascons on the nearside, is presented [1]. The solution has been obtained by acomplete and independent re-processing of Lunar Prospector
tracking data, allowing for a comprehensive and accurate
determination of local gravity fields on the Moon. The presented
solution requires no regularisation.
Lunar Prospector tracking data are first processed using the
GEODYN II software package. In this way, the reference orbit isdetermined and tracking data residuals with respect to the a priori
gravity field model are generated. From these residuals, the local
adjustments are estimated using a linear variational approach [2].
Figure 1 shows the new solution for Mare Serenitatis, using thelatest state-of-the-art lunar gravity field model LP150Q as a priori
model. The new solution is very similar to this model, which isalso reflected in the small adjustment to the a priori model asshown in the top plot of Figure 2. Nevertheless, the ring ofnegative anomalies surrounding the mascon appears to be more
continuous than in LP150Q, especially at the Southern border,
suggesting that the high-frequency features have a physical reality.
The bottom plot of Figure 2 shows the adjustment when anolder a priori gravity field model, GLGM-2, is used. This model
does not contain Lunar Prospector data (whereas LP150Q relies
heavily on these data). This plot clearly shows the power of thesolution method to extract the high-frequency information fromthe residuals. There is a clear ring structure visible, which can also
be seen in the differences between anomalies from the GLGM-2
and LP150Q models. Thus, using this local anomaly recovery
method, a comprehensive and detailed local study of gravity on
the lunar near side can be conducted.

Figure1: New local solution for Mare Serenitatis.

Using the LP150Q model

References[1] Goossens, S., et al.: 2005, Earth, Planets and Space, 57, 1127-1132.
[2] Goossens, S., et al.: 2005, Planet. Space Sci., 53, 1331.

Using the older GLGM-model
Figure2: Adjustments to the priori gravity field model. The top plot shows theadjustment to the LP150Q model, and the bottom plot shows theadjustment to the GLGM2 model.

13

Metal Abundances of Meteoroids in Meteor Showers:
Leonids vs Geminid
KASUGA, Toshihiro(RISE Project Office, NAOJ)

WATANABE, Jun-ichi(Hokkaido University)

KAWAKITA, Hideyo

EBIZUKA, Noboru(Kyoto Sangyo University)(RIKEN)

Spectroscopy of a large scale activity of the 2002 Leonid
meteor shower and a small scale activity of a 2004 Geminid
meteor shower have been reported [1], [2].
High-definition TV spectra in the ultraviolet to visible region
were obtained during the 2002 Leonid aircraft campaign. We
analyzed 20 meteor spectra obtained from the 1767 (sevenrevolution) and 1866 (four revolution) trails on 2002 November 19
and identified neutral atoms, mainly Mg I, Fe I, Ca I, and Na I, in
the observed wavelengths between 300 and 650 nm. The singly
ionized atomic emissions, Ca II and Mg II lines, also appeared in
the spectrum. The abundances of the metallic atoms, the electronic
excitation temperature, and the electron density are obtained foreach spectrum, assuming the Boltzmann distribution for thenumber at each energy level. The metallic abundances of Fe, Ca,
and Na relative to Mg are slightly lower than solar abundances on
average. We could not find any evidence of the solar heating effecton Leonid meteoroids between the 1767 and 1866 trails on orbit
with their perihelion (q ~ 1AU). We can support the idea thatsilicate and carbon-mixed silicate are preserved in interplanetary
space for at least several hundred years. Bands of CHON-related
molecules, such as OH and CN, are not detected [1].
The results of Geminids suggest the possibility that theabundances of Geminid meteors are slightly different from solar
abundances. Na/Mg＝0.0036±0.0005, which is much lower thanother meteor showers. On the other hand, the Ni/Mg ratio is 0.078±0.012, which is larger than solar abundance, and that of meteorsof other showers. Extreme Na depletion, and moreover, excess Ni
are derived for a Geminid meteor [2].
References[1] Kasuga, T., et al.: 2006, ApJ, 638, 1176.
[2] Kasuga, T., et al.: 2005, A&A, 438, L17.

14

YAMAMOTO, Tetsuo(Public Relations Center, NAOJ)

Figure1: A 2004 Geminid spectrum in Nobeyama Obs.

Observations of Star-forming Galaxies at z ~ 3 with ESO VLT:
Escape Fraction of Ionizing Photons and Stellar Populations
IWATA, Ikuru

INOUE, Akio K.

(Okayama Astrophysical Observatory, NAOJ)(Osaka Sangyo University)

DEHARVENG, J.-M., BURGARELLA, D., Buat, V.
(Laboratoire d’Astrophysique de Marseille)
The escape fraction of ionizing photons from star-forming
galaxies is one of the most interesting and controversial
parameters for galaxies in the early universe. Although it has beensuggested that star-forming galaxies might be a major source ofionizing photons which have reionized the neutral hydrogen in theinter-galactic space sometime at z＞6, current observational
constraints on the escape fraction of ionizing photons are quitepoor, even at the lower redshift ranges.
There are a few past works which investigated ionizing
radiation emitted from galaxies at z ~ 3, and their results areinconsistent with each other; Steidel et al. reported that the escapefraction could be fairly high (~ 60%) [1], while Giallongo et al.
placed much severe upper limits [2]. These studies are based on
spectroscopic observations for limited number of galaxies. Since
narrow-band imaging can achieve higher signal-to-noise ratio thanspectroscopy at the same integration time, it is potentially quite
effective way to explore the escape fraction of ionizing photons.
With this idea, we have carried out narrow-band imaging
observations using FORS1 attached to ESO VLT in 2003.
The target field is the Hubble Deep Field-South. We selected
sample of galaxies with photometric redshift estimates around z 〜
3 based on the ultra-deep images in UV, optical and near-infrared,and executed the multi-object spectroscopy to determine redshiftsof these galaxies, using VLT/FORS2. As a result, we haveidentified 5 new redshifts as well as confirmations of 6 redshifts[3].
The narrow-band imaging was made using an OII (373) filter.
A total exposure time was 40,636 sec. There are two galaxies forwhich the filter can trace the wavelength range just shortward of
Lyman-limit, at z＝3.170 and 3.275. We carefully examined the
reduced image and derived 3-σlimiting magnitude for positionsof these objects to be 27.37 and 27.40 AB mag [4]. These limits
correspond to the lower limits on the rate of non-ionizing UV flux
density to ionizing one, F1400 / F900 of 15.6 and 10.2 (3-σ). Under
the assumptions on the inter-galactic hydrogen absorption and the
intrinsic SEDs, this result suggests that the escape fraction ofionizing photons are smaller than the high value reported by
Steidel et al. Although in this work the number of sample objects
are limited to two, we have verified that narrow-band imaging is a
powerful method to explore the escape fraction for a specificredshift range. In order to reach a decisive conclusion on how
much ionizing photons are emitted to inter-galactic space at highredshift, we definitely need larger number of sample galaxies.
Currently we are developing a narrow-band filter to trace ionizing
photons at redshift around 3 for Subaru / Suprime-Cam, which hasa field of view about 20 times wider than VLT / FORS. The
observation with this filter should lead a drastic increase of sample
objects.
We also investigated the stellar populations of these starforming galaxies luminous in rest-frame UV wavelength. Star
formation rates, ages, amount of dust attenuation and stellar mass

were estimated by comparisons with template SEDs generated
with a population synthesis code (Fig. 1). As a result, we foundthat they are fairly young (＜200 Myr), actively star-forming(10−100M /yr) galaxies with small amount of dust (E (B−V) ＜10
0.3 in most cases) and stellar mass ((0.5−5)×10 M ). We
compared them with “distant red galaxies” (DRGs) in the same
field, which are also estimated to be at z ~ 3 and have J−K color
redder than 1.3 AB mag. We found that, although DRGs havebeen suggested to be a passively evolving galaxies at high redshift,
they would be in the actively star-forming phase with larger
amount of dust and stellar mass compared to UV-luminous
galaxies. DRGs could have large impact on the stellar massdensity estimates at z ~ 3.

Figure1: Estimates of age versus dust attenuation (upper panel) and stellar
mass (lower panel) for UV-luminous galaxies at z ~ 3 (open circles)
and DRGs (filled circles).

References[1] Steidel, C. C., et al.: 2001, ApJ 546, 665.
[2] Giallongo, E., et al.: 2002, ApJ 568, L9.
[3] Iwata, I., Inoue, A., Burgarella, D.: 2005, A&A, 440, 881.
[4] Inoue, A., et al.: 2005, A&A 435, 471.

15

Three Dimensional Motion of Plasmas Associated with a Coronal Mass
Ejection Observed with NOrikura Green-line Imaging System (NOGIS)SUZUKI, Isao, SAKURAI, Takashi, ICHIMOTO, Kiyoshi(Solar Observatory, NAOJ)

We present a Coronal Mass Ejection (CME) observation on
1999 May 7, in which NOGIS [1] revealed the motion of magnetic
loops prior to the CME and of the CME itself [2].
NOGIS is installed on a 10cm coronagraph at the Norikura
Solar Observatory, and has a unique capability of Doppler-shiftmeasurements. NOGIS has a field-of-view covering from 1.03 R
to 1.33 R , which is suitable for observing CME source regions in
the low corona.
In LASCO observation, the CME was ejected radially andeastward on 1999 May 7. Figure 1a and b show the CME source
region (NOAA 8541) observed with NOGIS before the CME and
MDI after the CME. This source region was basically bipolar, andshowed two stet loop systems (a large loop ‘L’ and a small loop‘S’). If we assume that the photospheric magnetic fields were notsignificantly disturbed, nor were they changed by the occurrenceof the CME, we might be able to infer the pre-CME magnetic
configuration by using post-event magnetograms. Figure 1c and dshow the current-free field lines [3] calculated from thephotospheric magnetogram of May 11.

km s−1) is much larger than the velocity in the plane of the sky anda downward plasma motion along the small loop was seen during
the event, the measured Doppler shift might be explained by the
downflow due to the projection effect.
The motion of the small loop toward the large loop lasted until
it touched the southern footpoint of the large loop. The small loop
apparently touched and destabilized the large loop, then massejection occurred. It was found in figure 2d that the mass wasejected with a red shift and south-eastward rather than radially.
The line-of-sight velocity from the Doppler measurement was a
few km s−1 with red shift on average.

Figure2: (a−b) NOGIS intensity and (c) Doppler images before the CME.
Symbols＋and＊indicate the large loop and the small loop,
respectively. Arrows show the locations of the footpoint of the smallloop. The dark (bright) regions in the Doppler image represent blue(red) shifts, respectively. (d) NOGIS Doppler image during the massejection. The arrow shows the mass ejection with red shift.
Figure1: (Top) Active region NOAA 8541 before and after the CME. (a)NOGIS intensity image and (b) MDI magnetogram. (Bottom)
Current-free field lines calculated from the photoshericmagnetogram of 1999 May 11.

These loop systems were initially static. However, around
02:00 UT (two and half hours before the CME) the southern
footpoint of the small loop started moving gradually toward thesouthern footpoint of the large loop (Fig. 2a and b). The velocity−1of the motion in the plane of the sky was 0.2 km s , which is areasonable value for typical shearing motion in active regions.
From the Doppler-shift measurements of NOGIS (Fig. 2c), thefootpoint of the small loop showed a higher blue shift relative tothe large loop. However, since the line-of-sight velocity (about 11
16

This CME was due to an interaction between the two
approaching flux systems. The source region was not over theactive region, but was at a lower altitude, at the footpoints of thetwo loops. The CME initially traveled non-radially until it reached
the altitude of the LASCO field-of-view. The direction of massejection was therefore determined by the magnetic field
configuration around the source region and the location of theinitial energy release in the magnetic field structure.
References[1] Ichimoto, K., et al.: 1999, PASJ, 51, 383.
[2] Suzuki, I., et al.: 2006, PASJ, 58, 165.
[3] Sakurai, T.: 1982, Sol. Phys. 76, 301.

Three-Mirror Anastigmat Telescope Design for an ELTNARIAI, Kyoji(Meisei University）

IYE, Masanori(Division of Optical and Infrared Astronomy, NAOJ)
The Ritchy-Cretien telescope design widely adopted for 8-10mclass telescopes is a two-mirror system for removing the sphericaland coma aberrations and providing a wide field of view. Its focal
plane, however, is curved and the remaining astigmatism limits theuseful field to about 6 arcmin in diameter (e.g. for Subaru
Telescope).
The next generation extremely large telescopes (ELTs) withdiameter exceeding 30m are expected to achieve diffraction
limited imaging with the advent of advanced adaptive optics.
Instruments for those ELTs inevitably become very large anddifficult to exchange. A wide-field telescope optics withdiffraction limited imaging performance, therefore, is beneficial in
deploying multiple instruments.
Obvious solution is three-mirror anastigmat telescopes. A

References[1] Korsch, D.: 1980, Applied Optics, 19, 3640.
[2] Nariai, K., and Iye, M.: 2005, PASJ, 57, 391.

Figure1: Three-Mirror Anastigmat Layout.

Figure2: Spot diagram with diffraction circles.

successful example is a Korsch three-mirror optics [1]. However,
it is for long focal ratio optics and the central field is vignetted.
Our newly designed optics [2] produces a flat focal-plane,
diffraction-limited, 20 arcmin field-of-view, by removing
spherical, coma, and astigmatism aberrations by a third asphericmirror that reimages the pseudo image produced by the two-mirror
system. An example of optical layout to secure vignetting freesemi-circle field is shown in Figure 1. Figure 2 shows the spot
diagram, demonstrating the image sizes are within the diffraction
circle out to 8 arcmin in radius.

17

SMA Observations of Submm Bright Galaxies at High-z
IONO, Daisuke(ALMA Project Office, NAOJ / Harvard-Smithsonian CfA)
Submillimeter surveys toward the deep universe have revealed
the presence of galaxies that emit strongly in dust emission [1].
The problem with these surveys is that the angular resolution of
JCMT is only 14", which is not high enough to identify the
optical/NIR counterparts to the distant sub-mm bright galaxies. Up
to the present, two of the common ways to identify the possible
counterpart is to use 1.4 GHz radio [2] or 1.3 mm [3]interferometry. While the former is easily accessible using large
scale interferometers such as the VLA, it is an indirect tracer thatutilizes the radio-FIR correlation [4] and often biased toward z ＜2−3 systems. The latter is a more direct tracer of the same dust
emission, but the dust emission at 1.3 mm is often below the detection
limit of existing mm instruments except for the brightest sources. With
the advent of submm interferometers, we can now directly identify the
optical/NIR counterparts to the submm bright galaxies.
Here we present Submillimeter Array (SMA) [5] observations
toward two recently discovered submm bright sources, GN 20 and
MIPS-J1428 [6]. GN 20 is a 20 mJy source discovered in the
SCUBA image [7] of the GOODS North field [8]. MIPS-J1428[9] is also a 20 mJy source, and it was discovered in the Spitzer
MIPS images of the NOAO Deep Wide Field Survey [10]. The
SMA is an 8-element submm interferometer operating primarily at
230 GHz (1.3mm) and 345 GHz (850μm) at the summit of Mauna
Kea in Hawaii. The observed angular resolution is ~ 2" and theastrometric accuracy of these observation is ~ 0."1.
The SMA images along with their optical counterparts areshown in Figure 1. For GN 20, the IRAC 3.6μm image reveals asource centered＜ 0 ". 5 west of the submm coordinates.
Furthermore, the higher resolution V-band image obtained by the

HST reveals a faint optical source 0."8 to the west. The analysis ofavailable ACS images provides us a rough estimate of theprobable redshift of the source and it is found to be z ~ 3−4. The
offset between the submm coordinates and the HST galaxy is
significant, and the submm emission may arise from part of a large
galaxy where V-band emission is completely obscured by theforeground dust. It is also possible that GN 20 might be aninteracting system where the optical galaxy is a companion to the
dusty, more actively star forming galaxy.
As for MIPS J1428, the optical/NIR galaxy seen here isunambiguously the galaxy responsible for the extremely brightsubmm emission. The accurate astrometry provided by the SMA
allows us to rule out fainter IRAC sources detected nearby [9] aspossible counterparts. It is still possible that MIPS-J1428 could bestrongly magnified by the foreground z＝1.034 galaxy, but thefirm upper limit to the source size of ＜ 1."2 (10 kpc at z＝1.325)
given by the SMA rules out strong magnification.
References[1] Smail, I., Ivison, R. J., Blain, A. W.: 1997, ApJ, 490, 5.
[2] Ivison, R. J., et al.: 1998, MNRAS, 298, 583.
[3] Downes, D., et al.: 1999, A&A, 347, 809.
[4] Condon, J. J.: 1992, ARA&A, 30, 575.
[5] Ho, P. T. P., Moran, J. M., Lo, K. Y.: 2004, ApJ, 616, 1.
[6] Iono, D., et al.: 2006, ApJL, 640, L1.
[7] Pope, A., et al.: 2005, MNRAS, 358, 149.
[8] Giavalisco, M., et al.: 2004, ApJ, 600, L93.
[9] Borys, C., et al.: 2006, ApJ, 636, 134.
[10] Jannuzi, B. T., Dey, A.: 1999, ASP Conf. Ser., 191. 111.

Figure1: (a) The SMA 890μm map of GN 20 and (inset) 1048＋717. The lowest positive contours represent 2σ, and the contours increase by 1σfor GN 20, and by
2σfor 1048＋717 which is our test QSO used to confirm our astrometric accuracy (see [6]). The SMA 890μm contours overlaid on the (b) Spitzer IRAC 3.6
μm image and over the (c) HST ACS V-band image, both obtained from the GOODS archive. The 4, 6, and 8σcontours from (a) are shown, and errorbars
near the center show the astrometric accuracy of the SMA image. (d) The SMA map of MIPS-J1428 and (inset) 1419＋543. The contours are the same as in
GN 20. The SMA 890μm map of MIPS-J1428 is shown overlaid on the NDWFS (e) K-band image and the (f) I-band image. The 3, 5, and 7σcontours from(d) are shown, and errorbars near the center show the astrometric accuracy of the SMA image.

18

A Coronagraphic Search for Brown Dwarfs and Planets
around Nearby Stars
NAKAJIMA, Tadashi, MORINO, Jun-Ichi, SUTO, Hiroshi, ISHII, Miki, TAMURA, Motohide
MIYAMA, Shoken, TAKAMI, Hideki, TAKATO, Naruhisa, OYA, Shin, HAYASHI, Saeko(NAOJ)

TSUJI, Takashi(IoA, University of Tokyo)

KUDO, Tomoyuki(GAUS)

FUKAGAWA, Misato

MURAKAWA, Kouji(Nagoya University)

ITOH, Youichi

OASA, Yumiko(Kobe University)(MPIfR)OPPENHEIMER, B. R.
(AMNH)We have started a corongraphic search for brown dwarfs andplanets around young nearby stars within 20 pc of the Sun, using
the adaptive optics coronagraph, CIAO, on Subaru [1]. The
dynamic range we have achieved is ∆K＝13 at 2 ". 5 from thecentral star. For a typical target with K＝7 at 10 pc, the limiting
absolute magnitude is MK＝20. We apply two kinematical age
criteria to select M and K dwarfs statistically younger than
350Myr. The first criterion is a small velocity deviation from thevelocity of LSR. The second is a (U,V,W) velocity vector similar
to a particular young moving group. The combination of the age
and magnitude limits implies that the mass limit for giant planet
detection is about 2MJ (Fig. 1). We show a sample image of atarget field at 3 pc of the Sun with faint companion candidates(Fig. 2), to be followed up for the common proper motion test.
Details of this work are published in [2].

Figure2: An example of a target field. The target star is younger than 350
Myr and located at 3 pc of the Sun. The FOV is 60×60 AU and theminimum search radius is 6AU. The detection limit is MK＝22.6.

References[1] Murakawa, K., et al.: 2004, PASJ, 56, 509.
[2] Nakajima, T., et al.: 2005, Astronomische Nachrichten, 326, 952.

Figure1: Contrast estimation by simulated planets. To study the effects ofspeckle noise on dynamic range, simulated planet images ofdifferent magnitudes (small white dots) are placed at different radiion a PSF subtracted CIAO image of a real K＝7 star. Magnitudes
and radii in arcsec of the simulated planets are (18,1.2), (19,1.5),(19.5,2.0), (20,2.5) for the panels at upper left, upper right, lower
left, and lower right, respectively. At a given radius, the SNRs of ten
simulated images range from 7 to 13.

19Morphological Classification of Galaxies using PhotometricParameters: the Concentration index versus the Coarseness parameter
YAMAUCHI, Chisato(Subaru project Office, NAOJ / Institute of Space and Astronautical Science)

ICHIKAWA, Shin-ichi

YAGI, Masafumi(Astronomical Data Analysis Center, NAOJ)(Division of Optical and Infrared Astronomy, NAOJ)

DOI, Mamoru, YASUDA, Naoki, SEKIGUCHI, Maki, FUKUGITA, Masataka, OKAMURA, Sadanori(University of Tokyo)

NAKAMURA, Osamu

GOTO, Tomotsugu(University of Nottingham)(Institute of Space and Astronautical Science)

We devised improved photometric parameters for themorphological classification of galaxies using a bright sample
from the Sloan Digital Sky Survey (SDSS) [1].
With the advancement of digitized galaxy surveys, it is highly
desirable to develop a fast, automated method of morphologicalclassification applicable to large data samples, without loosing theaccuracy of the traditional visual classification. The typicalapproaches employed for morphological classification are to apply
artificial neural networks, and characterizations with simple
surface photometric parameters [2], [3].
We focus on the photometric parameters for the morphologicalclassification of galaxies using Sloan Digital Sky Survey.
Previous studies [4], [5] showed that the concentration index,
calculated using circular isophotes as part of the standard SDSS
pipeline reductions correlates fairly well with morphological typeand can be used for classification into early and late galaxy types.
The success rate of these approaches, with reference to visualinspection, is approximately 80%.
In this study, we use the SDSS First Data Release imaging dataof 1421 galaxies selected from the SDSS Early Data Release andearly commissioning data to improve the success rate ofmorphological classifiers by introducing additional photometricparameters, and evaluate the performance of them in comparison
to the visually classified SDSS sample. First, we consider the
performance of two types of concentration indices, using circularand elliptical-apertures. We also introduce a new texture parameterto help our classification. Our texture parameter - coarseness describes the structure of the outer galaxy isophotes, emulating themethod employed in visual classification. The flux fluctuations arecomputed along elliptical circumferences in order to characterize
the galaxy profile’s departure from smoothness. The coarsenessparameter is defined as the ratio of the range of fluctuations insurface brightness along the elliptic circumference to the fulldynamic range of surface brightness of the galaxy.
We first examined the standard concentration index C＝r50/r90
defined with the Petrosian flux in the circular apertures and foundthat the correlation with visual types is significantly affected by theaxis ratio. We found that this effect is removed by defining theconcentration index using elliptical apertures (Ce). The successrate of classifying galaxies into early and late types using Ce was
86.7% with respect to the reference visual classification. With theaddition of the coarseness parameter (Y), we could achieve 88.1%
of completeness. A reasonably high success rate (66.2%) was also
attained in classifying galaxies into three types, early-type galaxies(E＋S0), early- (Sa＋Sb) and late- (Sc＋Sdm＋Im) type spiralgalaxies. We could further improve the classification by20

considering 2-dimensional (using the Ce-Y plane) classification(Fig. 1). In the case of classification into two morphological types,
this allowed us to attain a 89.4% completeness. For classification
into three morphological types, the completeness was 68.1%.

Figure1: The coarseness parameter Y of the 1421 galaxies in our sample
versus the concentration index Ce. The quadratic function is theregression line by least-squares fitting to the average 2-vector ofgalaxies. The two dotted lines are the best classifiers into three types,
E＋ S0, Sa＋ Sb and Sc＋ Sdm＋ Im on the 2-dimensionalclassification.

Our newly devised photometric parameter, coarseness,
provides a mode of morphological classification as good as the
traditionally used human-eye classification. Therefore, this newparameter has a potential to open new doors to detailed studies ofgalaxy morphology in current and future large CCD surveys.
References[1] Yamauchi, C., et al.: 2005, AJ, 130, 1545.
[2] Doi, M., et al.: 1993, MNRAS, 264, 832.
[3] Abraham, R., et al.: 1994, ApJ, 432, 75.
[4] Shimasaku, K., et al.: 2001, AJ, 122, 1238.
[5] Strateva, I., et al.: 2001, AJ, 122, 1861.

Dense and Warm Molecular Gas Observations of NGC 6240 with
the Nobeyama Millimeter Array and the RAINBOW Interferometer
NAKANISHI, Kouichiro, OKUMURA, Sachiko K.
(Nobeyama Radio Observatory, NAOJ)

KOHNO, Kotaro(Institute of Astronomy, University of Tokyo)

KAWABE, Ryohei(ALMA Project Office, NAOJ)

NAKAGAWA, Takao(Institute of Space and Astronautical Science, JAXA)

Figure1: HCN(1-0) integrated intensity map (contours) obtained with the NMA and the RAINBOW Interferometer [1] superposed on the near-infrared [Fe II ] at
1.644μm (left panel) and H2 (v＝1−0 S (1)) at 2.121μm (right panel) emission line maps [2]. The figure clearly shows that the HCN peak (dense moleculargas) agrees well with the H2 peak (hot molecular hydrogen excited by large-scale shock [3]) rather than the [Fe II ] peak (supernova remnants, current
massive star-forming regions).

Luminous infrared galaxies (LIRGs) are known to be huge
9molecular gas reservoirs [M (H2)＞10 M ]. The results of
12
CO(1−0) observations reveal that this molecular gas is usuallyconcentrated at the center of LIRGs. However, the physicalproperties, namely the density and the temperature, of themolecular gas in LIRGs are still being studied.
NGC 6240 is one of the most well-known nearby LIRGs. Thisgalaxy is a merger with clearly visible disturbed morphology andhas double nuclei. High spatial resolution observations of the12CO(1−0), HCN(1−0), HCO ＋ (1−0), and 13 CO(1−0)
molecular lines toward NGC 6240 have been performed using theNobeyama Millimeter Array (NMA) and the RAINBOWInterferometer [1]. The RAINBOW Interferometer is a 7-element
array combining the NMA with the NRO 45m telescope,providing higher spatial resolution and sensitivity than those of the
NMA.
All of the observed molecular emission lines are concentrated
in the region between the double nuclei of the galaxy. The＋
distributions of both HCN and HCO emissions, which aresupposed to be dense molecular gas tracers, are not coincident
with the current massive star-forming regions (see Fig. 1). The

12high HCN/ CO line intensity ratio suggests that most of themolecular gas between the double nuclei is dense. A comparisonof the observed high HCN/13CO intensity ratio with the resultsfrom radiative transfer model calculations [4] suggest that themolecular gas is dense [n (H2)＝104−6cm−3] and warm (Tkin＞50
K).
The observed structure in NGC 6240 may be explained by time
evolution of the molecular gas and star formation, which was
induced by an almost head-on collision or very close encounter of
the two galactic nuclei accompanied with the dense gas and starforming regions.
References[1] Nakanishi, K., et al.: 2005, PASJ, 57, 575.
[2] van der Werf, P. P., et al.: 1993, ApJ, 405, 522.
[3] Ohyama, Y., et al.: 2003, AJ, 126, 2291.
[4] Matsushita, S., et al.: 1998, ApJ, 495, 267.

21

Clustering of Lyman Break Galaxies at z = 4 and 5 in The Subaru Deep
Field: Luminosity Dependence of The Correlation Function Slope
KASHIKAWA, Nobunari(Division of Optical and Infrared Astronomy, NAOJ)

and Subaru Deep Field team
The clustering strength of galaxies is one of the mostfundamental measures in observational cosmology. The
measurement of galaxy clustering and its evolution enable us to
see the history of galaxy assembly, which is an essential process inthe present-day standard paradigm of hierarchical galaxy
formation. Recent numerical simulations suggest that some darkhalos may harbor more than one Lyman break galaxies (LBGs). If
this is the case, then clustering analyses made using a small FOV
are biased to probe dominantly for galaxy pairs in the same halo
and will tend to miss the halo-halo pair contribution, which has adistinct clustering strength at large scales.
We explored the clustering properties of LBGs at z＝4 and 5with an angular two-point correlation function on the basis of thevery deep and wide Subaru Deep Field data (Fig. 1). We
confirmed the previous result that the clustering strength of LBGs
depends on the UV luminosity in the sense that brighter LBGs are
more strongly clustered. In addition, we found an apparent
dependence of the correlation function slope on UV luminosity for
LBGs at both z＝4 and 5 (Fig. 2). More luminous LBGs have asteeper correlation function. The bias parameter was found to be ascale-dependent function for bright LBGs, whereas it appears to bealmost scale-independent for faint LBGs. Luminous LBGs have ahigher bias at smaller angular scales, which decreases as the scale
increases.
To compare these observational results, we constructednumerical mock LBG catalogs based on a semianalytic model ofhierarchical clustering combined with high-resolution N-bodysimulation, carefully mimicking the observational selection
effects. The luminosity functions and the overall correlation
functions for LBGs at z＝4 and 5 predicted by this mock catalog
were found to be almost consistent with the observation. The
observed dependence of the clustering on UV luminosity was not
reproduced by the model, unless subsamples of distinct halo mass
were considered. That is, LBGs belonging to more massive darkhalos had steeper and larger amplitude correlation functions. With
this model, we found that LBG multiplicity in massive dark halos
amplifies the clustering strength at small scales, which steepens
the correlation function. The hierarchical clustering model could
therefore be reconciled with the observed luminosity dependenceof the correlation function if there is a tight correlation between
UV luminosity and halo mass. Our finding that the slope of thecorrelation function depends on luminosity could be an indicationthat massive dark halos hosted multiple bright LBGs [1].

Figure1: Sky distribution of z＝4 LBG sample in the Subaru Deep Field.
Larger circles denote brighter objects in total i’-band magnitude. The
local overdensity, with the significance of each, is denoted by color
as shown in the color legend. The black shaded areas are masked
regions in which detected objects were rejected due to low S/N.
North is up and east is to the left.

References[1] Kashikawa, N., et al.: 2006, ApJ, 637, 631.
Figure2: Luminosity dependence of angular correlation functions (ACFs) inthe z＝4 LBG sample. The ACFs of i’ ≤ 25.5, 25.5＜i’≤ 26.5, and26.5＜i’≤ 27.4 are represented by symbols given in the legend. The
dotted line is the nonlinear ACF of dark matter at z＝4 calculatedwith the same observational selection function. Bottom; Our definedbias parameter b(θ) for each luminosity subsample with the same
symbol and color as indicated in the top panel.

22

Discovery of HE 1327-2326, the most iron-deficient star known
AOKI, Wako
(Division of Optical and Infrared Astronomy, NAOJ)
Measurements of chemical compositions for extremely metaldeficient stars have been providing constraints on the studies onformation and evolution of first generation stars, supernova
explosion mechanism, early nucleosynthesis etc. For such
purposes, surveys of extremely metal-poor stars have been madein the past few decades. Our group [1] conducted observations
with the High Dispersion Spectrograph of the Subaru Telescope tomeasure the chemical compositions of candidate extremely metalpoor stars ([Fe/H]＜−3) from 2003 to 2005. In this observing
program, we found that HE 1327-2326, a star identified as a
candidate metal-poor star by the Hamburg/ESO survey, is themost iron-deficient star known to date, and determined its detailed
chemical abundance pattern [2], [3].
This star turned out to be a main-sequence or subgiant starfrom the photometric observations. Figure 1 shows a comparisonof the spectrum of this object with that of CS 22876-032, thepreviously known most metal-deficient main-sequence star. The
candidates of metal-deficient stars are selected from the strength of
the Ca K line in the medium resolution spectra (upper panel).
However, the high resolution spectrum of HE 1327-2326 showsthat the contribution of interstellar absorption to this feature issignificant, and the Ca abundance at the surface of this object isremarkably low. Indeed, the absorption features of other heavy
elements like Fe are also extremely weak, and Fe abundance
derived by the detailed abundance analysis is 250,000 times lower
than the solar value. This is only about 60% of the Fe abundance
measured for HE 0107-5240, the previously known most irondeficient star (a red giant).
By way of contrast, a number of weak CH features are detectedin the spectrum of this object, indicating that the carbon abundanceof this object is not so deficient as Fe ([C/H] ~−1.3). Detailed
abundance analyses revealed the unique abundance pattern of thisobject that heavy elements (e.g. iron-peak elements) are extremely
deficient while light elements (C, N, and a elements) are relatively
rich. The low abundances of heavy elements suggest that this starwell preserves the yields of the first generation stars. The
nucleosynthesis of the first generation objects, and their massfunction, are at present discussed based on the chemicalcomposition of this star.
Moreover, the following two results for this objects were notexpected before our observation: (1) The Li resonance line, which
is detected in most main-sequence and subgiant stars at low
metallicity, is not detected; (2) The heavy element Sr is
overabundant ([Sr/Fe] ~＋1). These facts suggest the existence of
unknown processes related to the formation of first generationstars and their nucleosynthesis. We note that a new spectrum of
this object was obtained with ESO/VLT with longer exposure
time, and new results including the determination of oxygen
abundance [4] have been obtained.

Figure1: A comparison of spectra of HE 1327-2327 and CS 22876-032 (thepreviously known most metal-deficient main-sequence star). The
upper panel shows the medium resolution spectra, in whichhydrogen Balmer lines as well as the Ca K line appear. The lower
panel shows the high resolution spectra for the wavelength range
near the K line. The Ca interstellar absorption is well separated fromthe stellar absorption line in the spectrum of HE 1327-2326. While
no Fe absorption line is detected in this wavelength range for HE
1327-2326, weak absorption features of CH molecule are seen.
References[1] Followings are the members of this collaboration: W. Aoki, S. Honda, H.
Ando, T. Kajino (NAOJ), M, Takada-Hidai (Tokai University), K.
Nomoto, Y, Yoshii (University of Tokyo), M. Y. Fujimoto (Hokkaido
University), J. E. Norris, A. Frebel, M. Asplund (Australian National
University), T. C. Beers (Michigan State University), N. Christlieb(Hamburg University), S. G. Ryan, S. Tsangarides (Open University).
[2] Frebel, A., et al.: 2005, Nature, 434, 871.
[3] Aoki, W., et al.: 2006, AJ, 639, 897.
[4] Frebel, A., et al.: 2006, AJ, 638, L17.

23

Sulfur and Zinc Abundances of Galactic Disk/Halo Stars :Application of Extensive Detailed Non-LTE Calculations
TAKEDA, Yoichi

HASHIMOTO, Osamu, TAGUCHI, Hikaru(Division of Optical and Infrared Astronomy, NAOJ)(Gunma Astronomical Observatory)

YOSHIOKA, Kazuo

TAKADA-HIDAI, Masahide, SAITO, Yuji

HONDA, Satoshi(University of Air)

(Tokai University)(Subaru Telescope, NAOJ)

Sulfur (S) and zinc (Zn) are of particular astrophysicalimportance because they are chemically “volatile”. That is, they
are difficult to condense into solids (unlike other “refractory”
elements such as Mg, Si, Fe-group elements, etc.) and thus are
considered to be hardly affected by depletion due to dust
formation. Therefore, for the case of post-AGB stars in the latestage of stellar evolution, where atmospheric abundances ofrefractory elements have been more or less depleted because ofcondensation into dust coupled with mass-loss, [S/Zn] vs. [Zn/H]
relation is often used as a substitute for [S/Fe] vs. [Fe/H], fromwhich its original metallicity (or stellar population) may beinferred. In this sense, it is important as a prerequisite tounderstand the behavior of [S/Fe] and [Zn/Fe] with a change of[Fe/H] in metal-poor stars.
Unfortunately, however, these relations have not yet been
firmly settled. Especially, we are still in a confusing situation
concerning the case of S, for which two contradicting [S/Fe] trends
toward a decrease of [Fe/H] (increasing vs. flat) are argued forvery metal-poor stars ([Fe/H]＜−2), depending on the lines (S I
8693/8694 and S I 9212/9228/9237) used for abundance
determinations. On the other hand, the long-believed simple〜 0) over a large range ofscaling of Zn with Fe ([Zn/Fe]−
metallicity has now become questioned based on recent analyses,
which indicate a supersolar [Zn/Fe] toward an extremely metalpoor regime ([Fe/H]＜−3) as well as a slight tendency even ingalactic disk stars (−1＜ [Fe/H]＜＋0.5).
Here, it should be noted that all these analyses were done withthe assumption of LTE (application of Saha-Boltzmann equationby using local temperature and density for calculating level
populations), the validity of which has never been confirmed sofar. Therefore, we decided to carry out extensive non-LTE
calculations on neutral sulfur and zinc for the first time, in order toexamine whether such a discrepancy on S or the observed trend inZn may have something to do with the non-LTE effect, as well as
to establish the non-LTE [S/Fe] vs. [Fe/H] and [Zn/Fe] vs. [Fe/H]
relations. The results are shown in Figures 1 and 2, andsummarized as follows:
We still encounter a serious difficulty in the [S/Fe] vs. [Fe/H]
relation at the very metal-poor region of [Fe/H]＜−2, in the sensethat the [S/Fe] values derived from S I 8693/8694 (non-LTE effectis practically negligible) tend to rise progressively with a decreaseof metallicity while those from S I 9212/9228/9237 (suffering
considerably larger non-LTE effects) show a flat plateau or a signof slight downward bending; the discordance amounts up to 〜0.5
dex. Namely, the discrepancy seen in the LTE analyses is evenexaggerated due to the application of non-LTE corrections.
For the studied Zn I 4722/4810/6362 lines, the non-LTE effectis generally small and insignificant. Inspecting the [Zn/Fe] vs.
[Fe/H] relation resulting from our reanalysis, we almost confirmed
the recently reported tendency, such as the gradual increase of[Zn/Fe] from [Zn/Fe] ~ 0 (at [Fe/H] ~ 0) to [Zn/Fe] ~ 0.2 (at24

Figure1: Runs of [S/Fe]NLTE and ∆NLTE (non-LTE correction) against [Fe/H].

Figure2: Runs of [Zn/Fe]NLTE and ∆NLTE (non-LTE correction) against [Fe/H].

[Fe/H] ~ −1), nearly constant [Zn/Fe] (i.e., without particulartrend) over the region of −2＜ [Fe/H] ＜−1, and a beginning ofrise at [Fe/H]＜−2 continuing toward an extremely lowmetallicity regime.
The details of this study are described in [1].
References[1] Takeda, Y., et al.: 2005, PASJ, 57, 751.

Rotating Molecular Gas Associated with a Silhouette Disk
at the Center of the Radio Galaxy 3C 31
OKUDA, Takeshi, KOHNO, Kotaro(Institute of Astronomy, University of Tokyo)

IGUCHI, Satoru(ALMA Project Office, NAOJ)

NAKANISHI, Kouichiro(Nobeyama Radio Observatory, NAOJ)
The radio source 3C 31 is hosted by the D galaxy, which is thebrightest galaxy in the Zwicky cluster 0107.5＋3212 at a distanceof about 70 Mpc. Very Large Array (VLA) images of radio
wavelengths show bi-directional and twisting synchrotron jetswith a size of approximately a few 100 kpc emanating from thecenter of the galaxy [1]. The Hubble Space Telescope (HST)
observations reveal the presence of a silhouette disk with adiameter of about 6 arcsec or 2 kpc at a distance of 3C 31 [2]. The
detection of abundant molecular gas has been reported in thecourse of the survey of 12CO(J＝1−0) and 12CO(J＝2−1)
emissions toward 3C radio galaxies using the IRAM 30m
telescope [3]. The proximity and the large apparent size of the diskof 3C 31 make it an ideal object to study the structure and thekinematics of molecular gas in a silhouette disk.
We report high angular resolution 12CO(J＝1−0) observationsof the radio galaxy 3C 31 using the Nobeyama Millimeter Array(NMA) and the RAINBOW Interferometer, which is a 7-element
combined array between the NMA and the NRO 45m telescopethat can achieve a very large collecting area and a high spatial
resolution [4]. Our high-resolution (1."9×1."4 or 640 pc×470 pc at
D＝70 Mpc) 12CO image shows a circularly rotating moleculargas disk, which closely coincides with a silhouette disk observedin the Hubble Space Telescope (HST) optical images.
The molecular gas mass (Mgas) of the disk is estimated to be8
9.7×10 M within a radius of 1 kpc, and the peak gas surface
density ∑gas is 4.0×102M pc−2 at 440 pc from the center, if a
Galactic I(CO) to N(H2) conversion factor (1.8×1020 [cm−2 (K−1 −1
km s ) ]) is applied [5]. The rotation velocity of the disk is−1
460km s at a radius of 1 kpc, giving an enclosed mass
10
(dynamical mass) of Mdyn＝5.0×10 M within this radius.
The ratio of gas mass to dynamical mass, Mgas＝Mdyn is lessthan 0.02 within a radius of 1 kpc. This ratio is smaller than thosein typical star-forming/starburst galaxies by a factor of 3 orgreater, implying that the molecular gas disk in the center of 3C 31
is gravitationally stable, and this is consistent with the fact thatsuccessive massive star formation does not occur there [6].

12Figure1: The NMA and RAINBOW maps of CO (J＝1−0) emission in theradio galaxy 3C 31. The central cross in figure (a), (b), (c), and (d)marks the peak of 8.4 GHz in the continuum. (a) HST R-band imageof the center of 3C 31. The HST image was obtained from the dataarchive of the Multimission Archive at STScI. (b) Integrated
intensity map (contour) of 12CO (J＝1−0) superposed on an HST
12image (color). (c) Integrated intensity map of CO (J＝1−0). (d)12Intensity-weighted mean velocity map of CO (J＝1−0).

References[1] Lara, L., et al.: 1997, ApJ, 474, 179.
[2] Martel, A. R., et al.: 1999, ApJ, 122, 81.
[3] Lim, J., et al.: 2000, ApJ, 545, L93.

Figure2: Azimuthally averaged radial distributions of gas mass across themolecular disk in 3C 31.

[4] Okuda, T., et al.: 2005, ApJ, 620, 673.
[5] Dame, T. M., et al.: 2001, ApJ, 547, 792.
[6] Owen, F. N., et al.: 1990, ApJ, 352, 44.

25

Installation of Seismic Attenuation System (SAS)to Gravitational Wave Detector TAMA300
FUJIMOTO, Masa-Katsu, KAWAMURA, Seiji, YAMAZAKI, Toshitaka
TAKAHASHI, Ryutaro, ARAI, Koji, TATSUMI, Daisuke, FUKUSHIMA, Mitsuhiro
SATO, Shuichi, TAKAMORI, Akiteru, and the TAMA Collaboration(TAMA Project Office, NAOJ)
The development of Seismic Attenuation System (SAS) started
from 1999 in cooperation with the LIGO group of USA. The
experiments using SAS prototypes were finished by 2002. We
started manufacturing and assembling of four SAS towers for
TAMA300 from 2003. The first tower has been installed to thewest-end room in September, 2005 (Fig. 1).
After the installation, we identified the natural frequencies of
the inverted pendulum for horizontal isolation. The frequencies
were decided as 154 mHz for X, 46 mHz for Y, and 542 mHz for
rotation (θ) respectively. The horizontal modes (X and Y) were notdegenerated at all. The natural frequencies of the Geometric AntiSpring Filter for vertical isolation were 482 mHz and 919 mHz.
A full-digital system is introduced to control SAS for the firsttime in TAMA300. The system is handled by an all-purpose CPU(Penntium III/1.2 GHz) and a real-time OS. LabVIEW is available
to program the controller. There are three acceleration sensors,
three LVDTs, and three coil-magnet actuators for horizontal
directions on the top of SAS. A LVDT and a coil-magnet actuator
are used for vertical direction. Since acceleration sensors, LVDTs,
and actuators are not put along the direction of identified mode (X,Y, andθ), three signals must be diagonalized to the directions of X,
Y, and θ. Seven channels of acceleration sensor and LVDT are
assigned to inputs (A/D converters) of the digital controller. Seven
channels of diagonalized acceleration signal and actuator are
assigned to outputs (D/A converters). Main process of the digital
controller is diagonalization and filtering of input signals. The
first, the diagonalization matrix was decided using natural modes
which appear in the measured transfer functions from eachactuator to each sensor. The second, optimal servo filters were
designed using measured transfer functions from a diagonalized
virtual actuator to a virtual sensor. The resonances of each mode
were successfully damped by the designed servo system.
We added a digital controller for rotational motions (pitch andyaw) of the mirror in order to lock the 300 m cavity where one of
mirror is suspended by installed SAS. A local optical lever wasused as a angular sensor. A large resonant peak at 50 mHz due tothe torsion mode was damped using complicated servo filters that
it is difficult to construct by an analog controller. After the 300 m
cavity is locked, the control signals are changed to more sensitive
signals acquired by the Wave Front Sensing (WFS) method fromthe interferometer. Owing to this control, a stable lock of the 300
m cavity succeeded with SAS. We could change the control
signals from optical lever to WFS successfully without lock lost.
The remains of a SAS tower will be installed as they become
ready by autumn in 2006.

26

Figure1: Installation works for SAS in the west-end room.

Development of a laser interferometric high-precision angle sensor
for the JASMINE satellite
ARAI, Koji

NIWA, Yoshito

SAKAGAMI, Masaaki(TAMA Project Office, NAOJ)(Kyoto University / JASMINE Project Office, NAOJ)(Kyoto University)

GOUDA, Naoteru, KOBAYASHI, Yukiyasu, YANO, Taihei

YAMADA, Yoshiyuki(JASMINE Project Office, NAOJ)(Kyoto University)

Figure2: Power spectral density of the measured differential angle fluctuationof the two mirrors forming Fabry-Perot cavity.
Figure1: Schematic diagram of the optical, electronic, and servo-control
systems for the basic angle monitor.

The JASMINE project proposes an astronomical satellite
mission in near-infrared band. The goal of the project isestablishment of astrometry by observing annual parallaxes andproper motions with precision of 10μarcsec for several hundred
million stars in the galactic plane and the galactic bulge. Since it isdifficult to control rotation of the satellite with such precision, amirror called beam mixing mirror will be used to observe twolargely-separated sky field simultaneously in order to distinguishthe motion of stars from fluctuation of the satellite rotation. This
angle separation, which is 99.5 degree for JASMINE, is calledbasic angle.
If the basic angle fluctuates more then 10μarcsec, the required
observation precision would not be achieved. Therefore, thestability of the basic angle should be monitored by an highprecision angle sensor (basic angle monitor). Since 2004,
JASMINE Project, with assistance of TAMA Project, started
planning and development of a laser interferometer basic angle
monitor.
This year, basic angle monitor using Wave Front Sensing
technique[1], [2](WFS) was built. WFS is a technique to detect
difference of optical axes between an optical cavity and an
incident beam. In our instrument, the incident laser beam isaccumulated in a Fabry-Perot cavity formed by two sphericalmirrors. The reflected light is detected by quadrant photodetectors. Phase modulation is applied to the incident light so thatthe phase modulated light and the leakage intracavity lightinterferes on the quadrant photo detectors resulting in indication of
the optical axis difference when the output signals are being
demodulated. Using this instrument, differential fluctuation of themirror angle, which affects the observation of JASMINE, isselectively detected, separated from other common-mode mirror
angle fluctuation and incident beam fluctuation.
The characterization of our instrument was performed. The
optical, electronic, and servo-control systems of the instrument
were built (Fig. 1). The cavity length control establishes the statethat the laser beam continuously resonates to the cavity. In thisstate, the angles of the two cavity mirrors were artificially
actuated. From the response of the sensors, it was confirmed thatthe angle sensor linearly responds to the actuation and is 85 times
more sensitive to the differential angle actuation, which we wantto observe, than to the common-mode actuation. The differential
angle fluctuation of the cavity mirrors were measured without any
actuation (Fig. 2). It was found that the RMS fluctuation level
above 1mHz with the current optical system is about 2500 times
larger than the required level by JASMINE. This research resulted
in the master degree of Niwa.
Our next step is proceed the experiment to fulfill the required
level by JASMINE. Currently all of the optical system is placed
under the atmospheric pressure. The fluctuation of the cavity by
the air flow and the temperature change is to be considered byusing vacuum systems and passive and active temperaturestabilization systems.
References[1] Morrison, E., et al.: 1994, Appl. Opt., 33, 5041.
[2] Morrison, E., et al.: 1994, Appl. Opt., 33, 5037.

27

Velocity Drift of Water Maser Features of NGC 4258
YAMAUCHI, Aya(Kyushu University / Nobeyama Radio Observatory, NAOJ)

SATO, Naoko(Hokkaido University / Nobeyama Radio Observatory, NAOJ)

HIROTA, Akihiko

NAKAI, Naomasa(University of Tokyo / Nobeyama Radio Observatory, NAOJ)(University of Tsukuba)

Figure2: An illustration of the spiral structure in a maser disk. −r is the mean
radius of the maser disk, and θp and Ω are the pitch angle andpattern speed of the spiral arms.

Figure1: Velocity variations of red-shifted features from 1992 January 12.

We monitored the velocities of high-velocity features for a H2O
megamaser, NGC 4258, using the 45-m telescope of the
Nobeyama Radio Observatory (NRO) [1].
Water-vapor (H2O) maser emission is a unique probe toinvestigate the structure and dynamics of active galactic nuclei(AGN) on the (sub-)parsec scale directly. NGC 4258 is the moststudied megamaser. VLBI observations revealed the existence of acompact edge-on disk in Keplerian rotation and a massive blackhole at the nucleus of the galaxy [2].
For most of megamasers, including NGC 4258, the intensitiesof blue-shifted features are weaker than those of red-shiftedfeatures. Maoz and McKee (1998) explained the asymmetry of thehigh-velocity features (i.e., red- and blue-shifted features) using aspiral shock model in masing disk [3]. In this model, it is expectedthat rotation of the spiral shock should lead to a velocity drift ofhigh-velocity features. They predicted that red-shifted features
have negative drift rates, and vice versa. To confirm this model,
we measured the velocity drift rates of the high-velocity featuresof NGC 4258.
Observations of H2O maser emission were made from 1992
28

January through 2005 April. Figure 1 shows the velocity variationsof the red-shifted features at VLSR＝1220-1460km s−1. We plot thefeatures with peak intensities of ≥ 5σ for each observation. Using
the data of 1992−2005, the drift rate was detected to be −a ＝−0.036±0.007km s−1 yr−1 on the average for 10 red-shiftedfeatures. The drift rate of a blue-shifted feature was a＝0.20±
0.10km s−1 yr−1. These results are consistent with a prediction thatthe observed line-of-sight velocities of red-shifted features
decrease, and those of the blue-shifted increase, from the spiralshock model.
Assuming a logarithmic spiral (i.e., constant pitch angle of the
spiral), we can calculate the pitch angle, θp, given by−1

θp＝tana(−−v2−Ω−),using an assumed pattern speed of the spiral arms, Ω＝2250km−1−1
s pc , and the rates of velocity drifts measured. The pitch− ＝2°±1° on theangles of the spirals were obtained to be θpaverage for the red-shifted features, and θp＝13°±7° for the blueshifted feature from the measured drift rates.
References[1] Yamauchi, A., et al.: 2005, PASJ, 57, 861.
[2] Miyoshi, M., et al.: 1995, Nature, 373, 127.
[3] Maoz, M., McKee, C. F.: 1998, ApJ, 494, 218.

Nobeyama Millimeter Array Observations of GRB 030329:
a Decay of Afterglow with Bumps and Molecular Gas in the Host Galaxy
KOHNO, Kotaro, OKUDA, Takeshi, MURAOKA, Kazuyuki, ONODERA, Sachiko, SOFUE, Yoshiaki(University of Tokyo)

TOSAKI, Tomoka(Gunma Astronomical Observatory)

NAKANISHI, Kohichiro, KAMAZAKI, Takeshi, OKUMURA, Sachiko, KUNO, Nario, ISHIZUKI, Sumio(Nobeyama Radio Observatory, NAOJ)

KAWABE, Ryohei

OHTA, Koji

KAWAI, Nobuyuki(ALMA Project Office, NAOJ)(Kyoto University)(Tokyo Institute of Technology, RIKEN)

Figure1: Selected images of GRB 030329 afterglow atλ＝2 mm and 3 mm
to depict fading afterglow emission. The observed frequency, timeafter the burst, and the synthesized beam are indicated. The central
cross in each panel marks the position of the GRB 030329 opticalafterglow. The contour levels are -3σ, 3σ, 9σ, and 15σfor the 141
GHz image, and the contour intervals are 2σfor 93 GHz images.

Nobeyama Millimeter Array was used to observe millimeterwave afterglow of GRB 030329 at 93 GHz and 141 GHz from2003 April 6 (8.23 days after the burst) to 2003 May 30 (61.97
days). A sensitive search for CO (J＝1−0) emission/absorption
from the host galaxy of GRB 030329 was also carried out [1].
Unresolved millimeter continuum emission at the position of
GRB 030329 was detected until 2003 April 21. We found a steep−2.0
decline of continuum flux (∝t ) during this period, in accord
with a previous report. Moreover, our data implies that the decay
was accompanied by possible plateaus phases on a time scale ofseveral days. If they are caused by density fluctuations ofsurrounding ISM, the spatial scale of the structure corresponding3
to the time scale is about ~ 10 AU, supposing a relativistic
expansion. From an integrated spectrum, produced by summingup the data from 2003 April 10 to 2003 May 30, we found a
possible emission feature, which could be a redshifted CO (J＝1−0) line. Its position and redshift coincide well with those of
GRB 030329, though further observations are required to confirm
the detection. If the emission feature is real, the observed CO flux−1
is 1.4±0.52 Jy km s , corresponding to a large molecular gas
9mass of M(H2)＞10 M . This implies that the host galaxy, which
is optically faint, is highly obscured due to a rich interstellar
medium.
References[1] Kohno, K., et al.: 2005, PASJ, 57, 147.

Figure2: Time variation of λ＝2mm (square) and 3mm (circle) continuum
flux toward GRB 030329 observed with the Nobeyama Millimeter
Array. The upper limits are 2σ.

Figure3: (Left) Observed spectrum at the 98 GHz band toward GRB 030329,
produced by summing up the 3 mm data from 2003 April 10 to 2003
−1
May 30. The spectral resolution is 16 MHz or 48.6km s , and therms noise level is 3.8 mJy. (Right) A integrated intensity map of a−1
possible CO emission line over a velocity width of 220km s . The
synthesized beam, shown in the right bottom corner, is 7".0×6".3(position angle＝84°). The contour interval is 0.52 Jy−1 km s−1
(1σ).

29

A 385-500 GHz Sideband-separating (2SB) SIS Mixer
Based on a Waveguide Split-Block Coupler
KAMIKURA, Mamoru, TOMIMURA, Yu

SEKIMOTO, Yutaro, ASAYAMA Shin’ichiro(University of Tokyo)

SHAN, Wenlei(NAOJ)SATOU, Naohisa, IIZUKA, Yoshizo, ITO, Tetsuya, KAMBA, Toshiaki(NAOJ / Purple Mountain Observatory)

SERIZAWA, Yasutak(University of Tokyo)(NAOJ)NOGUCHI, Takashi(NAOJ)

Figure1: Photograph of an RF/LO coupler. An RF/LO coupler contains an RF
quadrature hybrid, two LO couplers, and an in-phase power divider.

Figure2: Results of the mechanical measurements of the RF quadrature
hybrid.

We have developed a 385-500 GHz sideband-separating (2SB)
SIS mixer, which is based on a waveguide split-block coupler [1].
The 2SB mixer is to be installed into the ALMA receiver for theBand 8 (385-500 GHz) frequency range. To reduce atmosphericnoise, sideband separation is necessary. So far sideband-separating
mixers have been designed and built at frequencies up to 370 GHz[2], [3]. This is a 2SB mixer at the highest frequencies at present.
For the 2SB mixer, we have developed and evaluated an
RF/LO coupler, which contains an RF quadrature hybrid, two LO
couplers, and an in-phase power divider (Fig. 1). We havemachined the waveguide (508μm×254μm) on only one side to
reduce the loss resulting from the misalignment of the two split
blocks.
The dimensions of the RF/LO coupler were measured
with a high precision (~0.5μm) scale. Amplitude and phasecharacteristics of the RF/LO coupler were also measured with avector network analyzer. The simulated results from themechanical measurements were almost consistent with themeasured results with the vector network analyzer. The
differences between these results were within 0.5 dB in amplitude,
30

Figure3: (a) Image rejection ratio, (b) single-sideband (SSB) noise
temperature of the ALMA Band 8 cartridge-type receiver [4] using
the 2SB mixer.

10 degrees in phase, respectively.
The image rejection ratio (IRR) and the single-sideband (SSB)
noise temperature of the ALMA Band 8 cartridge-type receiver [4]using the 2SB mixer were measured. The IRR was larger than 9.5
dB and typically 15 dB in the 385-500 GHz band (Fig. 3a).
The SSB noise temperature was around 5 times the quantum
limit at 435 GHz, and less than 14 times the quantum limit in the385-500 GHz band (Fig. 3b). We have achieved a broad-band andlow-noise receiver which meets almost the ALMA specification.
The SIS mixers in the receiver were developed by Shan et al. [5].
References[1] Kamikura, M., et al.: IRMMW, in press.
[2] Claude, S.: 2003, Proc. 14th ISSTT.
[3] Asayama. S., et al.: 2003, ALMA Memo 453.
[4] Satou, N., et al.: in preparation.
[5] Shan, W. L., et al.: 2005, IEEE Trans. AS, 15, 503.

Phoenicids in 1956 Revisited
WATANABE, Jun-ichi, SATO, Mikiya, KASUGA, Toshinori（Public Relations Center, NAOJ)
The outburst of the Phoenicids observed in 1956 wasinvestigated on the basis of the dust trail theory by using the newly
linked orbit that was estimated from the asteroid 2003 WY25 andcomet D/1819 W1 (Blanpain). We find that a bundle of the trails
formed from late 18th through early 19th centuries came close to
the Earth’s orbit at the epoch of the outburst in 1956. According tosimilar calculations for 1950-2030, the situation in 1956 is provento be the best epoch for the strong display in the Phoenicids. This
result shows not only the definite association of the objects to the
Phoenicids, but also the clear reason for the sudden outburst in
1956. Although the future activity is expected in 2014, it depends
on the cometary activity of the parent object, because the related
trails are expected to be relatively new. This is a new approach to
explore the past history of cometary activities of relatively
dormant objects by inspecting the activity of related meteor
showers, with a help of the dust trail theory [2].
References[1] Huruhata, M., & Nakamura, J.: 1957, Tokyo Astron. Bull. Second ser. 99,
1053.
[2] Watanabe, J., Sato, M., & Kasuga, T.: 2005, PASJ, 57, L45-L49.

Figure1: The geometrical relation between the dust trails and Earth’s orbit in
1956. Upper panel shows those trails formed before 1830, while thelower panel after 1856. Two lines indicate the duration of theoutburst summarized by
1) Kronk(http://comets.amsmeteors.org/meteors/showers/phoenicids.html,
2005) and2) Huruhata and Nakamura [1],including the epoch of the activity peak reported.

31

Size Distribution of Faint Jovian L4-Trojan Asteroids
YOSHIDA, Fumi, NAKAMURA, Tsuko(NAOJ)
Jovian Trojans are asteroids located at a mean distance of 5.2
AU from the Sun. They share the orbit of Jupiter but lead or trail
the planet by an angular distance of ~60˚; they lie clustered around
Jupiter’s L4 and L5 Lagrangian points. It has been believed thatthey originated from planetesimals that formed near Jupiter andwere captured into their current orbits, while proto-Jupiter was still
growing. Therefor if there is some possibility that some
information around Jupiter of early Solar system still remains tillnow, it may be on the Jovian Trojans. As a first step, weinvestigated the size distribution of the Trojans, in particular very
faint members of them for getting some information of early Solarsystem.
We detected faint 51 Jovian Trojan asteroids in the L4
Lagrangian swarm in a wide-field survey near the ecliptic with the
8.2m Subaru telescope and Suprime-Cam [1]. The survey area was2
about 3 deg and located ~ 30 deg in longitude ahead from the L4
point. The limiting magnitudes for our Trojan asteroids were R＝24.4 mag. The size range of the detected Trojans is 0.7km＜D＜
12.3km in diameter (D) (with an assumed albedo of 0.04 for eachobject, which is the mean albedo among known Trojans).
The mean slope of the cumulative size distribution, namely thepower-law distribution index, was found to be 1.9±0.1 for the
Trojans with 2km＜D＜10km. However, we noticed the slopechanges around D ~ 5km. The separately best-fitted slopes for thesize ranges of 2km ≤ D ＜5km and for 5km＜D ≤10km were 1.3± 0.1 and 2.4 ± 0.1, respectively. This changing nature of slope
have also been found in the size distribution of km-to-subkm
main-belt asteroids [2], it seems to be caused by collisional
evolutions among the initial population having single power-law
size distribution.
Using the size distribution of our Trojans and the spatial
distribution model of the L4 Trojans proposed by [3], we
estimated a total population number of the L4 Trojans with D＞
1km. We found that the total number of the L4 Trojans with D＞
5
1km (~ 6×10 ) is comparable to that of the main-belt asteroids
5
with D＞1km (~ 6.7×10 , [4]).

Figure1: Ecliptic longitude and latitude components of apparent motions for1111 moving objects detected in this survey. There are 861 MBAs,
10 Hildas, 51 Trojans and others. This figure is the same as Fig. 4 of[1], [2].

References[1] Yoshida, F., et al.: 2005, AJ, 130, 2900.
[2] Yoshida, F., et al.: 2003, PASJ, 55, 701.
[3] Jewitt, D. C., et al.: 2000, AJ, 122, 2099.
[4] Ivezić, Z., et al.: 2001, AJ, 122, 2749.

Figure2: The CSD of detected L4-Trojans (filled dots with error bars) and
fitted curves. Our detection limit for Trojan asteroids lies in the H＝17.7-bin. The dotted and dashed lines show the slope of 2.39 forasteroids with D＞5km, and that of 1.28 for D＜5km, respectively.
We used the red solid line which connected smoothly between bothslopes to estimate the number of the L4 Trojans with D＞1km [1].

32

Near-Infrared Imaging Survey of Bok Globules: Density Structure
KANDORI, Ryo, NAKAJIMA, Yasushi, TAMURA, Motohide, TATEMATSU, Ken’ichi(NAOJ)AIKAWA, Yuri

NAOI, Takahiro

SUGITANI, Koji

(Kobe University)(JAXA)(Nagoya City University)

NAKAYA, Hidehiko

NAGAYAMA, Takahiro, NAGATA, Tetsuya(NAOJ)(Kyoto University)

KURITA, Mikio, KATO, Daisuke, NAGASHIMA, Chie, and SATO, Shuji(Nagoya University)
We conducted a JHK s imaging survey of Bok globules(isolated dense cores) using the infrared camera SIRIUS on the
IRSF 1.4 m telescope in South Africa. On the basis of dust
extinction (AV∝column density) measurements of both starlessand star-forming globules, we investigated their density structureusing the Bonnor-Ebert model. We report important findings on
the density structure, stability, and evolution of globules [1].
The Bonnor-Ebert sphere model ([2], [3]) describes a pressureconfined, self-gravitating isothermal gas sphere in hydrostatic
equilibrium. The dimensionless radial parameterξmax determines
the shape of a Bonnor-Ebert density profile as well as the stabilityof the equilibrium state, e.g., the solution ofξmax＞6.5 is unstable
to the gravitational collapse. The model well fits column density
profiles of observed globules (Fig. 1), and physical properties
includingξmax of each globule were derived. We investigated thestability of globules on the basis ofξmax for ten globules from ourobservations and four globules in the literature (Fig. 2). The
sample consists of 11 starless and 3 star-forming globules. In
addition to the near-infrared imaging, we have carried out radio
molecular line observations toward the ten globules using the
NRO 45 m telescope, and found that the globules are mostly
dominated by thermal support.
(1) We found that more than half of the starless globules (7 outof 11 sources) are located near the critical state,ξmax＝6.5±2. We
suggest that a nearly critical Bonnor-Ebert sphere characterizes the
typical density structure of starless globules, and it approximatesthe initial condition of gravitational collapse.

Figure1: Radial column density profile of the globule FeSt 1-457. The solidline denotes the best-fit Bonnor-Ebert profile which is convolved to
the resolution of AV map (33"). The broken line denotes 1σ
detection limit. Inset figure shows the JHKs-composite image of theglobule.

Figure2: The solid line shows the relationship betweenξmax and density
contrast (center-to-edge density ratio). Filled and open black circles
denote starless and star-forming globules, respectively. The verticaldashed line denotes critical state ofξmax=6.5.

(2) We found that four out of eleven starless globules show
clearly unstable states (ξmax≫6.5). Since unstable equilibrium
states should not be long sustained, we expect that they are alreadycollapsing toward higher central condensation or that extra force(e.g., magnetic and/or turbulent pressure) accounting for largeξmax
stabilizes the globules (e.g., [4]). It was also found that all three
star-forming globules have unstable solutions, which is consistent
with the fact that they have started gravitational collapse.
(3) We investigated the collapse of the Bonnor-Ebert spherefrom a nearly critical state using the model calculation [5], andfound that the column density profiles of the collapsing sphere
mimic those of static Bonnor-Ebert spheres (unstable equilibrium
solutions). By relatingξmax to the collapsing sphere at a specifictime, the evolutionary state of globules can be interpreted, and thedetection probability of eachξmax value can be predicted from themodel calculation. Since the evolutionary timescale decreases withincreasing density, the collapsing sphere resembles a marginallyunstable Bonnor-Ebert sphere for a long time. It was found that thefrequency distribution ofξmax for the observed starless globules is
consistent with that from model calculations of the collapsingsphere.
References[1] Kandori, R., et al.: 2005, AJ, 130, 2166.
[2] Bonnor, W. B.: 1956, MNRAS, 116, 351.
[3] Ebert, R.: 1955, Z. Astrophys., 37, 217.
[4] McKee, C. F., Holliman, J. H., II.: 1999, ApJ, 522, 313.
[5] Aikawa, Y., et al.: 2005, ApJ, 620, 330.

33

Extremely high-velocity gas in a merginggalaxy Arp 220
revealed with ammonia absorption lines
TAKANO, Shuro, NAKANISHI, Kouichiro(Nobeyama Radio Observatory, NAOJ)

NAKAI, Naomasa(University of Tsukuba)

TAKANO, Toshiaki(Chiba University)
We observed ammonia toward a merging galaxy Arp 220 with
the Nobeyama 45-m radio telescope. We report detection of
extremely wide absorption lines [1].
Arp 220 exists at ~ 77Mpc, and it is quite gas rich. It shows
12
strong emission at far-infrared wavelength (~ 10 solar
luminosity). It is a prototypical ultraluminous infrared galaxy. At
the center, two nuclei have been found, indicating that they are stillin the process of merging two galaxies.
Observations were carried out with the Nobeyama 45-m radio
telescope in May 2004. The receiver was equipped with cooled
HEMT amplifiers for both circular polarizations. The four
inversion transitions of (J,K)＝(1,1), (2,2), (3,3), and (4,4) at the23.7-24.1 GHz region (rest frequency) in both polarizations wereobserved simultaneously. The spectra were obtained using
acousto-optical spectrometers. The bandwidth of each
spectrometer was 250 MHz.
The absorption lines were detected for all four transitions (Fig.
1, the (4,4) line is tentative). The (1,1) and (2,2) lines areoverlapped each other, but the (3,3) line is not overlapped. The
total width of the (3,3) absorption lineis extremely broad 〜 1800
km s−1 (approximate value obtained at the present signal-to-noise
ratio). The widths of the (3,3) and (1,1) lines are extremely broad.
Such extremely wide molecular absorption lines were detected forthe first time in galaxies.
The rotational temperature of ammonia was calculated to be ~42K from the (1,1) and (2,2) absorption lines. The total column
17−2
density obtained is ~ 2×10 cm . This is the highest value inexternal galaxies.
There are two remarkable points in the present study. First, thewidth, itself, is quite large. Second, the lines are observed inabsorption. Absorption lines are formed by foreground gas only infront of the continuum emission. The size of the strong central
continuum in Arp 220 is ~ 1". The wide absorption lines,
therefore, indicate extremely high-velocity motion near the center.
There are three possibilities to explain this extremely high-velocity
motion. The first is that gas is rapidly rotating around the nuclear
region. In such a case, the present situation may be partly similar
to that of extremely high-velocity water masers at the active−1
galactic nucleus in NGC 4258 (±1000 km s offset from thecentral velocity). Using this maser emission, they found evidence
for a massive black hole[2], [3]. In the aspect of velocity, thepresent results are similar to those in NGC 4258 suggesting theexistence of an AGN in the central region. The second possibility
is extremely high-velocity out flowing or inflowing gas at thenuclear region. In optical and X-ray observations the emissions
from atomic gas were found to be extended. However, it is not
sure whether the corresponding molecular gas exists. The third
possibility is violent turbulence of gas, which may be caused near
the colliding merging nuclei.
34

Figure1: Spectra of ammonia in Arp 220. The horizontal axis is velocity, andthe vertical axis corresponds to intensity. Smooth curves are resultsof Gaussian fit.
References[1] Takano, S., et al.: 2005, PASJ, 57, L29.
[2] Nakai, N., Inoue, M., Miyoshi, M.: 1993, Nature, 361, 45.
[3] Miyoshi, M., et al.: 1995, Nature, 373,127.

Discovery of Circumstellar Disk around a Massive Protostar by the
Subaru Telescope
JIANG, Z., YANG, J.

TAMURA, Motohide, SUTO, Hiroshi, ISHII, Miki

(Purple Mountain Observatory)(NAOJ)

FUKAGAWA, Misato

HOUGH, J., LUCAS, P.

(University of Tokyo)(University of Hertfordshire)

The formation process for stars with masses several times thatof the Sun is still unclear. The two main theories are mergers ofseveral low-mass young stellar objects, which requires a highstellar density, or mass accretion from circumstellar disks in thesame way as low-mass stars are formed, accompanied by outflows
during the process of gravitational infall. Although a number ofdisks have been discovered around low- and intermediate-mass
young stellar objects, the presence of disks around massive youngstellar objects is still uncertain.
One of the best methods for distinguishing these two
hypothesis is to directly detect a compact circumstellar disk
around massive a YSO. However, massive stars are rarer thanlow-mass stars, and massive YSOs are distant in general. The
nearest massive YSOs are situated at a distance of 450 pc, about
three times farther than the typical nearest low-mass YSOs. Since
the expected accretion disk has a scale of 100 to a few 100 AU, aspatial resolution of 0.1 arcsec is necessary.
Such a high resolution has not been achieved yet at
submillimeter or millimeter wavelengths, while it is difficult topenetrate the heavy extinction in the star forming regions at optical
wavelengths. Although adaptive optics (AO) observations on 8-mclass telescopes can achieve ~ 0.1 arcsec resolution, the central
massive YSOs are too bright for direct imaging to detect faintcircumstellar nebula.
We have conducted high resolution (0.1 arcsec) near-infrared
imaging polarimetry with the adaptive optics, an IR camera(CIAO), and its polarimeter on the Subaru telescope [1]. Figure 1
shows the polarization image of the BN object at 1.6μm [2]. The
background shows a pseudo-color image of degrees ofpolarization, the red vectors correspond polarization angle and its
degree, and the white contours show surface brightness.
While the surface brightness only show a circular structure near
the central star except for the outer elongation, the polarization
images clearly show the presence of an outflow/disk system
around the Becklin-Neugebauer protostellar object, which has amass of at least seven solar masses. Subsequent Monte-Carlosimulations well reproduce such structures. This strongly supports
the theory that stars with masses of at least 7 solar masses form inthe same way as lower mass stars.
High resolution polarimetry is thus proven to be a powerfultool to detect circumstellar disks around massive YSOs and can beused to test the accretion hypothesis for more massive (＞10 solar
masses) stars.

Figure1: Polarization image of the Orion BN object obtained with the Subaru
telescope, adaptive optics (AO), IR camera (CIAO), and its
polarimeter. The observed wavelength is 1.6μm (H band).

References[1] Tamura, M., et al.: 2003, SPIE, 4843, 190.
[2] Jiang, J., et al.: 2005, Nature, 437, 112.

35

Observations of Giant Silhouette Envelope Object M17-SO1
SAKO, Shigeyuki, MIYATA, Takashi, KAMAZAKI, Tsuyoshi(Institute of Astronomy, University of Tokyo)

YAMASHITA, Takuya, FUJIYOSHI, Takuya, TERADA, Hiroshi(Subaru Telescope, NAOJ)

KATAZA, Hirokazu, HONDA, Mitsuhiko(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)

OKAMOTO, K. Yoshiko

JIANG, Zhibo(Institute of Astrophysics and Planetary Sciences, Ibaraki University)(Purple Mountain Observatory)

HANAWA, Tomoyuki

ONAKA, Takashi(Center for Frontier Science, Chiba University)(Department of Astronomy, University of Tokyo)

Circumstellar envelopes are the main source of mass supply to
protoplanetary disks, which are cradles of planets, as well as to thecentral star. A mixture of dynamical forces induced by rotation,
turbulence, magnetic field, and outflows will affect the envelopes
forming protoplanetary disks [1]. Therefore, observational studiesof these structures are crucial in understanding how eachmechanism influences the disk formation processes to produce thevariety of sizes and structures seen in protoplanetary disks [2].
Structures of envelopes extended to a few thousands of AU in
radius around class 0/I protostars (＜105 yr) have been observedwith radio interferometers and infrared observations [3], [4].
However, the present radio interferometers do not posses sufficientspatial resolution to make it clear how mass is transferred from theenvelope to the disk. Although scattered light around the central
star is a better tool to study the structure at high resolution, wholearea of the envelope cannot be traced with the scattered light alone
because of its decreasing brightness away from the central star.
The problem with the scattered light can be resolved by using
the silhouette of the envelope against a uniformly extended nebula
since it provides a light source even in distant areas away from thecentral star. We focused on this merit and carried out survey
observations at the Subaru telescope for silhouette objects in the
M17 star-forming region. We used the 2.166-μm Brγ emission
line as the background light and discovered a giant silhouetteobject M17-SO1 (Fig. 1) [5].
In follow up observations in the JHK bands, and at midinfrared at the Subaru telescope and millimeter wavelengths at the
Nobeyama millimeter array, M17-SO1 is revealed as anintermediate class I protostar of 2.5 to 8 solar masses. The
silhouette image against the uniform background light source not
only derives the exterior appearance but also the column density
distribution. The envelope consists of two components - an innerdense part and an outer less dense part, whose masses are
estimated to be 0.006 and 0.08 solar masses, respectively. The
radial distribution of scale height of the envelope also indicatesthat the central star is heavier than 2.5 solar masses. Four darkarms are seen in the silhouette image. They tightly enclose thenebulosity due to scattering and are clearly separated from theflared structure of the envelope. The geometrical appearance
suggests that the four arms are produced by bipolar outflows
because this kind of structure is typical of systems associated with
outflows.
The fact that the four arms are detached from the flared
structure indicates that its scale height is determined not by thepressure from outflows but by the dynamical equilibrium between

36

Figure1: (top) JHK pseudo-colour image of M17-SO1. This image wasobtained by the IRCS with the adaptive optics system at the Subaru
telescope on 15 Aug. 2003. The image area is 14.8 arcsec×7.4
arcsec. (bottom) Silhouette image of M17-SO1 against the Brγ(2.166μm) emission. The image area is the same as in the top image.

gravity of the central star and forces induced by pressure gradient,turbulence motion, and magnetic field. This suggests that thematerials in the envelope fall to the centre not through direct pathbut through nearby disk mid-plane.
References[1] Shu, F. H., et al.: 2000, in Protostars and Planets IV, 789.
[2] Mundy, L. G., et al.: 2000, in Protostars and Planets IV, 355.
[3] Ohashi, N., et al.: 1996, ApJ, 466, 317.
[4] Padgett, D. L., et al.: 1999, AJ, 117, 1490.
[5] Sako, S., et al.: 2005, Nature, 434, 995.

Forthcoming Launch of the SOLAR-B Spacecraft
KATSUKAWA, Yukio, ASAI, Ayumi, ICHIMOTO, Kiyoshi, KATO, Yoshihiro
KANO, Ryouhei, KUMAGAI, Kazuyoshi,SHIMOJO, Masumi, SUEMATSU, Yoshinori
TAMURA, Tomonori, TSUNETA, Saku, TONOOKA, Hideaki, NOGUCHI, Motokazu
NAKAGIRI, Masao, HARA, Hirohisa, MIYASHITA, Masakuni, WATANABE, Tetsuya(NAOJ)KOSUGI, Takeo, SAKAO, Taro, SHIMIZU, Toshifumi,
MATSUZAKI, Keiichi, KUBO, Masahito(JAXA / ISAS)

Figure1: SOLAR-B spacecraft when the front door of Solar Optical
Telescope (SOT) was opened. SOT was located at the center, X-Ray
Telescope (XRT) on the lower right, and EUV Imaging
Spectrometer (EIS) on the upper left.

The Solar-B Project Office of the National Astronomical
Observatory of Japan (NAOJ) contributes to system design andspacecraft-level performance testing of all the mission instruments,
developments of the Optical Telescope Assembly (OTA) in the
Solar Optical Telescope (SOT) and the CCD camera of the X-ray
Telescope (XRT), and spacecraft-level contamination control in
the SOLAR-B project with the Institute of Space andAstronautical Science of Japan Aerospace Exploration Agency(ISAS/JAXA). The office also plays a role of the interface
between the spacecraft system and foreign partners in US and UK.
After the electrical and mechanical interface testing in 2004, three
mission instruments were disintegrated and were returned to
institutes in charge. After fixing the problems found in the test, all
the flight models were gathered in the clean room of ISAS in June
2005. The integration was performed so that the optical axes
among three telescopes and sun-censors were aligned; the
SOLAR-B spacecraft became a final form ready for launch (Fig.
1).
From August 2005, the electrical performance test was carriedout for the three mission instruments and the spacecraft bus
instruments, and it was completed without problems. The
mechanical environment test was carried out in October 2005 toverify healthiness of the spacecraft against rocket launch
environment. We confirmed that alignment among the telescopes
and the electrical performance did not change during themechanical environment test. The thermal vacuum test was
performed in March 2006 at the ISAS space chamber (Fig. 2)
where the thermal environment on orbit was simulated. In this test,

Figure2: SOLAR-B spacecraft at the ISAS space chamber just before thethermal vacuum test. The satellite was surrounded by aluminium
frames equipped with test heaters to control outer temperatures.

we verified healthiness of the thermal design, function oftemperature control systems, and electrical performance in thethermal vacuum environment. We completed all theenvironmental tests required for launch.
In parallel with the spacecraft tests, Solar-B project office built
Solar-B Science Center (SBSC) in NAOJ aiming to provide
scientific analysis environment for researchers. We started
development of analysis software and hardware in SBSC. We
organized a SOLAR-B workshop in February 2006 for domestic
researchers so that they would know what kind of data will beobtained by SOLAR-B.
In the next fiscal year, the final performance test is carried out
until July 2006 in the clean room of ISAS, then the spacecraft istransported to Uchinoura Space Center (USC). The spacecraft
launch operation starts at USC from August 2006. In the end of
September, the SOLAR-B spacecraft will be launched by the M-Vrocket, and installed to a sun-synchronous polar orbit of altitude
about 680km.

37

Expanding Radio Lobe Revealed by VSOP Observations
ASADA, Keiichi, KAMENO, Seiji, INOUE, Makoto(NAOJ)

SHEN, Zhi-Qiang

HORIUCHI, Shinji

GABUZDA, Denise C.

(SAO)(Swinburne University of Technology)(University College Cork)

Figure2: (left) Size of the radio structure is plotted against time. Open circles
represent our VSOP observations, and the others are obtained byprevious VLBI observations. (right) The light curve of 3C 84 at 5
GHz observed by UMRAO with fitting results for adiabatic
expansion.

Figure1: The contours show the total intensity at second epoch and the color
scale shows the distribution obtained by dividing of total intensity
image at the second epoch by that of the first epoch. The increasingof the flux at the south edge in the second epoch clearly shows the
expansion of the radio lobe.

We report the detection of the expansion of a young radio lobe
associated with the bright radio source 3C 84 in the Seyfert galaxy
NGC 1275 with VSOP observations [1].
Compact Symmetric Objects (CSOs) have similar structure to
those of the classical double radio sources, but sizes of CSOs are
103 times smaller than those of the classical double radio sources.
The compact structure of CSOs led a hypothesis at those are on ayoung stage of evolution to a large classical double radio lobe.
The compact radio source 3C 84, hosted by the Seyfert galaxy
NGC 1275, is one of the strongest radio sources. Since it is anearby (z＝0.018) source, 1 mas corresponds to 0.4 pc. Early
VLBI observations revealed that 3C 84 had a complicated radio
structure on parsec scales, consisting of a bright core with a flat
spectrum and a complex structure of the southern radio lobe with asteep spectrum. Single dish observations of 3C 84 show that theoutburst started at 1959, and total flux density showed several
peaks in the mid-1980’s and is now in a decay phase [2]. In orderto reveal the evolution of radio lobe, we performed VSOP
monitoring observations towards 3C 84.
As the results, we imaged well resolved structure of thesouthern radio lobe and detected its expansion (see Fig. 1, Fig. 238left). If we assume that the southern radio lobe is expanding withconstant velocity, the source size extrapolated back to zero atabout the time of the 1956 and thus we estimated an expansion
velocity of 0.50±0.11 c. Then, this southern radio lobe is one of
the youngest radio lobes with 40 yrs old. In addition, the epochcoincidentally corresponds to the beginning of the outburst event
detected by single dish observations.
In order to discuss the origin of the decay of the total flux
density, we consider the efficiency of the expansion cooling andsynchrotron cooling of the radio lobe. We found that the decay of
total flux density can be naturally explained by an adiabatic
cooling due to the expansion of the radio lobe, if we assume thatthe emitting region is the surface of the radio lobe and no injectionof relativistic electron at the hotspot and jet components due to insitu acceleration. It is consistent with the picture suggested by Xray observations [3]. On the other hand, we ruled out thesynchrotron cooling, because we need B> 48 mG to see such aneffect and that is a little stronger than the equipartition magnetic
field suggested for the radio lobes of CSO objects
References[1] Asada, K., et al.: 2006, PASJ, 58, 261.
[2] Nesterov, N. S., et al.: 1995, A&A, 296, 628.
[3] Tashiro, M., et al.: 1998, ApJ, 499, 713.

Near-infrared deep imaging of Subaru Supe Deep Field
using Adaptive Optics
MINOWA, Yosuke, KOBAYASHI, Naoto, YOSHII, Yuzuru(Institute of Astronomy, University of Tokyo)

TOTANI, Tomonori, MAIHARA, Toshinori, IWAMURO, Fumihide(Kyoto University)

TAKAMI, Hideki, TAKATO, Naruhisa, HAYANO, Yutaka,
TERADA, Hiroshi, OYA, Shin, IYE, Masanori(Division of Optical and Infrared Astronomy / Subaru Telescope, NAOJ)

Tokunaga, Alan T(University of Hawaii)
We present a deep K’-band (2.12μm) imaging of the 1’×1’
Subaru Super Deep Field (SSDF) taken with the Subaru adaptive
optics (AO) system [1]. AO compensates the disturbed wavefront
by Earth’s atmosphere and provides nearly diffraction-limited spatial resolution. Because the flux in the diffraction-limited corelargely increases, it is expected to improve the sensitivity ofdetecting faint objects with AO. Total integration time of 26.8 hr
results in the limiting magnitude of K’= 24.7 (5σ, 0".2 aperture) for
point sources, which is the deepest limit ever achieved in the K’band (Fig. 1). The average stellar FWHM of the co-added image isabout 0".18, which is comparable to or even smaller than thatobtained with the Hubble Space Telescope in the near infrared.
We obtained the differential galaxy number counts down to K’~ 25, which is more than 0.5 mag deeper than the previous data
and then the faintest number count data ever obtained (Fig. 2). We
found that the number count slope d log N/dm is about 0.15 at 22＜K’＜25, which is flatter than the previous data. This flatter slope
at the faint-end (K’＞22) rejects earlier theoretical studies thatpredict further increase of the number counts beyond K’ ~ 23because of a large number of faint blue dwarf galaxies [2] or larger
cosmic density at high-redshift than today [3].
The isophotal size distribution of the galaxies was obtained
from the K’-band SSDF image down to the area size of less than2
0.1 arcsec , which is less than half of that of the previous data in
the K’-band. We compared the observed galaxy size vs. apparent
magnitude relation with a simple pure luminosity evolution modelallowing for intrinsic size evolution and found that a model withno size evolution gives the best fit to the data. It implies that thesurface brightness of galaxies at high redshift is not much different
from that expected from the size-luminosity relation of presentday galaxies.
References[1] Minowa, Y., et al.: 2005, ApJ, 629, 29.
[2] Babul, A., Ferguson, H. C.: 1996, ApJ, 458, 100.
[3] Tomita, K.: 1995, ApJ, 451, 1.
[4] Djorgovski, S., et al.: 1995, ApJ, 438, L13.
[5] Bershady, M. A., et al.: 1998, ApJ, 505, 50.
[6] Labbe, I., et al.: 2003, AJ, 125, 1107.
[7] Maihara, T., et al.: 2001, PASJ, 53, 25.

Figure1: IRCS+AO K’-band image of the SSDF. The field size is about 1'×
1'.

Figure2: Differential K’-band number counts of galaxies estimated from the
SSDF. For purposes of comparison, the counts in the literature([4],[5],[6],[7]) are also plotted.

39

Reverberation Measurements of the Inner Radius of the Dust Torus
in Nearby Seyfert 1 Galaxies
SUGANUMA, Masahiro

YOSHII, Yuzuru

KOBAYASHI, Yukiyasu(JASMINE Project Office, NAOJ)(University of Tokyo)(JASMINE Project Office, NAOJ)

MINEZAKI, Takeo(University of Tokyo)

ENYA, Keigo(JAXA)(University of Tokyo)

KOSHIDA, Shintaro

PETERSON, Bruce A.

(University of Tokyo / NAOJ)(Australian National University)

We carried out the intense monitoring observations in opticaland near-infrared wavebands for nearby Seyfert 1 galaxies using
MAGNUM telescope. Clear time-delayed response of the K-band
flux variations to the V-band variations was detected for NGC
5548, NGC 4051, NGC 3227, and NGC 7469. The lag times canbe interpreted as light-travel time between the central engine andthe inner edge of the dust torus. Comparing our lag timemeasurements with other quantities (optical luminosity, central
virial mass, and broad-line lag) based on our sample and others in
the literature, we ensured next two important evidences [1].
1) The infrared lag time is tightly correlated with the opticalluminosity according to ∆t∝L 0.5
opt in agreement with the expected
relation of dust reverberation.
2) Infrared lags place an upper boundary on similar lag
measurements of broad-emission lines in the literature, which not
only supports the unified scheme of AGNs, but also implies aphysical transition from the broad emission-line region (BLR) out
to the dust torus that encircles the BLR.
The unified scheme of active galactic nuclei (AGNs) and radioquiet quasars explains that Seyfert 1 nuclei with a broad emissionline region (BLR) would be classified as Seyfert 2 if high velocity
clouds emitting broad emission lines are hidden by the dust torus
that encircles such clouds [2]. However, the angular scale of innerdust torus even in the nearest AGN is too small to be spatiallyresolved with any current technology in optical and near-infrared
imaging observations.
It is generally accepted that the near-infrared emission from
Seyfert galaxies and quasars is thermally produced by hot dust
heated to its sublimation temperature about 1500 K by UV
radiation from the central engine. This model necessarily claims adust distribution with a central hole. If we monitor their continuum
fluxes in the UV/optical and near-infrared, a lag time would be
expected that corresponds to the light-travel distance between thecentral engine and the hot dust region from which the bulk of nearinfrared emission is radiated. The most successful case of similar
technique is the reverberation mapping of the BLR carried out for
many Seyfert 1 galaxies and quasars during the last decade (e.g.,[3]). However, there have been only few cases where lag times forboth BLR and dust torus were measured for the same AGN.
Over three years of observations, after the operation of the
MAGNUM telescope started in early 2001, clear time-delayed
response of the K-band flux variations to the V-band flux
variations was detected for four galaxies including NGC 5548
(Fig. 1), after the first result in NGC 4151 [5]. We found that thelag time is tightly correlated with the optical luminosity as
0.5
expected from dust reverberation (∆ t ∝ L ), while only weakly
with the central virial mass, which suggests that an inner radius of
the dust torus around the active nucleus has a one-to-one
correspondence to central luminosity. In the lag time versus central
40

TOMITA, Hiroyuki, AOKI, Tsutomu

Figure1: Observed V and K light curves of NGC 5548 nucleus. Green and red
circles correspond to V and K, respectively. The red line is the K
light curve shifted backwards by 50 days [4].

luminosity diagram (Fig. 2), the K-band lag times place an upperboundary on the similar lag times of broad-emission lines in theliterature. This not only supports the unified scheme of AGNs, butalso implies a physical transition from the BLR out to the dust
torus that encircles the BLR.

Figure2: Lag times plotted against the absolute V magnitude of AGNs. Red
filled symbols show the infrared lags measured in this work, and red
open symbols from a literature [5]. Blue (for Hβlines) and light-blue(for other) symbols show the lag times of broad emission lines forthe corresponding AGNs in the literatures.
References[1] Suganuma, M., et al.: 2006, ApJ, 639, 46.
[2] Antonucci, R.: 1993, ARA&A, 31, 473.
[3] Kaspi, S., et al.: 2000, ApJ, 533, 631.
[4] Suganuma, M., et al.: 2004, ApJ, 612, L113.
[5] Minezaki, T., et al.: 2004, ApJ, 600, L35.

Compilation and Publication of Union Catalog for Books andMaterials on Japanese Astronomy before Meiji Era
NAKAMURA, Tsuko, ITO, Setsuko(Public Relation Center, NAOJ)
In conducting researches on the Japanese astronomy of the Edo
era (1603-1868), the first step to be done is to know whereaboutsof original books and materials on the discipline. For that purpose,it has been common that we use Kokusho Somokuroku (General
Catalog of National Books before 1868) for consultation.
However, because the main body of this catalog was compiled
before WW-II, it is likely that a non-negligible fraction of thecatalog entries has been destroyed by war-fires, or lost, or now
belong to libraries different from those described in the catalog.
Moreover, due to recent activities of local libraries, archives andmuseums in Japan for collecting and cataloging historical books
and documents and their increased efforts to publicize suchinformation via Internet services, we are in a position to havea
much easier and better access to unknown historical sources newly
acquired after WW-II.
With such background in mind, we started in 2002 as a team a
project under governmental support to compile a general catalog
of Japanese archives before 1870 on astronomy, land-surveying
and relating disciplines. An interim report of this program,including the motivation and aims of this project, had already been
made at a Commission-41 meeting of General Assembly of IAU
in Sidney [1].
The four-year efforts, with 10 domestic and three overseas
research members, to survey and inventorize Japanese
astronomical books and materials preserved at 410 domestic and24 overseas libraries and museums resulted in a book “General
Catalog of Japanese Astronomical Books and Materials in the PreMeiji Era”, published in February 2006 [2]; catalogs of such kinds
including books preserved at overseas libraries have never been
made before. This publication comprises about 6200 book titles,
with whereabouts for each. This number outnumbers by about
50% that included in the Inventory Book for Survey, which was
prepared as a basis of this survey at the start of this project [3].
With this catalog, we suppose that roughly 90% of the existingbooks and materials belonging to the above two disciplines arecovered. Although this book also includes parts of books on
Japanese mathematics (Wasan), navigation, physics andgeosciences, etc. they are not so extensive and limited to thosemainly relating to astronomy and land-surveying.
Here are some characteristics of our publication. First, we
attempted as far as possible to contain in our catalog also thebooks and materials whose whereabouts are unknown but only
cited in the literature. Second, we separated old every-year
calendars such as Guchu-reki and Ise-goyomi from our main
catalog into Appendices as an independent one; this will enhanceboth the systematic nature of this catalog and search ease.
The Japanese astronomy had heavily been affected by the
Chinese culture from antiquity till the pre-modern times. After
import-ban deregulation of foreign books by the eighth Shogun
Tokugawa Yoshimune in 1720, the Japanese began to recognize
the superiority of the European modern astronomy over the
traditional Chinese one, and gradually learned understanding thewestern astronomical books without referring to the Chinesetranslation. Because of those reasons, this book also gives inAppendices the lists of the Chinese and western books that
influenced the Japanese astronomy.
We expect that this book is of use, for an extended period oftime, in researches in the fields of history of sciences, the westerncultural transfer (Yogaku), as well as in the history of astronomy
and land-surveying.
References[1] Nakamura, T.: 2004, Journal of Astronomical Data, 10, 55-65.
[2] Nakamura, T., Ito, S., eds.: 2006, Meiji-zen Nihon Tenmon-rekigaku,
Sokuryo no Shomoku Jiten (General Catalog of Japanese AstronomicalBooks and Materials in the Pre-Meiji Era), pp 335＋32.
[3] Nakamura, T., ed.: 2002, Tenmon-rekigaku, Sokuryo, Kokai, tou no Washo
Mokuroku (Inventory Book for Survey), pp 243.

41

First Fringe Measurement of `OHANAPERRIN, Guy

KOTANI, Takayuki(Observatoire de Paris)(Subaru Telescope, NAOJ / University of Tokyo)

GUYON, Olivier

NISHIKAWA, Jun(Subaru Telescope, NAOJ)(MIRA Project Office, NAOJ)

Other 31 Co-Authors
We report the success of the first interferometric observation ofthe `OHANA (Optical Hawaiian Array for Nanoradian
Astronomy) project.
The `OHANA project aims at linking large telescopes on
Mauna Kea, including Subaru, by using single-mode optical fiber
to construct an infrared interferometer uniquely combining long
baselines (up to 800-m) with large individual apertures [1]. The
project was started in 2000. Figure 1 shows telescopes which will
be used for `OHANA and possible baselines. As `OHANA utilizes
existing telescopes equipped with Adaptive Optics, large andsensitive infrared array can be build easily. The sensitivity of`OHANA can be comparable with the next-generation infraredinterferometer, VLTI (Very Large Telescope Interferometer) and
Keck Interferometer, and its angular resolution is at least 4 times
higher. `OHANA will give us critical information on the central
region of YSO (Young Stellar Object) and AGN (Active Galactic
Nucleus) by direct imaging [2]. The spatial resolution of `OHANA
corresponds to 0.05 ~ 0.8 AU at the nearby star-formation region(150 pc), which enables us to observe the origin of jets, interaction
between disk and star, and even stellar diameter. For nearby AGN(10Mpc), `OHANA can resolve 0.02 ~ 0.3 pc scale, whichcorresponds to the size of BLR (Broad Line Region) and inner
region of dust torus.

Figure1: Telescopes used for `OHANA on Mauna Kea and possible
baselines.

We carried out the interferometric observation in June 2005 byconnecting the two Keck telescopes (85-m baseline) with the 300m K-band fibers which replaced bulk-optics beam train (i.e.
mirrors to transport beams) [3]. The starlight was injected into thefibers near the AO focuses in the Nasmyth platform, and fibers
were attached to the telescope structures and going down to theinterferometric laboratory in the basement. The delay lines andbeamcombiner of the Keck interferometer were used. The first
fringes, shown in Figure 2, were obtained on the star 107 Her(A7V, K magnitude＝4.6). The apparent fringe contrast, i.e.
42

Figure2: Fringes on 107 Her (A7V, K magnitude＝4.6). Data is high-passfiltered in order to remove the effect of photometric fluctuation.

visibility was 0.26, which is rather low considering the almost
unresolved angular diameter of 107 Her. Apparent fringe visibility
is usually lower than the ideal value due to imperfect optics,
mismatch of the polarization states, etc. For this observation, thedegradation of visibility was caused by the chromatic dispersion
arising from the different dichroich mirrors in the AO system of
the two Keck telescopes. These dichroic mirrors can be easily
replaced: we therefore expect to obtain much higher visibility forthe next observations.
The light transmission of `OHANA was measured to be 0.5%
but it is a lower limit because of the bad weather. In the clear sky
condition, a 4% transmission is expected and can be increased up
to 10% by improving optics. For comparison, Keckinterferometer’s transmission, with the more traditional beamtransfer optics, is 1%. Therefore, `OHANA will be potentiallymuch sensitive than the non-fiber configuration.
The success of this first `OHANA baseline demonstration is an
important step toward a 800-m baseline interferometer withmultiple baselines and large telescopes atop Mauna Kea. We will
carry out our next step, the CFHT-Gemini interferometricobservation, at the end of 2006. We also expect to combine theSubaru and two Keck telescopes within a few years.
References[1] Perrin, G., et al.: 2003, SPIE, 4838, 1290.
[2] Lai, O., et al.: 2003, SPIE, 4838, 1410.
[3] Perrin, G., et al.: 2005, Science, 311, 194.

Combination of Nulling Interferometer and Modified Pupil for
Observations of Exo-Planets
NISHIKAWA, Jun

KOTANI, Takayuki

MURAKAMI, Naoshi, BABA, Naoshi(MIRA Project Office, NAOJ) (Observatorie de Paris / University of Tokyo)(Hokkaido University)

ITOH, Yoichi

TAMURA, Motohide(Kobe University)(Division of Optical and Infrared Astronomy, NAOJ)

Very high dynamic range observations are required especiallyfor the direct detection of extra-solar planets, which have a−9contrast of less than 10 at a distance of about 0."1 from thecentral star. We proposed to use a nulling interferometer as preoptics combined with a modified pupil telescope to achieve highperformance coronagraph (Fig. 1 ; see [1] more details).
Nulling interferometry is one of the useful methods ofachieving high dynamic range observations. Another method is themodified pupil, which suppresses the halo of the diffraction imageof a point source relative to the core intensity, and others are theadvanced nulling coronagraphs. The nulling interferometer can
produce the total extinction for an on-axis point source but it
transmits leakage light for a resolved star with off-axis rays. The
residual wavefront is still flat and we consider it can be combinedwith the next high dynamic range method for a single telescope.
With the combination presented here, the effects of the nullinginterferometer and the modified pupil are independent and they are
multiplied, resulting in higher dynamic range than either methodby itself.
For the source intensity reduction effect of the nullinginterferometer (e.g. 10−3) in the combination methods to reach the−10desired total dynamic range of 10 , the modified pupil is−7
required to provide a lower contrast halo suppression (e.g. 10 )which is a welcome situation for helping exo-planet-finding
telescopes to reduce the image core radius (e.g. ≤ 3λ/D) by themodified-pupil and to increase throughput (Fig. 2).
The present combination is useful for the case where thediffraction image core radius of each element telescope is a few
times smaller than the separation angle of the target exo-planet
from the central star.
An example of the condition is a 600nm wavelength
observation of a Sun-Earth-like system at a distance of 10 pc, with
an apparent stellar diameter of 1 mas and a separation between thestar and the planet of 100 mas, using a 3m baseline interferometer
which is composed of two 3m sub-apertures with a diffraction
limit of 41 mas extracted from a 6m telescope.
A nulling interferometer is shown to work as pre-optics which
reduces the source intensity in front of any single telescope optics,
just like the modified pupil method and the modern nulling
coronagraph method. An additional nulling operation is applicablewhen the wavefront at the output pupil plane for each point of theresolved source has a uniform distribution after any previous
nulling operation.
In analogy with the present concept, it is important toinvestigate various optical designs and combinations which have
not yet been explored but have the potential to achieve higher
dynamic range than that obtained by presently known methods
and combinations. We are interested in making modifications toknown methods including the proposals of the present paper inorder to achieve high dynamic range with available opticalcomponents.

Figure1: Coronagraphic optics by pre-optics nulling interferometer combinedwith modified pupil method.

Figure2: Intensity profiles along the high-contrast axis for combinations ofnulling interferometer with modified pupils. The profiles for threemodified pupil under nulling interferometer destructive conditions
are shown (1, 2, 3). In the case of the circular aperture we show bothconstructive condition (4) and destructive nulling condition (5).

References[1] Nishikawa, J., et al.: 2005, A&A, 435, 379.

43

Development of 187Re-187Os nucleo-cosmochronometerfor r-process in supernovae [1]
HAYAKAWA, Taketo

SHIZUMA, Toshiyuki(JAEA / NAOJ)(JAEA)

KAJINO, Toshitaka(NAOJ / UT / GUAS)CHIBA, Satoshi, SHINOHARA, Nobuo, NAKAGAWA, Tsuneo(JAEA)

Figure1: A partial nuclear chart around a Re-Os region. Arrows are
187
187
nucleosynthesis flows. The isotope Re decays to Os with a halflife of 44 Gyr. The nucleus 187Re should be produced by a new s186
process path though the Re isomer (dot-line arrow).

Long-lived radioactive isotopes are used as nucleocosmochronometers, which are useful for an investigation of
nucleosynthesis process and the solar system formation. The
radioactive nuclei of cosmological significance are rare and only
six chronometers with half-lives in the range of the cosmic age 1 ~100 Gyr were proposed. They are 40K [2] and 87Rb [3] for the s176
process or explosive nucleosynthesis in supernovae, Lu [4] forthe photodisintegration reaction nucleosynthesis in supernovae,
187
232
238
and Re [3], Th and U [2] for the r-process. The nucleus
187
Re is dominantly synthesized by the r-process in supernovae but
the s-process in low-mass AGB stars also contributes to the187
abundance of Re as shown in Fig. 1 [5], [6]. We study a new s186
187
process path through an isomer of Re to improve the Re
chronometer.
186
First, we propose a new s-process path through a Re isomer187
that contributes to the abundance of Re and affect to 187Re -187Os
chronology (see Fig. 1). The neutron-capture cross-section to theisomer with the experimental uncertainty has not been reported.
Second, we measure a ratio of neutron capture cross-sections of
186
the isomer to the ground state of Re at thermal neutron energy
with neutrons provided from a nuclear reactor JRR-4. We measure186
the c-rays from the Re isomer as shown in Fig. 2. We obtain theratio of Rth＝0.54±0.11%. From this ratio we estimate the ratio of
Maxwellian averaged cross sections at kT＝30 keV by using astatistical-model. The ratio is Rst＝1.3±0.8%. We calculate the sprocess contribution to 187Re from the new path in a steady-flow
187
model. The additional abundance of Re is estimated to be Ns＝0.56±0.35% relative to the abundance of 186Os.
Finally, we calculate the effect to a sample affected strongly by187
a single supernova such as pre-solar grains [7] using the Re
chronometer. We calculate the age of such samples in a sudden
approximation under various conditions. The difference between
44

ARIMA, T(University of Tohoku)

Figure2: A measuredγ-ray spectrum from a sample after a neutron
184
irradiation. Mostγ-rays are irradiated from Re. Aγ-ray of 137
186
keV is most strongγ-ray from the Re isomer.

the ages under the different conditions is at most ~ 2%.
References[1] Hayakawa, T., et al.: 2005, ApJ, 618, 533.
[2] Burbidge. E., et al.: 1957, ReMP, 29, 548.
[3] Clayton, D. D.: 1964, ApJ, 139, 637.
[4] Hayakawa, T., et al.: 2004 PRL, 93, 161102.
[5] Käppeler, F., et al.: 1991, ApJ, 366, 605.
[6] Shizuma, T., et al.: 2005, PRC, 72, 025808.
[7] Amari, S., et al.: 1992, ApJ, 394, L34.

Sensitivity of R-Process Nucleosynthesis in Supernovae and GRBs tothe Light-Element Nuclear Reactions [1]
SASAQUI, Takahiro

KAJINO, Toshitaka(HITACHI High-Technologies Corporation)(NAOJ / University of Tokyo / GUAS)

MATHEWS, Grant J.

OTSUKI, Kaori

NAKAMURA, Takashi(University of Notre Dame)(University of Chicago)(Tokyo Institute of Technology)

Figure1: Comparison of the final r-process abundances obtained with9
different a (an, c) Be reaction rates. Three lines are for the different
rate adopted in literatures as summarized in ref. [1]. Y2nd and Y3nd
indicate the typical r-process abundances of the 2nd peak and 3rd
peak elements, respectively. The solar system r-process abundancesfrom ref. [6] are shown by filled circles.

We study the efficiency and sensitivity of r-process
nucleosynthesis to the light-element nuclear reaction rates. We
adopt empirical power-law relations [2] to parameterize thereaction sensitivities. We utilize two different hydrodynamic
models for the neutrino-driven winds in order to study thedependence of our result on supernova wind models [3]. We alsoutilize an exponential model to approximate a wide variety ofother plausible conditions for the r-process. We identify several
specific nuclear reactions among light neutron-rich nuclei that playa critical role in determining the final r-process nucleosynthesis
yields.
We also found a new concept of “semi-waiting” points among
the light neutron-rich radioactive nuclei including lithium, boron,
carbon, and oxygen isotopes. We show that not only neutron
capture and b-decay, but also (a,n) reactions are important indetermining waiting points along the r-process path.
Our numerical results from this sensitivity analysis serve
foremost to clarify which light nuclear reactions are mostinfluential in determining the final r-process abundances. We also
quantify the effects of present nuclear uncertainties on the final rprocess abundances. This study thus emphasizes and motivates
which future determinations of nuclear reaction rates will moststrongly impact our understanding of r-process nucleosynthesis.
We also studied extensively the dependence of the sensitivity
on the expansion flow models. We adopted exponential flow
models to simulate various expansion dynamics such as promptand delayed supernova explosions, gamma-ray bursts central
engines, binary neutron star or neutron star-black hole mergers,
etc. [3], [4], [5]. The four important physical parameters which

Figure2: Time evolution of carbon isotope abundances. Because of the large
measured reaction cross section for 18C(n, c)19C, the abundance of
19
C is increased compared with the abundance based upon the HF
19estimate. The accumulated abundance of C rapidly
18
photodisintegrates to C due to the small neutron-separation energy.

characterize the profile in the flow models are the dynamicaltimescaleτdyn, the entropy per baryon s/k, the initial electron
fraction Ye, and the asymptotic temperature Ta. We found that thesensitivities depend most strongly on the dynamical timescale.
Nuclear reactions and SN dynamics are thus complementary facets
to understanding r-process nucleosynthesis. We believe that thepresent work provides a useful tool to elucidate which reactions
are most important and also the synergy between the SN dynamics
and nuclear reactions in r-process nucleosynthesis.
References[1] Sasaqui, T., et al.: 2005, ApJ, 634, 1173.
[2] Otsuki, K., et al.: 2000, ApJ, 54, 424.
[3] Bahcall, J. N., et al.: 1982, Rev. Mod. Phys., 533, 767.
[4] Woosley, S. E., et al.: 1994, ApJ, 433, 229.
[5] Freiburghaus, C., et al.: 1999, ApJ, 525, L121.
[6] Arlandini, C., et al.: 1999, ApJ, 525, 886.

45

Neutrino-Effects on R-Process Nucleosynthesis
in Black-Hole Formation [1]SASAQUI, Takahiro(HITACHI High-Technologies Corporation)

KAJINO, Toshitaka

Figure1: Final abundance patterns as a function of mass number in the fourcases of different neutrino cutoff times calculated in Otsuki flow
model [2]. The cutoff times are set to be 0.001s (dashed line), 0.005
s (dotted line), 0.1 s (dash-dotted line), and ∞ (solid line). The
points indicate recent observational data of abundance ratios
232
151
153
235
238
151
153
Th/( Eu＋ Eu) and ( U＋ U)/( Eu＋ Eu) of metaldeficient halo stars [3].

Massive stars ≥ 8M culminate their evolution by supernova(SN) explosions which are presumed to be most viable candidate
for the astrophysical site of heavy r-process nucleosynthesis. If themodels for the r-process are correct, then our nucleosynthesis
results could also pose a significant constraint on the remnant of
SN explosions, i.e. neutron star (NS) or black hole (BH).
In case of massive core collapse is thought to be formed aremnant stellar black hole. Intensive neutrino flux from theneutralized core and neutrino sphere might stop suddenly during
the Kelvin-Helmholtz cooling phase because of the BH formation.
It is another current interest in astrophysics and particle physics
what kind of observable phenomena we could find from these SN
neutrinos. In several theoretical studies of particle physics, it isdiscussed that even the neutrino mass is to be determined from thetime delay of deformed neutrino energy spectrum after the ceaseof neutrino ejection (neutrino flux cutoff effect [4]).
We therefore studied expected theoretical response of the rprocess nucleosynthesis to the neutrino cutoff effect in order tolook for another independent observable of this phenomenon. We
found a pretty sensitive response of the r-process yields, especiallythe heaviest end of r-process elements such as 232Th and 238U
(actinides) as shown in Fig. 1. One obtains the biggest response if
the neutrino cutoff occurs after the critical time when the
expanding materials in the neutrino-driven wind drop out of theNSE. We found that actinide abundance profile can be fit byz = zt " 3+z1a
1 + ^t/t h
0

or by the normalized form of46

BALANTEKIN, Akim Baha(NAOJ / University of Tokyo / GUAS)（1）(University of Wisconsin)z−zt→∞
1
Figure2: Normalized abundance ratio ξ＝─＝─
vs. neutrino cutoffz
1＋(t / t )time t=t cut calculated in the exponential models which arecharacterized by the different dynamical expansion time scalesτdyn＝5, 10, 20, 30, and 50 ms of the neutrino-driven wind, as indicated.
Calculated data points are fit by universal curves. The parameter t0,
which corresponds to the time around which a drastic change of the
final abundance occurs, is proportional to the dynamical timescaleτdyn . Observed range includes both observational errors anddispersion from [3].
a

1

p=

z zt " 3 =1
az1
1 + ^t/t h

0

（2）

0

as displayed in Fig. 2 for many different SN expansion models
232151with differentτdyn. In these equations, t＝tcut, z≡ Th/( Eu＋153Eu), zt→∞ means the abundance ratio of no neutrino cutoff, andz1＋ zt→∞(≡z0) means the abundance ratio with no neutrinos, t0
means the start of the drastic change of the ratio z , and a is aconstant value. The quantity a＝3 is model independent and theother quantities are model dependent.
The r-process nucleosynthesis changes maximally if the cutoff
occurs during the r-process. Using this theoretical finding
connected with future detection of the time-variation of SN
neutrino spectrum, we are able to identify when the black holeformation occurs in the course of SN collapse and explosion.
References[1] Sasaqui, T., et al.: 2005, ApJ, 634, 534.
[2] Otsuki, K., et al.: 2000, ApJ, 533, 424.
[3] Honda, S., et al.: 2004, ApJ, 607, 474.
[4] Beacom, J. F., et al.: 2001, Phys. Rev., D63, 073011.

Primordial magnetic field constrained from CMB anisotropies
YAMAZAKI, Dai G.

ICHIKI, Kiyotomo(University of Tokyo / NAOJ)(University of Tokyo)

KAJINO, Toshitaka

MATHEWS, Grant J.

(NAOJ)(University of Notre Dame)densities, the spectral index and the amplitude of primordial scalarfluctuation, and the optical depth, in flat Universe models, using
the technique of the MCMC method.
For the first time we have studied scalar mode effects of the
PMF on the CMB [2]. We have confirmed numerically without
approximation that the excess power in the CMB at higher l can be
explained by the existence of a PMF. For the first time a likelihood
analysis utilizing the WMAP, ACBAR and CBI data with a
MCMC method has been applied to constrain the upper limit on
the strength of the PMF to be (Fig. 1)|Bλ|＜7.7nG .

Figure1: Results of the MCMC method constrained by the WMAP, ACBAR,
and CBI data [2]. Excluded and allowed regions at the 1σ(68%)
C.L. and 2σ(95.4%) C.L. are shown in the two parameter plane of|Bλ| vs. nB, where |Bλ| is the primordial magnetic field strength and nB
is the power-law spectral index. Solid and dotted curves are for ∆χ
2＝2.3 and 6.17, respectively. The black-solid, skyblue-dotted, andpink-dashed lines are the upper limit of the produced PMF at the
big-bang nucleosynthesis, the electroweak transiton, and theinflation epochs, respectively [3]. If the PMF is produced at theepochs of big-bang nucleosynthesis, the electroweak transition, or
inflation, respectively, the region of I＋II＋III, II＋III, or III on theright hand side are allowed by these constraints on the PMF for thegalaxy cluster scale at the PLSS and the MCMC method with
WMAP, ACBAR, and CBI data.

The primordial magnetic field (PMF) can strongly affect thecosmic microwave background (CMB) power spectrum and theformation of large scale structure. In this presentation, we calculate
the CMB temperature anisotropies generated by including a
power-law magnetic field at the photon last scattering surface(PLSS). We then deduce an upper limit on the primordial
magnetic field based upon our theoretical analysis of the powerexcess on small angular scales. We have taken into accountseveral important effects such as the modified matter sound speed
in the presence of a magnetic field. An upper limit to the fieldstrength of |Bλ|＝7.7 nG at the present scale of 1 Mpc is deduced.
This is obtained by comparing the calculated theoretical result
including the Sunyaev-Zeldovich (SZ) effect with recent observed
data on the small scale CMB anisotropies from the Wilkinson
Microwave Anisotropy Probe (WMAP), the Cosmic Background
Imager (CBI) and the Arcminute Cosmology Bolometer Array
Receiver (ACBAR). We discuss several possible mechanisms forthe generation and evolution of the PMF in our study.
In order to constrain the PMF, we evaluate likelihood functionof the WMAP TT, CBI, and ACBAR data in a wide range ofparameter of the magnetic field strength |Bλ| at 1 Mpc and thepower-law spectral index n B, along with six cosmologicalparameters, the Hubble parameter, the baryon and cold dark matter

We have also considered three conditions on the generation andevolution of the cosmological PMF: 1) our result (Fig. 1); 2) thelower limit of the PMF from the magnetic field of galaxy clusters;and 3) the constraint on the PMF from gravity waves. Combining
these, we find the following concordance region for the the PMF
parameters;
1nG＜ |Bλ|＜4.7nG , −3.0＜nB＜−2.4 .
The PMF also affects the formation of large scale structure. For
example, magnetic pressure delays the gravitational collapse. It isthus very important to constrain the PMF as precisely as possible.
If we combine our study and future plans to observe the CMB
anisotropies and polarizations for higher multipoles l, e.g. via the
Planck Surveyor, we will be able to constrain the PMF moreaccurately, and explain the evolution and generation of themagnetic field on galaxy cluster scales along with the formation of
the LSS.
References[1] Yamazaki, D. G., Ichiki, K., Kajino, T.: 2005, ApJ, 625, L1.
[2] Yamazaki, D. G., et al.: 2006, ApJ, 646, 719-729.
[3] Caprini, C., Durrer, R.: 2002 Phys. Rev. D, 65, 023517.

47

Supernova Neutrino Nucleosynthesis of Light Elementswith Neutrino Oscillations
YOSHIDA, Takashi

KAJINO, Toshitaka(Astronomical Institute, Tohoku University)(Division of Theoretical Astronomy, NAOJ)

YOKOMAKURA, Hidekazu, KIMURA, Keiichi(Nagoya University)

TAKAMURA, Akira

HARTMANN, Dieter, H.

(Toyota National College of Technology)(Clemson University)

Figure1: The yield ratios of 7Li and 11B related to the mixing angle
sin2 2θ13. Thick and thin lines indicate the yield ratios of 7Li
11
and B, respectively. Solid lines and dotted lines correspondto normal mass hierarchy and inverted mass hierarchy.

We investigate the nucleosynthesis of light elements, 7Li andB, in supernovae taking account of neutrino oscillations [1].
Neutrinos emitted from the neutrino sphere change their flavors
propagating in the surrounding stellar materials. The change of theneutrino energy spectra by the neutrino oscillations will change the711yields of Li and B produced in supernovae.
We calculate detailed explosive nucleosynthesis using thesupernova model of a 16.2 M star [2] corresponding to SN
1987A. Parameter values of neutrino oscillations are adopted inaccordance with the Large Mixing Angle solutions confirmed byrecent neutrino experiments. However, whether mass hierarchy isnormal or inverted has not been clarified and only upper limit of7
θ13 has been determined. We investigate the dependence of the Li
11
and B yields on mass hierarchy andθ13.
The relation between the yield ratios of 7Li and 11B and themixing angle sin2 2θ13 is shown in Fig. 1. When we do not7
11
consider neutrino oscillations, the yields of Li and B are 2.36×−7−7
10 M and 6.26×10 M , respectively. One finds that both7112of the Li and B yields depend on sin 2θ13. In a normal mass2
−3
7
hierarchy and sin 2θ13 ≥ 2×10 , the Li yield increases by afactor of 1.9. In an inverted mass hierarchy, the increase is smaller
even relatively large sin2 2θ13 value. In the case of sin2 2θ13 ≤ 2×
10−5 the yield ratio is about 1.1. On the other hand, the change of11
the B yield ratio is smaller and the yield ratio is less sensitive to
11mass hierarchy. The B yield ratio increase by a factor of 1.4 in a
11

48

Figure2: The relation of the 7Li/11B abundance ratio with the mixing angle2
711
sin 2θ13. The shaded ranges of Li/ B are due to the uncertainties in
the neutrino temperatures and the total neutrino energy evaluated in[3].

normal mass hierarchy and sin 2θ13 ≥ 2×10 .
The studies of Galactic Chemical Evolution (GCE) constrain
11
the production of B in supernovae. We have constrained theneutrino temperatures to reproduce the supernova contribution of11
B during GCE [3]. However, the neutrino temperatures and thetotal neutrino energy still have uncertainties and the affected7
11
uncertainties of the Li and B yields make the effect by theneutrino oscillations ambiguous. Thus, we evaluate the711dependence of the Li/ B abundance ratio on mass hierarchies and2
sin 2θ13 taking into account uncertainties of the neutrino
7
11
temperatures. The relation of the Li/ B ratio to mass hierarchies
2and sin 2θ13 is shown in Fig. 2. When we do not consider neutrino
oscillations, the 7Li/11B is about 0.6. In a normal mass hierarchy
2
−3
7
11
7
11
and sin 2θ13 ≥ 2×10 , the Li/ B is larger than 0.87. The Li/ B
becomes larger by the neutrino oscillations. Therefore, a normal
2
mass hierarchy and relatively large sin 2θ13 might be constrained
from the studies of light element synthesis in supernovae.
2−3

References[1] Yoshida, T., et al.: 2006, Phys. Rev. Lett. 96, 091101.
[2] Shigeyama, T., Nomoto, K.: 1990, ApJ, 360, 242.
[3] Yoshida, T., et al.: 2005, Phys. Rev. Lett. 94, 231101.

II

Publications, Presentations

1. Refereed Publications
Abada-Simon, M., Casares, J., Evans, A., Eyres, S., Fender, R.,
Garrington, S., de Jager, O., Kuno, N., Mart nez-Pais, I. G., de
Martino, D., Matsuo, H., Mouchet, M., Pooley, G., Ramsay,G., Salama, A., and Schulz, B.: 2005, First Detections of theCataclysmic Variable AE Aquarii in the Near to Far Infraredwith ISO and IRAS: Investigating the Various Possible
Thermal and Non-Thermal Contributions, A&A, 433, 10631077.
Abbott, B., et al. including Fujimoto, M.-K., Fukushima, M.,
Hayama, K., Kawamura, S., Kozai, Y., Miyama, S., Ohishi,N., Sato, S., Takahashi, R., Tatsumi, D., Tsunesada, Y.,
Ueda, A., Waseda, K., Yamazaki, T.: 2005, Upper limits
from the LIGO and TAMA detectors on the rate ofgravitational-wave bursts, Phys. Rev. D, 72, 122004.
Abe, L., Murakami, N., Nishikawa, J., Tamura, M.: 2006,
Removal of central obscuration and spider arm effects withbeam-shaping coronagraphy, A&A, 451, 363-373.
Abe, S., Ebizuka, N., Murayama, H., Ohtsuka, K., Sugimoto, S.,
Yamamoto, M., Yano, H., Watanabe, J., Borovicka, J.: 2005,
Video and Photographic Spectroscopy of 1998 and 2001
Leonid Persistent Trains from 300 to 930 nm, Earth, Moon,
and Planets, 95, 265-277.
Adelman-McCarthy, J. K., et al. including Ichikawa, S.: 2006,
The Fourth Data Release of the Sloan Digital Sky Survey,
ApJS, 162, 38-48.
Ajiki, M., Mobasher, B., Taniguchi, Y., Shioya, Y., Nagao, T.,
Murayama, T., Sasaki, S.: 2006, Narrowband Survey of the
GOODS Fields: Search for Lya Emitters at z＝5.7, ApJ, 638,
596.
Ajiki, M., Shioya, Y., Taniguchi, Y., Murayama, T., Nagao, T.,
Sasaki, S., Sumiya, R., Morioka, T., Hatakeyama, Y.,
Yokouchi, A., Takahashi, M., Koizumi, O.: 2006, Strong
Emission-Line Galaxies at Low Redshifts in the Field aroundthe Quasar SDSSp J104433.04-012502.2, PASJ, 58, 113.
Akutsu, T., Ando, M., Kanda, N., Tatsumi, D., Telada, D.,
Hayakawa, H., Yamamoto, K., Miyoki, S., Ohashi, M., Kuroda
K., and the TAMA Collaboration: 2005, Burst wave analysis of
TAMA300 data with the ALF filter, Class. Quantum Grav., 22,
S1303-S1309.
Anderson, S. F., Haggard, D., Homer, L., Joshi, N. R., Margon, B.,
Silvestri, N. M., Szkody, P., Wolfe, M. A., Agol, E., Becker, A.
C., Henden, A., Hall, P. B., Knapp, G. R., Richmond, M. W.,
Schneider, D. P., Stinson, G., Barentine, J. C., Brewington, H.
J., Brinkmann, J., Harvanek, M., Kleinman, S. J., Krzesinski,
J., Long, D., Neilsen, E. H., Jr., Nitta, A., and Snedden, S. A.:
2005, Ultracompact AM Canum Venaticorum Binaries fromthe Sloan Digital Sky Survey: Three Candidates Plus the First
Confirmed Eclipsing System, AJ, 130, 2230-2236.
Ando, M., Akutsu, T., Akutsu, T., Arai, K., Aso, Y., Fukushima,M., Hayama, K., Kanda, N., Kondo, K., Mio, N., Miyoki, S.,
Moriwaki, S., Nagano, S., Sato, S., Shibata, M., Tagoshi, H.,
Takahashi, H., Takahashi, R., Tatsumi, D., Tsunesada, Y.,
Yamazaki T., and the TAMA Collaboration: 2005, Upper
limits on gravitational-wave bursts radiated from stellar-corecollapses in our galaxy, Class. Quantum Grav., 22, S1283-

S1291.
Ando, M., et al. including Arai, K., Hayama, K., Kawamura, S.,
Nagano, S., Sato, S., Takahashi, R., Tatsumi, D.,
Tsunesada, Y., Fujimoto, M.-K., Fukushima, M., Kozai, Y.,
Miyama, S., Ohishi, N., Ueda, A., Waseda, K., Yamazaki,
T.: 2005, Observation results by the TAMA300 detector on
gravitational wave bursts from stellar-core collapses, Phys.
Rev. D, 71, 082002.
Aoki, W., Frebel, A., Christlieb, N., Norris, J., Beers, T. C.,
Minezaki, T., Barklem, P., Honda, S., Takada-Hidai, M.,
Asplund, M., Ryan, S., Tsangarides, S., Eriksson, K.,
Steinhauer, A., Deliyannis, C., Nomoto, K., Fujimoto, M.,
Ando, H., Yoshii, Y., and Kajino, T.: 2006, HE 1327-2326, anUnevolved Star with [Fe/H] < −5.0. I. A Comprehensive
Abundance Analysis, ApJ, 639, 897-917.
Aoki, W., Honda, S., Beers, T. C., Kajino, T., Ando, H., Norris,
J. E., Ryan, S. G., Izumiura, H., Sadakane, K., Takada-Hidai,
M.: 2005, Spectroscopic Studies of Very Metal-poor Stars with
the Subaru High Dispersion Spectrograph. III. Light NeutronCapture Elements, ApJ, 632, 611-637.
Aoki, W.: 2005, Elemental and isotopic abundances in metaldeficient stars, Nucl. Phys. A, 758, 209-216.
Ariyoshi, S., Matsuo, H., Otani, C., Sato, H., Shimizu, H. M.,
Kawase, K., and Noguchi, T.: 2005, Characterization of an
STJ-Based Direct Detector of Submillimter Waves, IEEE
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Asai, A., Nakajima, H., Shimojo, M., White, S. M., Hudson, H.
S., and Lin, R. P.: 2006, Preflare Nonthermal Emission
Observed in Microwaves and Hard X-Rays, PASJ, 58, L1-L5.
Asano, K.: 2005, Cooling of Accelerated Nucleons and Neutrino
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Asano, K., and Nagataki, S.: 2006, Very High Energy Neutrinos
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Asano, K., and Takahara, F.: 2005, Coherent Curvature Radiation
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630, L53.
Asano, K., Yamazaki, R., and Sugiyama, N.: 2006, Possibility of
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Atteia, J.-L., Kawai, N., Vanderspek, R., Pizzichini, G., Ricker, G.
R., Barraud, C., Boer, M., Braga, J., Butler, N., Cline, T., Crew,
G. B., Dezalay, J.-P., Donaghy, T. Q., Doty, J., Fenimore, E.
E., Galassi, M., Graziani, C., Hurley, K., Jernigan, J. G., Lamb,
D. Q., Levine, A., Manchanda, R., Martel, F., Matsuoka, M.,
Morgan, E., Nakagawa, Y., Olive, J.-F., Prigozhin, G.,
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Yamauchi, M., Yoshida, A.: 2005, HETE-2 Observation of
Two Gamma-Ray Bursts at z > 3, ApJ, 626, 292-297.
Bailin, J., Kawata, D., Gibson, B. K., Steinmetz, M., Navarro, J.
F., Brook, C. B., Gill, S. P. D., Ibata, R. A., Knebe, A., Lewis,
G. F., Okamoto, T.: 2005, Internal Alignment of the Halos of
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ApJ, 627, L17.
Beuther, H., Sridharan, T. K., Saito, M.: 2005, Caught in the Act:The Onset of Massive Star Formation, ApJ, 634, L185.
Beyersdorf, P., Kawamura, S., Somiya, K., Kawazoe, F., and49

Agüeros, M.: 2005, Power-recycled resonant sideband
extraction interferometer with polarization detection, Appl.
Opt., 44, 3413-3424.
Brannigan, E., Takami, M., et al.: 2006, On the detection ofartefacts in spectro-astrometrty, MNRAS, 367, 315-322.
Broadhurst, T., Takada, M., Umetsu, K., Kong, X., Arimoto, N.,
Chiba, M., Futamase, T.: 2005, The Surprisingly Steep Mass
Profile of A1689, from a Lensing Analysis of Subaru Images,
ApJ, 619, L143-L146.
Byun, D.-Y., Koo, B.-C., Tatematsu, K., and Sunada, K.: 2006,
Interaction Between the Supernova Remnant HB 21 andMolecular Clouds, ApJ, 637, 283-295.
Cameron, P. B., Chandra, P., Ray, A., Kulkarni, S. R., Frail, D. A.,
Wieringa, M. H., Nakar, E., Phinney, E. S., Miyazaki, A.,
Tsuboi, M., Okumura, S. K., Kawai, N., Menten, K. M., andBertoldi, F.: 2005, Detection of a Radio Counterpart to the 27
December 2004 Giant Flare from SGR 1806-20, Nature, 434,1112-1115.
Cellino, A., Yoshida, F., Anderlucci, E., Bendjoya, P., Martino,
M. D., Ishiguro, M., Nakamura, A., Saito, J.: 2005, A
polarimetric study of asteroids 25143 Itokawa, Icarus, 179,
297-303.
Chiba, M., Minezaki, T., Kashikawa, N., Kataza, H., Inoue, K. T.:
2005, Subaru Mid-Infrared Imaging of the Quadruple Lenses
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Lensing, ApJ, 627, 53-61.
Chiba, T., Takahashi, R., Sugiyama, N.: 2005, Classifying thefuture of universes with dark energy, Class. Quantum Grav.,
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Chiu, K., Zheng, W., Schneider, D. P., Glazebrook, K., Iye, M.,
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10: Cloning and Discovery, AJ, 130, 13-22.
Civiis, S., Hosaki, Y., Kagi, E., Izumiura, H., Yanagisawa, K.,
Sedivcova, T., and Kawaguchi, K.: 2005, Search for C−
2 in
Diffuse Clouds, PASJ, 57, 605-609.
Culhane, J. L., Harra, L. K., Doschek, G. A., Mariska, J. T.,
Watanabe, T., and Hara, H.: 2006, The Solar-B EUV
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Melnikov, V. F., Gorbikov, S. P., Reznikova, V. E., andShibasaki, K.: 2005, Dynamics of Electron Spatial
Distribution in Microwave Flaring Loops, Proc. of the 11th
European Solar Physics meeting “The dynamic sun:challenges for theory and observations”, Eds. D. Danesy, S.
Poedts, A. De Groof, and J. Andries, ESA SP-600, 132.1.
Migenes, V., Cruz-Vazquez, L., Slysh, V. I., Val’Tts, I. E.,
Horiuchi, S., Inoue, M.: 2005, The VLBA Survey of OH
Masers towards SFR: Preliminary Results, Future Directions inHigh Resolution Astronomy: The 10th Anniversary of the
VLBA, ASP Conf. Proc., 340, Eds. J. Romney and M. Reid,
361.
Minowa, Y., Kobayashi, N., Tsujimoto, T., Takato, N., Iye, M.:
2005, Adaptive optics imaging search for damped Lyalphaabsorbers toward APM 08279＋5255, IAU Colloquium 199,
Probing Galaxies through Quasar Absorption Lines, Eds. P. R.
Williams, C.-G. Shu, B. Menard, 448-450.
Minowa, Y., Kobayashi, N., Yoshii, Y., Totani, T., Takami, H.,
Takato, N., Hayano, Y., Iye, M.: 2005, Subaru Deep Field
with Adaptive Optics, Science with Adaptive Optics, Eds. W.
Brandner and M. E. Kasper, 365.

Misawa, T., Tytler, D., Iye, M., Paschos, P., Norman, M.,
Kirkman, D., O’Meara, J., Suzuki, N., and Kashikawa, N.:
2006, H I gas in higher density regions of the IGM, pgqa conf.,
454.
Miura, N., Kodama, N., Ohkama, H., Odagiri, H., Baba, N., Kita,
H., Kitai, R., Ueno, S., Ichimoto, K., and Sakurai, T.: 2005,
Image Acquisition and Processing Using a PC Cluster toward
Real-Time Solar Image Improvement, Proc. of the 20-th
Congress of the Int. Commission for Optics, SPIE 6027.
Miyamoto, H., et al. including Sasaki, S.: 2006, Regolith on a
Tiny Asterid: Granular Materials Partly Cover the Surface of
Itokawa, Proc. 37th Lunar and Planetary Science Conf., #1686.
Miyoshi, M., Imai, H., Nakashima, J., Deguchi, S., and Shen, Z.Q.: 2005, VLBA Observations of an Intraday Flare of
Sagittarius A*, Proc. of the “Future Directions in High
Resolution Astronomy: A Celebration of the 10th Anniversaryof the VLBA”, ASP Conf. Ser., 340, Eds. J. D. Romney, and M.
J. Reid, 258-262.
Mori, Y., Sekiguchi, T., Sugita, S., Matsunaga, N., Fukushi, H.,
Kaneyasu, N., Kawadu, T., Kandori, R., Nakajima, Y.,
Tamura, M.: 2006, Near-IR Monitoring Observation of
Comet 9P/Tempel 1, 37th Annual Lunar and Planetary Science
Conf., 2458.
Nagasawa, M., Lin, D. N. C., Thommes, E.: 2005, The Final
Coagulation of the Inner Solar System: Dynamical Shakeup
Model, Proc. of the 38th ISAS Lunar and Planetary Symp.,
132-134.
Nagashima, M., Yahagi, H., Enoki, M., Yoshii, Y., Gouda, N.:
2006, Numerical Galaxy Catalog: a semi-analytic galaxy
formation model with high-resolution N-body simulations,
Proc. of The 9th Asian-Pacific Regional IAU Meeting 2005,
Eds. W. Sutantyo, et al., 245-246.
Nagata, H., Kobayashi, J., Matsuo, H., Akiba, M., Fujiwara, M.:
2005, Cryogenic GaAs Readout Circuits for Low Temperature
Detectors, XXVIIIth General Assembly of Int. Union of Radio
Science (URSI), JB-P.9.
Nagata, H., Kobayashi, J., Matsuo, H., Akiba, M., Fujiwara, M.:
2005, Cryogenic Readout Integrated Circuits for submillimeter
Camera, The Joint 30th Int. Conf. on Infrared and Millimeter
Waves and 13th Int. Conf. on Terahertz Electronics
Williamsburg, Eds. G. R. Neil, B. Danly, 630.
Nakajima, T., and Morikawa, M.: 2006, Fully Degenerate
Fermionic Dark Matter in the Cluster Center and Black Hole, J.
of Phys. Conf. Ser., 31, 179.
Nakajima, Y.: 2005, Deep Infrared Surveys of Star
Formingregions in the MWG and LMC, J. Korean Astron.
Soc., 38.
Nakamura, K.: 2006, Second Order Gauge Invariant Perturbation
Theory and Cosmological Perturbations, Proc. of 15th
workshop on general relativity and gravitation in Japan, Eds.
T. Shiromizu, et al.
Narita, N., Suto, Y., Winn, J. N., Turner, E. L., Aoki, W., Leigh,C. J., Sato, B., Tamura, M., Yamada, T.: 2006, Subaru HDS
transmission spectroscopy of the transiting extrasolar planet
HD209458b, Revista Mexicana de Astronomía y Astrofísica
(Serie de Conferencias), 24, Eds. L. Arnold, F. Bouchy, and C.
Moutou, 254-256 .
Nishikawa, K.-I., Mizuno, Y., Fuerst, S., Wu, K., Hardee, P.,
Richardson, G., Koide, S., Shibata, K., Kudoh, T., Fishman, G.
J.: 2005, 3-D GRMHD Simulations of Disk-Jet Coupling andEmission, Astrophysical Sources of High energy Particles and63

Radiation, AIP Conf. Proc., 801, 184-187.
Nishikori, H., Machida, M., Matsumoto, R.: 2005, Global Threedimensional MHD Simulations of Galactic Gaseous Disks,
Magnetic Fields in the Universe: From Laboratory and Stars
to Primordial Structures, AIP Conf. Proc., 784, 786.
Noda, H., Hanada, H., Kawano, N., and Iwata, T.: 2005, The
SELENE mission and Japanese lunar exploration scenario, J.
Korean Astr. Soc., 38, 311-314.
Noda, H., Asari, K., Namiki, N., Iwata, T., Kono Y., Hanada,
H., Kawano, N., Yamamoto, Z.: 2005, Ground-based
verification of four-way Doppler measurement for the
SELENE mission, A Window on the future of geodesy, IAG
symp., 128, Ed. F. Sanso, 152-156.
Nogami, D., Kawamura, T., Kuriyama, J., Sugiyasu, K., Kubota,
K., Yanagisawa, K., Kouzuma S., Yamaoka, H., Kawai, N.:
2005, GRB051117B: optical observation., GCN Circular,
4396.
Nomoto, K., Tominaga, N., Umeda, H., Kobayashi, C.: 2005,
Yields of Population III Supernovae and the Abundance
Patterns of Extremely Metal-Poor Stars, IAU Symp., 228: From
Lithium to Uranium: Elemental Tracers of Early Cosmic
Evolution, Eds. V. Hill, P. Francois, and F. Primas, 287-296.
Noumaru, J.: 2005, Collaboration Among East Asian
Astronomers at Subaru Telescope, J. Korean Astron. Soc., 38,
101.
Ohnishi, K., Horaguchi, T., Agata, H., and Paofits WG: 2005,
Determination of 1 AU by the Parallax measurement of Planet
Transit between the Earth and Satellites, Proc. of The 9th
Asian-Pacific Regional IAU Meeting 2005 (APRIM 2005),
Eds. W. Sutantyo, et al., 348-349.
Ohta, I. S., Hattori, M., Takahashi, J., Matsuo, H.: 2005, The first
astronomical mm and submm observation with Multi-Fourier
Transform interferometer, The Joint 30th Int. Conf. on Infrared
and Millimeter Waves and 13th Int. Conf. on Terahertz
Electronics Williamsburg, Eds. G. R. Neil, B. Danly, 359-360.
Ootsubo, T., Sugita, S., Kadono, T., Honda, M., Miyata, T., Sako,
S., Sakon, I., Fujiwara, H., Fujiyoshi, T., Yamashita, T.,
Takato, N., Fuse, T., Subaru/Comics Deep Impact Team:2005, Mid-Infrared Observation of the Collision Between Deep
Impact Projectile and Comet 9P/Tempel 1 with
SUBARU/COMICS, Dust in Planetary Systems, 124.
Ota, K., Kashikawa, N., Nakajima, T., Iye, M.: 2005, z ~ 6 iDropout Galaxies in the Subaru XMM/Newton Deep Field, J.
Korean Astro. Soc., 38, 179.
Otsuka, M., Tamura, S., and Tajitsu, A.: 2005, Highly Resolved
Spectroscopic Study of the PNe with HIDES - A Case Study ofNGC 6572, AIP Conf. Proc. Subseries: AA, 804, 98-98.
Peck, A., Iono, D., Petitpas, G., Pope, A., Borys, C., Dunlop, J.,
Krips, M., Wilner, D.: 2006, Astrometric Imaging of HighRedshift Galaxies at 345 GHz, American Astronomical Society
Meeting 207.
Petitpas, G., Iono, D., Peck, A., Wilson, C., Matsushita, S.,
Sakamoto, K.: 2005, Warm Gas and Temperature Gradients in
the Giant Molecular Associations of the Antennae, Protostars
and Planets V, 8317.
Petitpas, G., Peck, A., Iono, D., Wilson, C., Matsushita, S., Krips,
M., Ho, P.: 2006, SMA Observations of Warm Molecular Gas
in Nearby Galaxies, American Astronomical Society Meeting
207.
Petitpas, G., Peck, A., Iono, D., Wilson, C., Matsushita, S., Krips,
M., Ho, P.: 2005, Warm, Optically thin Molecular Gas in
64

Nearby Galaxies: NGC 2903 & NGC 3627, American
Astronomical Society Meeting 206.
Pyo, T.-S., Hayashi, M., Kobayashi, N., Tokunaga, A. T.,
Terada, H., Goto, M., Takami, H., Takato, N., Gässler, W.,
Oya, S., Hayano, Y., Kamata, Y., Minowa, Y., Usuda, T.,
Iye, M., Yamashita, T.: 2005, The Structure of the Young
Stellar Outflows Revealed by High Angular Resolution [Fe II]
λ 1.644μm Spectroscopy, Science with Adaptive Optics, Eds.
W. Brandner, and M. E. Kasper, 242.
Reznikova, V. E., Nakariakov, V. M., Melnikov, V. F., andShibasaki, K.: 2005, Diagnostics of MHD-Oscillation Modesof a Flaring Loop Using Microwave Observations with HighSpatial Resolution, Proc. of the 11th European Solar Physics
meeting The dynamic sun: challenges for theory andobservations, ESA SP-600, Eds. D. Danesy, S. Poedts, A. De
Groof, and J. Andries, 140.1.
Rodriguez, J. A. P., Tanaka, K. L., and Sasaki, S.: 2006, Sources,
sinks and migrations patterns of dark veneers in the northern
polar deposits of Mars, Proc. 37th Lunar and Planetary
Science Conf., #1437.
Saigo, K., Tomisaka, K.: 2005, The Evolution of the First Core in
Rotating Molecular Core, Protostars and Planets V, Ed. B.
Reipurth, 8624.
Saito, M. M., Tanikawa, K.: 2005, Survey of one dimensional
three-body problem through the symbol sequence, Order andChaos in Stellar and Planetary Systems.
Saito, N., Akagawa, K., Hayano, Y., Takami, H., Saito, Y., Iye,
M., and Wada, S.: 2006, 1W 589nm Coherent Light-Source
Achieved by Quasi-Intracavity Sum-Frequency Generation,
Advanced Solid State Photonics, 457-461.
Sakamoto, S.: 2005, Development of paper models of telescopes
for education and public outreach, 9th Asian-Pacific Regional
IAU Meeting (APRIM 2005).
Sasaki, S., et al.: 2006, Space Weathering of Rock Surface
Without Regolith: Laboratory Simulation of Spectral Change,
Proc. 37th Lunar and Planetary Science Conf., #1705.
Sasaki, S., et al.: 2006, Observations of 25143 Itokawa by theAsteroid Multiband Imaging Camera (AMICA) Of
HAYABUSA: Morphology of Brighter and Darker Area, Proc.
37th Lunar and Planetary Science Conf., #1671.
Sato, B.: 2005, Okayama Planet Search Program, J. Korean
Astron. Soc., 38, 315-318.
Sawada, T., Tatematsu, K., Kandori, R., Nakanishi, K.,
Morita, K.-I., and Sunada, K.: 2005, Development of a
Virtual Observatory Prototype in ALMA-Japan, Proc. of the“Astronomical data analysis software and system XIV”, ASP
Conf. Ser., 347, Eds. P. Shopbell, M. Britton, and R. Ebert,
252-256.
Sawada-Satoh, S., Kameno, S., Shibata, K. M., Inoue, M.: 2005,
Positional Coincidence between Water Masers and a Plasma
Torus in NGC 1052, Future Directions in High Resolution
Astronomy: The 10th Anniversary of the VLBA, ASP Conf.
Proc., 340., Eds. J. Romney and M. Reid, 119.
Shan, W., Asayama, S., Kamikura, M., Noguchi, T., Shi, S.,
and Sekimoto, Y.: 2005, Development of a 385-500GHz SIS
Mixer for ALMA Band 8, Proc. of 16th Int. Symp. on Space
Terahertz Technology, Eds. M. Ingvarson, J. Stake, and H.
Harald Merkel, 175-180.
Shimojo, M.: 2005, The Joint Observations of Prominence
Eruptions using Solar-B, STEREO and NoRH, 35th COSPAR
Scientific Assembly, 1927.

Shirasaki, Y., Ohishi, M., Mizumoto, Y., Tanaka, M., Honda,
S., Oe, M., Yasuda, N., Masunaga, Y.: 2005, Structured Query
Language for Virtual Observatory, Astronomical Data Analysis
Software and Systems XIV, ASP Conf. Ser., 347, Eds. P.
Shopbell, M. Britton, and R. Ebert, 262.
Shitov, S., Noguchi, T., Matsunaga, T., Tamura, T., Uvarov,
A., Cohn, I., and Hasegawa, T.: 2005, A SIS Mixer for
ALMA Band 10: Development Concept, Proc. of 16th Int.
Symp. on Space Terahertz Technology, Eds. M. Ingvarson, J.
Stake, and H. Harald Merkel, 165-168.
Skopal, A., Errico, L., Vittone, A. A., Tamura, S., Otsuka, M.,
Wolf, M., Elkin, V. G.: 2005, A multiple mass-ejection by the
symbiotic prototype Z And during its 2000-03 outburst, AIP
Conf. Proc. Subseries: AA, 797, 557-560.
Sôma, M., Tanikawa, K.: 2005, Variation of Delta T between
AD 800 and 1200 Derived from Ancient Solar Eclipse
Records, Journées 2004, Fundamental Astronomy, Eds. N.
Capitaine, 265-266.
Sôma, M., Yamaoka, H., Nakano, S.: 2005, Nova Scuti 2005, IAU
Circular 8607, Ed. D. W. E. Green.
Takato, N., Terada, H., Bus, S., Pyo, T.-S., Kobayashi, N.: 2005,
Detection of a Deep 3-μm Absorption Feature in the Spectrumof Jovian Satellites Amalthea and Thebe, Protostars andPlanets V, 8270.
Takeda T., and Ohtsuki, K.: 2006, Angular momentum transfer
in the collision between rubble pile objects, Proc.of the 9th
Asian-Pacific Regional Meeting, Eds. W. Sutantyo, P. W.
Premadi, P. Mahasena, T. Hidayat, and S. Mineshinge, 63-64.
Tamura, M.: 2005, Subaru Explorations of EXO-Solar Planets
and Disks, J. Korean Astron. Soc.
Tamura, M., Fukagawa, M.: 2005, Circumstellar Disks in PMS
and T Tauri Stars---Herbig Ae/Be Stars, Vega-like Stars, andSubmillimeter Polarizations, Astronomical Polarimetry:
Current Status and Future Directions, Eds. A. Adamson, C.
Aspin, C. J. Davis.
Tanaka, M., Wada, K., Machida, M., Matsumoto, R., Miyaji, S.:
2005, Magnetohydrodynamic Simulations of the Wiggle
Instability in Spiral Galaxies, Magnetic Fields in the Universe:
From Laboratory and Stars to Primordial Structures, AIP
Conf. Proc., 784, 792.
Tanaka, M., Shirasaki, Y., Honda, S., Mizumoto, Y., Ohishi,M., Yasuda, N., Masunaga, Y., Ishihara, Y., Abe, K.,
Tsutsumi, J., Nakamoto, H., Kobayashi, Y., Yoshida, T.,
Morita, Y.: 2005, Japanese Virtual Observatory (JVO)
Prototype 2, Astronomical Data Analysis Software and Systems
XIV ASP Conf. Ser., 347, Eds. P. Shopbell, M. Britton, and R.
Ebert., 267.
Terada, H., Kobayashi, N., Tokunaga, A. T., Takato, N.,
Takami, H., Pyo, T.-S., Hayashi, M.: 2005, Near-Infrared AO
Spectroscopy of Edge-On Protoplanetary Disks with Subaru
IRCS, Science with Adaptive Optics, Eds. W. Brandner, and M.
E. Kasper, 211.
Tomisaka, K., Machida, M. N., Matsumoto, T., Hanawa, T.:2005, Role of Magnetic Field in Star Formation Process, The
Magnetized Plasma in Galaxy Evolution, Eds. K. T. Chyzy, R.J. Dettmar, K. Otmianowska-Mazur, and M. Soida.
Tsuboi, M., Ohno, T., Tanabe, Y., Kasuga, T., Kuno, N.,
Sakamoto, A., Miyazaki, A., and Matsuo, H.: 2005,
Observation of the Sunyaev-Zel’dovich Effect toward
CL0016+16 at 43 GHz, Proc. of the IAU Symp., 201, “NewCosmological Data and the Values of the Fundamental

Parameters”, Eds. A. Lasenby and A. Wilkinson, 521-522.
Tsujimoto, T., Yamada, Y., Gouda, N.: Statistical calibrations oftrigonometric parallaxes, IAU Colloquium 196, Transits ofVenus: New Views of the Solar System and Galaxy, Ed. D. W.
Kurtz, 411-419.
Ueda, S., Yamada, Y., Kuwabara, T., Gouda, N., Tsujimoto, T.,
Kobayashi, Y., Nakajima, T., Matsuhara, H., Yano, T.,
Suganuma, M., and The JASMINE Working Group: 2005,
JASMINE simulator, IAU Colloquium 196, Transits of Venus:
New Views of the Solar System and Galaxy, Ed. D. W. Kurtz,
483-490.
Ujino, H., Vinet, L., Yoshida, H.: 2005, Another Derivation of theSuper-Integrable Discretization of the Calogero Model for thetwo-body case, Group Theoretical Methods in Physics 185,
Eds. G. S. Pogosyan, L. E. Vicent, K. B. Wolf, 533-538.
Usuda, T., Goto. M.: 2005, Molecular Hydrogen Absorption Line
Detected in Dense Molecular Clouds, High Resolution Infrared
Spectroscopy in Astronomy, Eds. H. U. Käufl, R.
Siebenmorgen, and A. F. M. Moorwood, 248-251.
Wiedner, M. C., Volgenau, N. H., Iono, D., Saito, M., Sakamoto,K., Wang, J., Wilner, D., Wilson, C. D.: 2005, Sequential
starburst in Arp 220?, Astron. Nachr., 326, 534.
Yamada, Y., Gouda, N., Tsujimoto, T., Kobayashi, Y.,
Nakajima, T., Matsuhara, H., Yano, T., Ueda, S., Suganuma,
M., and The JASMINE Working Group: 2005, Overall designof JASMINE, IAU Colloquium 196, Transits of Venus: New
Views of the Solar System and Galaxy, Ed. D. W. Kurtz, 476482.
Yamauchi, A., Nakai, N., Sato, N., and Diamond, P.: 2005,
Water-Vapor Maser Emission from the Seyfert 2/LINER NGC
3079, Proc. of the Future Directions in High Resolution
Astronomy: A Celebration of the 10th Anniversary of the
VLBA, ASP Conf. Ser., 340, Eds. J. D. Romney, and M. J. Reid,
241-243.
Yanagisawa, K., Sakamoto, T., Kawai, N.: 2005, GRB 051227:
optical observation, GCN Circular, 4418.
Yanagisawa, K., Toda, H., Kawai, N.: 2006, GRB 060108:
Mitsume optical observations, GCN Circular, 4451.
Yanagisawa, K., Toda, H., Kawai, N.: 2006, GRB 060110:
Mitsume optical observations, GCN Circular, 4478.
Yanagisawa, K., Toda, H., Kawai, N.: 2006, GRB 060111B:
MITSuME detection of optical afterglow, GCN Circular,
4496.
Yanagisawa, K., Toda, H., Kawai, N.: 2006, GRB 060115:
MITSuME optical afterglow candidate, GCN Circular, 4510.
Yanagisawa, K., Toda, H., Kawai, N.: 2006, GRB 060115: OT
finding chart, GCN Circular, 4513.
Yanagisawa, K., Toda, H., Kawai, N.: 2006, GRB 060115: OT
photometry with MITSuME, GCN Circular, 4517.
Yanagisawa, K., Yatsu, Y., Kawai, N.: 2005, GRB 060105:
Mitsume optical observations, GCN Circular, 4436.
Yanagisawa, K., Toda, H., Kawai, N.: 2005, GRB 050525:
MITSuME optical observation in VRI, GCN Circular, 3489.
Yanagisawa, K., Toda, H., Kawai, N.: 2005, GRB 050416:
Mitsume optical observation, GCN Circular, 3287.
Yano, H., et al. including Sasaki, S.: 2006, HAYABUSA’s Touch
Down Sites at the Smooth Terrain on Asteroid 25143 Itokawa:
Initial Invesitigation, Proc. 37th Lunar and Planetary Science
Conf., #2643.
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T., Nakajima,T., Hanada, H., Yamada, Y., Araki, H., Tazawa, S., Asari,
65

K., Tsuruta, S., Kawano, N., Takato, N.: 2005, The opticalsystem for JASMINE and the CCD centroiding experiment,
IAU Colloquium 196, Transits of Venus: New Views of the
Solar System and Galaxy, Ed. D. W. Kurtz, 476-482.
Yoshida, M.: 2005, Current Status of the Instruments,
Instrumentation and Open Use of Okayama AstrophysicalObservatory, J. Korean Astron. Soc., 38, 117-120.
Ohtsuka, K., Sekiguchi, T., Kinoshita, D., Watanabe, J.: 2005,
2005 UD and the Daytime Sextantids, Central Bureau
Electronic Telegrams, 283, 1.
Kasuga, T., Watanabe, J., Sato, M.: 2005, Scientific Mission to3200 Phaethon-Nature of the extinct comet and artificial
meteor showers, Proc. 38th ISAS Lunar and Planetary Symp.,
146-150.
5. Publications in English
Aoki, W., Beers, T., Christlieb, N., Frebel, A., Ando, H.,
Asplund, M., Barklem, P., Eriksson, K., Fechner, C., Fujimoto,M., Honda, S., Kajino, T., Nomoto, K., Norris, J., Ryan, S.,
Takada-Hidai, M., Tsangarides, S., and Yoshii, Y.: 2005,
Chemical Abundance Patterns of Extremely Metal-Poor Stars
with [Fe/H] ＜−3.5, Cambridge University Press, U.K..
Ciba, S., Kawano, T., Koura, H., Nakagawa, T., Tachibana, T.,
Kajino, T., Oryu, S., Hayakawa, T., Seki, A., Maruyama, T.,
Tanigawa, T., Watanabe, Y., and Ohsaki, T.: 2005, Nuclear
Data for Astrophysical Nucleosynthesis: A Japanese＋LANL
Activity, AIP, U.S.A.
Frebel, A., Aoki, W., Christlieb, N., Ando, H., Asplund, M.,
Barklem, P., Beers, T., Eriksson, K., Fechner, C., Fujimoto, M.,
Honda, S., Kajino, T., Minezaki, T., Nomoto, K., Norris, J.,
Ryan, S., Takada-Hidai, M., Tsangarides, S., and Yoshii, Y.:
2005, The new record holder for the most iron-poor star: HE
1327 - 2326, a dwarf or subgiant with [Fe/H]＝−5.4,
Cambridge University Press, U.K.
Hayakawa, T., Shimizu, T., Arima, T., Kajino, T., Chiba, S.,
186
Shinohara, N., and Utsunomiya, H.: 2005, Re isomer
187
187
contribution to Re- Os Cosmochronometer, World
Scientific, Singapore.
Honda, S., Aoki, W., Ishimaru, Y., Wanajo, S., Ryan, S. G.,
Kajino, T., Ando, H., Beers, T. C.: 2005, Subaru/HDS studiesof r-process elements in metal-poor stars from near UVspectra, Cambridge University Press, U.K.
Ishizuka, C., Ohnishi, A., Sumiyoshi, K., and Yamada, S.: 2005,
Supernova explosion energy with relativistic EOS including
hyperon, World Scientific, Singapore.
Otsuki, K., Honda, S., Aoki, W., Kajino, T., Truran, J. W.,
Dwarkadas, V., and Medina, A.: 2005, r-process elements inglobular clusters, Cambridge University Press, U.K.
Roepke, G., Grigo, A., Sumiyoshi, K., and Shen, H.: 2005,
Superdense QCD Matter and Compact Stars, Clusters andcondensates in the nuclear matter equation of state, NATO
Science Series, Netherland.
Sakurai, T., Shibata, K., Nakajima, H., Kurokawa, H.: 2005, The
Source of Energy and Disturbances Affecting the Earth inAdvances in Solar-Terrestrial Physics, pp.1-100, Terrapub,
Tokyo.
Sasaqui, T., Otsuki, K., Kajino, T., Mathews, G. J., andNakamura, T.: 2005, Theoretical study of supernova r-process:Dependence on the light neutron-rich nuclear reactions, World
Scientific, Singapore.
66

Terasawa, M., Langanke, K.-H., Kajino, T., and Mathews, G. J.:
2005, Neutrino effects before during and after the freezeout of
the r-process, World Scientific, Singapore.
Yoshida, T., and Kajino, T.: 2005, Light element synthesis
through the n-process in supernova explosions, World
Scientific, Singapore.
Yoshida, T., Kajino, T., and Hartmann, D. H.: 2005, Lightelement synthesis constraining the supernova neutrino
spectrum, Cambridge University Press, U.K.
6. Conference Presentations
Abe, L., Tamura, M., Nakagawa, T., Enya, K., Tanaka, S., Fujita,
K., Nishikawa, J., Murakami, N., Kataza, H., and The SPICA
Working Group: 2005, Current status of the coronagraphic
mode for the 3.5m SPICA space telescope, Direct Imaging of
Exoplanets: Science & Techniques, Proceedings IAU
Colloquium 200, (Villefranche-sur-Mer, France, Oct. 3-7).
Agata, H.: 2005, The Future of Astronomical Education &Popularization in Japan, The 9th Asian-Pacific Regional IAU
Meeting 2005 (APRIM 2005), (Bali, Indonesia, July 29).
Agata, H.: 2005, Public Outreach in Astronomy, Global HOU
conference in Beijing, (Beijing, China, Aug. 3).
Akutsu, K., Arai, K., Sato, S., and TAMA Collaboration: 2005,
Contributions of oscillator noises to the sensitivity of
TAMA300, 6th Edoardo Amaldi Conference on Gravitational
Waves, (Okinawa, Japan, June 20-24).
Ando, M., Akutsu, T., Akutsu, T., Arai, K., Aso, Y., Fukushima,M., Hayama, K., Kanda, N., Kondo, K., Mio, N., Miyoki, S.,
Moriwaki, S., Nagano, S., Sato, S., Shibata, M., Tagoshi, H.,
Takahashi, H., Takahashi, R., Tatsumi, D., Tsunesada, Y.,
Yamazaki, T., and the TAMA Collaboration: 2005, Upper
limits on gravitational wave bursts radiated from stellar-corecollapses in our Galaxy, 6th Edoardo Amaldi Conference on
Gravitational Waves, (Okinawa, Japan, June 20-24).
Aoki, W., et al.: 2005, An abundance study of the most iron-poorstar HE1327-2326 with Subaru/HDS, Origin of Matter and
Evolution of Galaxies: New Horizon of Nuclear Astrophysics
and Cosmology, (Tokyo, Japan, Nov. 8-11).
Aoki, W., et al.: 2005, Chemical Abundance Patterns ofExtremely Metal-Poor Stars with [Fe/H]<−3.5, From Lithium
˜ Cosmic Evolution,
to Uranium: Elemental Tracers of Early
IAU Symposium Proceedings of the international
Astronomical Union 228, (Paris, France, May 23-27).
Aoki, W., et al.: 2005, Chemical composition of carbon-enhanced
stars with [Fe/H]<−3, ESO/MPE workshop “Carbon-rich
Ultra-Metal-Poor Stars in the Galactic Halo”, (Ringberg Castle,
Germany, Nov. 30-Dec. 2).
Arai, K., and the TAMA collaboration: 2005, Current efforts on
the TAMA300 detector, 6th Edoardo Amaldi Conference on
Gravitational Waves, (Okinawa, Japan, June 20-24).
Arai, K., on behalf of TAMA collaboration and LCGT
collaboration: 2005, Status of gravitational wave detection in
Japan, HEP2005 International Europhysics Conference on
High Energy Physics, (Lisbon, Portugal, July 21-27).
Arai, T.: 2006, ASTE observation of the massive star formation
region Sgr B2: A GIANT IMPACT, Perspective of
Submillimeter Astronomy with Atacama Submillimeter
Telescope Experiment (ASTE), (Mitaka, Japan, Mar. 16-17).
Araki, H., Tazawa, S., Tsubokawa, T., Noda, H., Asari, K.,
Kawano, N., and Kunimori, H.: 2005, Observation of LunarTopography by Laser altimeter (LALT) on board SELENE,
Asia Oceania Geoscience Society 2005, (Singapore, Jully 2024).
Ariyoshi, S., Otani, C., Dobroiu, A., Matsuo, H., Sato, H., Taino,T., Kawase, K., Noguchi, T., Shimizu, H. M.: 2005, Terahertz
Imaging with an STJ-based Direct Detector, 7th European
conference on Applied Superconductivity, (Vienna, Austria,
Sep. 11-15).
Asai, A., Nakajima, H., Shimojo, M., and White, S. M.: 2005,
Preflare Features in Radios and in Hard X-Rays, Asia Oceania
Geosciences Society (AOGS) 2nd Annual Meeting,(Singapore, June 20-24).
Asai, A., Nakajima, H., Shimojo, M., White, S. M., and Hudson,
H. S.: 2005, Preflare Features in Radios and in Hard X-Rays,
The 9th Asian Pacific Regional IAU Meeting, (Indonesia, July
26-29).
Asai, A., Yokoyama, T., Shimojo, M., Masuda, S., and Shibata,K.: 2005, Evolution of H-alpha Flare Kernels and Energy
Release, The 6th Solar-B Science Meeting, (Kyoto, Japan,
Nov. 8-11).
Asai, A., Yokoyama, T., Shimojo, M., Masuda, S., and Shibata,K.: 2005, Flare Ribbon Expansion and Energy Release,
International Solar Workshop on Transient Phenomena on the
Sun and Interplanetary Medium, (India, Apr. 5-7).
Asano, K.: 2005, UHECR and Neutrino Production in GammaRay Bursts, Santorini Summer School on Gamma-Ray Bursts,(Santorini, Greece, Aug. 29-Sep.2).
Asano, K.: 2006, High Energy Cosmic Rays, Neutrinos, andPhotons from Gamma-Ray Bursts, International Workshop on
Energy Budget in the High Energy Universe, (Tokyo, Japan,
Feb. 22-24).
Asayama, S.: 2005, Current Status of the ALMA Band 4,
Workshop on Submillimeter Astronomy and ReceiverTechnologies Joint Workshop with the 6th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Nanjing, China, Dec. 8-10).
Baba, N., Murakami, N., Tate, Y., Sato, Y., Tamura, M.: 2005,
Objective spectrometer for exoplanets based on nullingpolarization interferometry, SPIE Conference, (San Diego,
USA, Jul. 31-Aug. 4).
Cellino, A., Belskaya, I., Bendjoya, P., di Martino, M., Gil-Hutton,
R., Muinonen, K., Tedesco, E. F., Yoshida, F.: 2005, Asteroid
polarimetry: Recent results, IAU Symposium 229: Asteorids,
Comets, Meteors, (Brazil, Aug. 7-12).
Endo, A., Noguchi, T., Matsunaga, T., and Tamura, T.: 2005,
Development of Nb/Al-AlNx/Nb SIS Junctions for High-Jc
Submillimeter Mixers, Workshop on Submillimeter
Astronomy and Reciever Technologies / Joint Workshop withthe 6th Workshop on Submillimeter-Wave ReceiverTechnologies in Eastern Asia, (Nanjing, China, Dec. 8-10).
Enoki, M.: 2006, Subaru Telescope Sciences Archive System:
SMOKA, Subaru East Asia Youth Seminar 2006, (Hawaii,
USA, Mar. 13-17).
Enoki, M., Inoue, K. T., Nagashima, M., Sugiyama, N.: 2005,
Gravitation Radiation from Coalescing Supermassive Black
Hole Binaries in a Hierarchical Galaxy Formation, Formationand Evolution of Supermassive Binary Black Holes, Workshop
of Yukawa Institute of Theoretical Physics, (Kyoto, Japan, Sep.
20-21).
Enoki, M., Nagashima, M., Yahagi, H., Yoshii, Y., Gouda, N.:
2005, QSO formation and its environments, The 9th Asian-Pacific Regional IAU Meeting 2005, (Bali, Indnesia, July 2629).
Enya, K., et al. including Tamura, M., Abe, L.: 2005, Cryogenic
infrared optics for the SPICA coronagraph, Direct Imaging of
Exoplanets: Science & Techniques, Proceedings IAU
Colloquium 200, (Villefranche-sur-Mer, France, Oct. 3-7).
Ezawa, H.: 2005, ASTE: The Atacama Submillimeter Telescope
Experiment, Submillimeter Astronomy In the Era of the SMA,
(Harvard University, Cambridge, MA, USA, June 13-16).
Ezawa, H.: 2005, ASTE: The Atacama Submillimeter Telescope
Experiment, Workshop on Submillimeter Astronomy andReceiver Technologies / Joint Workshop with the 6thWorkshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nanjing, China, Dec. 8-10).
Ezawa, H.: 2006, The ASTE Project, Perspective of
Submillimeter Astronomy with the Atacama Submillimeter
Telescope Experiment (ASTE), (Tokyo, Mitaka, Mar. 16-17).
Ezawa, H., Kawabe, R., Kohno, K., Yamamoto, S., and the
ASTE team: 2005, ASTE: The Atacama Submillimeter
Telescope Experiment, XXVIIIth General Assembly ofInternational Union of Radio Science (URSI), (New Delhi,
India, Oct. 23-29).
Ezawa, H., Kohno, K., Kawabe, R., Yamamoto, S., and the
ASTE team: 2005, Progress and Current Status of The
Atacama Submillimeter Telescope Experiment (ASTE), The
9th Asian-Pacific Regional IAU Meeting 2005, (The Westin
Resort, Nusa Dua, Bali, Indonesia, July 26-29).
Fujimoto, M.-K.: 2005, Ten Years of the TAMA Project, 6th
Edoardo Amaldi Conference on Gravitational Waves,(Okinawa, Japan, June 20-24).
Fujita, Y.: 2006, The generation of magnetic fields and X-ray
observations, The Origin and Evolution of Cosmic Magnetism,(CNR Area della Ricerca, Bologna, Italy, 29 Aug. 29-Sept. 2).
Furusho, R., Kawakita, H., Ikeda, Y., Kasuga, T., Sato, Y.,
Watanabe, J.: 2005, Polarimetric Imager for Comets: PICO,
American Astronomical Society, DPS meeting #37, #16.11,(Cambridge, UK, Sep. 4-9).
Furusho, R., Kawakita, H., Watanabe, J., Fuse, T., Arimoto, N.,
Sadakane, K., Ohnishi, K., Ohkubo, M.: 2005, Abundant CO2of comet C/2001 A2(LINEAR) derived from a new evaluation
method, AOGS 2nd Annual meeting, (Singapore, June 20-24).
Goossens, S., Matsumoto, K., Visser, P. N. A. M.: 2005, Global
and Local Gravity Field Determination from Lunar Prospector
Tracking Data, 2005 American Geophysical Union Fall
Meeting, (San Francisco, USA, Dec. 5-9).
Hagiwara, Y.: 2005, HI/OH absorption in N6240, New
Techniques in Low Frequency Radio Astronomy, (Tasmania,
Australia, Dec. 7-10).
Hagiwara, Y.: 2005, KVN Summer School, (Muju, Korea, Aug.
17-19).
Hamana, T.: 2005, Theoretical/numerical predictions for weaklensing halo search, Probing the Dark Universe with Subaru
and Gemini, (Waikoloa, Hawaii, Nov. 6-9).
Hanada, H., Iwata, T., Namiki, N., Kawano, N., Asari, K.,
Ishikawa, T., Kikuchi, F., Liu, Q., Matsumoto, K., Noda,
H., and Tsuruta, S.: 2005, Gravimetric missions by VLBI and
Doppler in SELENE, AGU 2005 Fall Meeting, (San Francisco,USA, Dec. 5-9).
Hanada, H., Iwata, T., Namiki, N., Kawano, N., Asari, K.,
Ishikawa, T., Kikuchi, F., Liu, Q., Matsumoto, K., Noda,
H., Ping, J., Tsuruta, S., Iwadate, K., Kameya, O., Kuji, S.,
67

Tamura, Y., Hong, X., Aili, Y., Ellingsen, S.: 2005,
Gravimetric Missions in Japanese Lunar Explorer, XXVIIIthGeneral Assembly of International Union of Radio Science(URSI), (New Delhi, India, Oct. 23-29).
Hanada, H., Kunimori, H., Hosokawa, M., Katayama, M.,
Noda, H., Araki, H., Sasaki, S., Kawano, N.: 2005,
Moonlight project - Observations of Lunar rotation andEphemeris by optical methods on the Moon, International
Lunar Conference 2005, (Toronoto, Canada, Sep. 18-23).
Hanaoka, Y.: 2005, Ha Polarimetry as a probe of Chromospheric
Magnetic Fields, NSO Workshop #23 Solar MHD: Theory andObservations - a High Spatial Resolution Perspective,(Sunspot, USA, July 18-22).
Hanaoka, Y.: 2005, High-Precision Imaging Polarimetry in the
Ha line, 4th Solar Polarization Workshop, (Boulder, USA,
Sep. 19-23).
Hanaoka, Y.: 2005, Ha Polarimetry and Magnetic Field Structurein the Chromosphere, International Workshop The 6th Solar-B
Science Meeting, (Kyoto, Japan, Nov. 8-11).
Hanaoka, Y.: 2006, Ha Polarimetry as a Probe for the
Chromospheric Vector Magnetic Fields, 2006 Spring Meetingfor the Korea-Japan Collaborative Research on the Solar
Activity, (Seoul, Korea, Mar. 8).
Hanayama, H.: 2005, Biermann Mechanism in Primordial
Supernova Remnant and Seed Magnetic Fields, The Origin and
Evolution of Cosmic Magnetism, (Bologna, Italy, Aug. 29).
Hanayama, H.: 2005, Long-Term Evolution of Supernova
Remnants in Magnetized Interstellar Medium, Polarization
2005, (Orsay, France, Sep. 12).
Hanayama, H.: 2006, Seed Magnetic Fields from Primordial
Supernova Remnant, East Asian Young Astronomers Meeting
2006, (Kiyosato, Japan, Feb. 13).
Hara, H.: 2005, Solar-B EUV Imaging Spectrometer, The 6th
Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
Hara, H.: 2005, Solar-B/EIS, Stereo/Solar-B Science Planning
Workshop, (Turtle Bay, Oahu, Hawaii, Nov. 15-18).
Harada, Y., Heki, K.: 2005, Secular Obliquity Variations Due to
Climate Friction on Mars: Re-Examination in Influence ofMartian Internal Viscosity Structure, International Workshop
by 21st Century Earth Science COE Program: Predictability of
the Evolution and Variation of the Multi-scale Earth System,(Tokyo, Japan, Sep. 21-22).
Harada, Y., Heki, K.: 2005, Secular Obliquity Variations Due to
Climate Friction on Mars: Re-Examination in Influence ofMartian Internal Viscosity Structure, 2005 American
Geophysical Union Fall Meeting, (San Francisco, USA, Dec.
5-9).
Hatsukade, B., Kohno, K., Endo, A., Tosaki, T., Ohta, K., Kawai,N., Vreeswijk, P., Cortes, J., Nakanishi, K., Okuda, T.,
Muraoka, K., Kawabe, R.: 2005, A Search for Molecular Gas
toward the Host Galaxy of GRB 980425 Using ASTE,
Workshop on Submillimeter Astronomy and ReceiverTechnologies / Joint Workshop with the 6th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Nanjing, China, Dec. 8-10).
Hattori, M., Ohta, I. S., Takahashi, J., and Matsuo, H.: 2005,
Development of bolometric astronomical interferometer in mm
and submm wavebands, The Joint 30th International
Conference on Infrared and Millimeter Waves and 13th
International Conference on Terahertz Electronics, (Virginia,
USA, Sep. 19-23).
68

Hayama, K., Fujimoto, M.-K., and TAMA collaboration: 2005,
Wavelet-based method to monitor non-stationary signals in aninterferometer, 6th Edoardo Amaldi Conference on
Gravitational Waves, (Okinawa, Japan, June 20-24).
Hayashi, M., Nakamoto, T., Kita, T., Tachibana, S.: 2005, ShockWaves in Protoplanetary Disk Generated by Magnetic Bubblesof X-Ray Flares I: MHD Simulations, Protostars & Planets V,(Big Island of Hawaii, USA, Oct. 24-28).
Hayashi, M.: 2005, MHD Simulation of Jets & Flares of PreMain Sequence Stars, Magnetohydrodynamic Phenomena in
Galaxies, Accretion Disks, and in Star Forming Regions,(Chiba, Japan, Nov. 17-18).
Higuchi, A.: 2005, Orbital Evolution of Planetesimals by the
Galactic Tide, American Astronomical Society, Division on
Dynamical Astronomy, (Santa Barbara, California, USA, Apr.
10-14).
Higuchi, A.: 2005, Orbital Evolution of Planetesimals under the
Galactic Tide, Asia Oceania Geosciences Society 2nd Annual
Meeting, (Suntec, Singapore, June 10-14).
Higuchi, A.: 2005, Evolution of the Oort Cloud under Galactic
Perturbations, American Astronomical Society, Division on
Planetary Science, (Cambridge, UK, Sep. 4-8).
Higuchi, A.: 2005, Evolution of the Oort Cloud Under the
Galactic Tide, Protostars and Planet V, (Hawaii, USA, Oct. 2428).
Hiramatsu, M.: 2006, ASTE observations of Chamaeleon star
forming region, Perspective of Submillimeter Astronomy with
Atacama Submillimeter Telescope Experiment (ASTE),(Tokyo, Japan, Mar. 16-17).
Hiramatsu, M., Hayakawa, T., Tatematsu, K., Hasegawa, T.,
Onishi, T., Mizuno, A., and ASTE team: 2005, ASTE
Submillimeter Observations of YSO-Close-Packed Region
Cederblad 110, Submillimeter Astronomy In the Era of the
SMA, (Harvard University, Cambridge, MA, USA, June 1316).
Hiramatsu, M., Hayakawa, T., Tatematsu, K., Hasegawa, T.,
Onishi, T., Mizuno, A., and ASTE team: 2006, Outflow - CoreInteraction in Chamaeleon Star Forming Region, East-Asian
Workshop “Evolution of Molecular Clouds: Recent
Observational and Theoretical Results and Prospects”, (Tokyo,
Japan, Feb. 6-8).
Hirota, T.: 2005, Water maser observations for Orion region,
Japan-Korea VLBI Meeting 2005, (Ishigaki Island, Japan, Nov.
10-11).
Hirota, T.: 2006, East Asia Winter School on Radio Astronomy,
The 2nd Meeting of East Asia Core Observatories Association(EACOA), (Tokyo, Japan, Mar. 7).
Hirota, T., and Yamamoto, S.: 2005, Molecular Line
Observations of Chemically Young Dark Cloud Cores, IAU
Symposium 231, “Astrochemistry Throughout the Universe:
Recent Successes and Current Challenges”, (Asilomar, CA,
USA, Aug. 29-Sep. 2).
Honda, S., Aoki, W., Ishimaru, Y., Wanajo, S., Ryan, S. G.:
2005, Subaru/HDS studies of r-process elements in metal-poorstars from near UV spectra, Origin of Matter and Evolution of
Galaxies (OMEG05), (Tokyo, Japan, Nov. 7-11).
Honda, S., Aoki, W., Ishimaru, Y., Wanajo, S., Ryan, S. G.,
Kajino, T., Ando, H., Beers, T. C.: 2005, Subaru/HDS studiesof r-process elements in metal-poor stars from near UV spectra,
IAU Symposium 228, From Lithium to Uranium Elemental
Tracers of Early Cosmic Evolution, (Paris, France, May 23-

27).
Honma, M.: 2005, Water maser observations for S269, JapanKorea VLBI Meeting 2005, (Ishigaki Island, Japan, Nov. 1011).
Hori, K., Ichimoto, K., Sakurai, T.: 2005, Flare-associatedoscillations in coronal multiple loops observed with the
Norikura Green-line Imaging System, International Workshop
The 6th Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
Hori, K., Katsukawa, Y., Oka, M., Sakamoto, Y., Watanabe, T.,
and Kurokawa, H.: 2005, RHESSI and NoRH Observations of
the 3 July 2002 Flare, SHINE (Solar Heliospheric andInterplanetary Environment) 2005 Workshop, (Kona, Hawaii,
Jul. 11-15).
Hosokawa, T., Inutsuka, S.: 2005, Formation of the Molecular
Gas Around Giant HII Regions, Protostars and Planet V,(Hawaii, USA, Oct. 24-28).
Hosokawa, T., Inutsuka, S.: 2005, Dynamical Expansion of
Ionization and Dissociation Front around a Massive Star,
Massive Star Birth: A Cross Raods of Astrophysics (IAU
Symp. 227), (Italy, Acireale, May. 16-20).
Hosokawa, T., Inutsuka, S.: 2006, Radiative Feedback from
Massive Stars (oral), East-Asian Molecular Cloud Workshop,(Mitaka, Japan, Feb. 6-8).
Ichimoto, K.: 2005, Optical Performance of the SOT: Test Reportfor the Flight Telescope, The 6th Solar-B Science Meeting,(Kyoto, Japan, Nov. 8-11).
Ichimoto, K., and the Solar-B Team: 2005, The Solar Optical
Telescope onboard the Solar-B: Capability of the Magnetic
Field Diagnostic, International Scientific Conference on
Chromospheric and Coronal Magnetic Fields (ESA SP-596),(Katlenburg-Lindau, Germany, Aug. 30-Sep. 2).
Iizuka, Y., Agata, H., Oe, M., Hiei, E.: 2006, Scientific
Dissemination of Eclipse Events in Japan, Annual Meeting of
the Balkans, Black Sea and Caspian Sea Regional Network on
Space Weather Studies, (Antalya, Turkey, Mar. 30).
Imai, H., Kan-ya, Y., and VERA Project Team: 2005, Water
masers in W51A observed with VERA, IAU Symposium 227:
Massive Star Birth, (Acireale, Italy, May 16-20).
Imanishi, M.: 2005, Buried AGNs and Compact Starbursts in
Nearby ULIRGs, Extreme Starbursts: Near and Far, (Yunnan
Province, China, Aug. 15-19).
Imanishi, M.: 2005, Nuclear starbursts in Seyfert 1 and 2
galaxies, Extreme Starbursts: Near and Far, (Yunnan Province,
China, Aug. 15-20).
Imanishi, M.: 2005, Buried AGNs in nearby ultraluminous
infrared galaxies, Infrared Diagnostics of Galaxy Evolution,(Pasadena, CA, USA, Nov. 14-16).
Imanishi, M.: 2005, Comparison of nuclear starbursts
luminosities between Seyfert 1 and 2 galaxies, based on
infrared 3-4 micron spectroscopy, Infrared Diagnostics ofGalaxy Evolution, (Pasadena, CA, USA, Nov. 14-16).
Imanishi, M.: 2005, Millimeter interferometric investigations of
the energy sources of nearby luminous infrared galaxies,
Extreme Starbursts: Near and Far, (Yunnan Province, China,
Aug. 15-19).
Imanishi, M.: 2005, Millimeter interferometric investigations of
the energy sources of ULIRGs, Galactic and Extragalactic ISM
Modelling in an ALMA Perspective, (Gothenburg, Sweden,
Oct. 13-15).
Inoue, M.: 2005, Progress report in Japan, ISSC14, (Puna, India,
Nov. 4-5).

Inoue, M.: 2006, Status of VSOP-2 and SKA, ISSC15, (Socorro,
USA, Mar. 16-17).
Inoue, M.: 2006, SKA and Cooperation of International Projects
in East Asia, EACOA, (Tokyo, Japan, Mar. 7).
6
Inoue, S.: 2005, Li in Very Metal-Poor Halo Stars Observed bySubaru/HDS and Implications, From Lithium to Uranium:
Elemental Tracers of Early Cosmic Evolution, IAU
Symposium 228, (Paris, France, May 23-27).
Inoue, S.: 2005, Probing Magnetic Fields in Cluster Outskirts
through Hard X-Rays and Gamma-Rays Induced by UltraHigh Energy Protons, The Origin and Evolution of Cosmic
Magnetism, (Bologna, Italy, Aug. 28-Sep. 2).
Inoue, S.: 2005, Gamma-Ray and Cosmic Ray Astrophysics ofClusters, GLAST Science Workshop, (Tokyo, Japan, Nov. 2425).
Inoue, S.: 2006, Astrophysical Origins of the Highest Energy
Cosmic Rays, Energy Budget in the High Energy Universe,(Kashiwa, Japan, Feb. 22-24).
Inoue, S.: 2006, Exploring the Very High Redshift Universe
through GRBs with ALMA and Subaru, ALMA Science
Working Group Meeting, (Tokyo, Japan, Mar. 2-3).
Iono, D.: 2005, SMA Observations of Nearby and Distant Active
Galaxies, Inagural Japan-Taiwan ALMA Science Workshop,(Taiwan, Dec. 15-16).
Iono, D.: 2006, Revealing the Active High-z Universe with the
SMA, American Astronomical Society Meeting 207,
(Washighton D.C., USA, Jan. 8-12).
Ito, T., Strom, R. G., Malhotra, R., Yoshida, F., Kring, D. A.:
2005, Size distribution of asteroids and old terrestrial creaters:
Implications for asteroidal dynamics during LHB, AsiaOceania Geosciences Society 2nd Annual Meeting, (Singapore,
June 20-25).
Ito, T., Strom, R. G., Malhotra, R., Yoshida, F., Kring, D. A.:
2005, The origin of planetary impactors in the inner solar
system., IAU Symposium 229: Asteorids, Comets, Meteors,(Rio de Janeiro, Brazil, Aug. 7-12).
Iwata, I., Ohta, K., Tamura, N., Akiyama, M., Aoki, K., Ando,
M., Kiuchi, G.: 2005, Evolution of Lyman Break Galaxies
From z＝5 to 3, The Fabulous Destiny of Galaxies: Bridging
Past and Present, (Marseille, France, June 20-24).
Iwata, T., Namiki, N., Hanada, H., Kawano, N., and Takano, T.:2005, Global mapping of lunar gravity field using SELENE
two small satellites, IAA International Symposium on LowCost Planetary Missions, (Kyoto, Japan, Oct. 11-13).
Jike, T., and VERA Team: 2005, Start of semi-regular geodetic
observations with VERA, 17th Working Meeting on European
VLBI for Geodesy and Astrometry, (Noto, Italy, Apr. 22-23).
Jike, T., Tamura, Y., Manabe, S., and NAOJ VERA Group:
2006, The first year of VERA geodetic experiments, 4th IVS
General Meeting, (Concepción, Chile, Jan. 9-11).
Kajino, T.: 2005, Radioactive Nuclei in Supernovae and the BigBang Cosmology, APCTP - Korean Physical Society
Workshop, (Jeonju, Korea, Oct. 20-22).
Kajino, T.: 2005, Big-Bang Cosmology, 3rd European Summer
School on Experimental Nuclear Astrophysics, (Santa Tecla,
Sicily, Italy, Oct. 2-8).
Kajino, T.: 2005, Neutrino processes in Supernova
Nucleosynthesis, 2nd Joint US-Japan Physical Society Meetin,
Workshop on Neutrino Astrophysics, (Hawaii, USA, Sep. 1822).
Kajino, T.: 2005, Nucleosynthesis in Supernovae and the Big69

Bang I and II, 4th International Summer School, (Tokyo,
Japan, Aug. 18-22).
Kajino, T.: 2005, Big-Bang Cosmology and Supernova
Nucleosynthesis, Advanced Studies Institute on Symmetries
and Spin, (Charles University, Prague, July 27-Aug. 3).
Kajino, T.: 2005, A model of dark mater and dark energy andtheir observational test, INT 2005 Program on Underground
Science, (Seattle, USA, July 17-22).
Kajino, T.: 2005, Big-Bang Cosmology and Cosmic Chemical
Evolution, 0th International Nuclear Physics Divisional
Conference of the European Physical Society on Nuclear
Physics in Astrophysics, (ATOMKI, Debrecen, Hungary, May
16-20).
Kajino, T.: 2006, Supernova neutrino-process: Nucleosynthesis
and neutrino oscillation parameters,θ13 and mass hierarchy,
International Symposium on Structure of Exotic Nuclei and
Nuclear Forces, (Tokyo, Japan, Mar. 9-12).
Kajino, T.: 2006, Explosive nucleosynthesis and Big-Bangcosmology, International RCNP-JAEA Workshop on Nuclear
Photon Science “Hadron-nuclear physics probed by photon”,(Kyoto, Japan, Feb. 16-18).
Kameno, S.: 2005, VSOP-2 Science Case, URSI 28th General
Assembly, (New Delhi, India, Oct. 23-29).
Kameno, S.: 2005, Interferometry and Visibility, KVN Summer
School, (Muju, Korea, Aug. 17-19).
Kameno, S.: 2005, Amplitude and Phase Calibration for
Visibilities, KVN Summer School, (Muju, Korea, Aug. 17-19).
Kameya, O.: 2005, Status of VERA stations, Japan-Korea VLBI
Meeting 2005, (Ishigaki Island, Japan, Nov. 10-11).
Kameya, O., Kurayama, T., Suda, H., Kobayashi, H., and
VERA member: 2005, Water-Vapor Maser VLBI
Observations of W3OH Region using VERA, The 9th AsianPacific Regional IAU Meeting, (Nusa Dua, Bali, Indonesia, Jul.
26-29).
Kamikura, M., et al.: 2005, Design of ALMA band 8 Design of
ALMA band 8 ortho ortho-mode transducer, Submillimeter
Receiver Workshop, (Nanjing, Dec. 8-10).
Kamohara, R., Omodaka, T., Deguchi, S., Kobayashi, H., and
VERA team: 2006, Study of the H2O maser proper motions in
the circumstellar envelope around VX Sagittarii with VERA,
East Asia Young Astronomer Meeting 2006, (Yamanashi,
Japan, Feb. 13-18).
Kano, R.: 2005, Micro-Flare and High-Speed Down-Flowobserved with VTT, The 6th Solar-B Science Meeting, (Kyoto,
Japan, Nov. 8-11).
Kano, R.: 2005, Solar-B/XRT, Stereo/Solar-B Science Planning
Workshop, (Turtle Bay, Oahu, Hawaii, Nov. 15-18).
Kashikawa, N.: 2006, The End of the Reionization Epoch Probed
by Ly-alpha Emitters, STScI-Workshop: The End of the Dark
Ages: From First Light to Reionization, (Baltimore, USA, Mar.
13-15).
Kasuga, T., Watanabe, J., Ebizuka, N.: 2005, Metall abundancesof 2004 Geminid Meteor Spectrum: Extremely Na Depletion ?,AOGS 2nd Annual meeting, (Singapore, June 20-24).
Katsukawa, Y.: 2005, Observational analysis of the relation
between coronal loop heating and photospheric magnetic field,
The 6th Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
Katsukawa, Y.: 2005, Calibration of SOT Dopplergrams, The 6th
Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
12
Kawabe, R.: 2006, ASTE CO J＝3-2 observations of themolecular outflows in Taurus L1551 region, Perspective of70

Submillimeter Astronomy with Atacama Submillimeter
Telescope Experiment (ASTE), (Tokyo, Japan, Mar. 16-17).
Kawagoe, S.: 2005, Effect in Supernova-Shock Propagation,
OMEG 05, (Kyoto, Japan, Nov. 8-11).
Kawagoe, S.: 2005, Shock Propagation in Prompt Supernova
Explosion and the MSW effect of Neutrino, HAW 05, (Maui,
Hawaii, Sep. 18-22).
Kawagoe, S.: 2005, Shock wave Propagation in Prompt
Supernova Explosion and the MSW effect of Neutrino, TAUP
2005, (Zaragoza, Spain, Sep. 14).
Kawagoe, S.: 2005, Shock wave Propagation in the Adiabatic
Prompt Explosion Model and Neutrino Oscillation, The 59th
Yamada Conference, (Tokyo, Japan, June 20-24).
Kawaguchi, N.: 2005, Optical Fiber connected VLBI Network inJapan, 4th eVLBI workshop, (Sydney, Australia, Jul. 13).
Kawaguchi, N.: 2005, Status of fiber linked observations, JapanKorea VLBI Meeting 2005, (Ishigaki Island, Japan, Nov. 1011).
Kawaguchi, N.: 2005, Status of VERA frontend and backend
system, Japan-Korea VLBI Meeting 2005, (Ishigaki Island,
Japan, Nov. 10-11).
Kawaguchi, N.: 2005, VLBI Technology, Observations and Its
Future, Japan-Korea VLBI Meeting 2005, (Nigelia, Japan, Apr.
20).
Kawaguchi, N.: 2005, VLBI Technology, Observations and Its
Future, Japan-Korea VLBI Meeting 2005, (Nigelia, Japan, Apr.
21).
Kawaguchi, N.: 2006, Fiber-linked Real-time VLBI Network,
The 2nd Meeting of East Asia Core Observatories Association(EACOA), (Tokyo, Japan, Mar. 7).
Kawakita, H., Dello Russo, N., Furusho, R., Fuse, T., Watanabe,J., Boice, D., Arimoto, N., Sadakane, K., Ohkubo, M.,
Ohnishi, K.: 2005, Nuclear spin temperatures of water,
ammonia and methane in comet C/2001 Q4 (NEAT),
American Astronomical Society, DPS meeting #37, #16.11,(Cambridge, UK, Sep. 4-9).
Kawakita, H., Watanabe, J., Furusho, R., Fuse, T., Boice, D.:2005, Nuclear Spin Temperature of Methane in Comet C/2001
Q4, AOGS 2nd Annual meeting, (Singapore, June 20-24).
Kawamura, S., and the DECIGO working group: 2005, The
Japanese Space Gravitational Wave Antenna - DECIGO, 6th
Edoardo Amaldi Conference on Gravitational Waves,(Okinawa, Japan, June 20-24).
Kawazoe, F., Kokeyama, K., Sato, S., Somiya, K., Fukushima,M., Miyakawa, O., Arai, N., Kawamura, S., Sugamoto, A.:
2005, The experimental plan for a 4m Resonant Sideband
Extraction interferometer, 6th Edoardo Amaldi Conference on
Gravitational Waves, (Okinawa, Japan, June 20-24).
Kleinman, S. J.: 2006, SUBARU East Asia Youth Seminar,
Subaru Instruments SUBARU East Asia Youth Seminar,(Kona, Hawaii, Mar 13-17).
Kleinman, S. J.: 2006, Science with Surveys, Subaru Instruments
SUBARU East Asia Youth Seminar, (Kona, Hawaii, Mar 1317).
Kobayashi, C.: 2005, Galactic and Cosmic Chemical Evolution
with Hypernovae, IAU Symposium 228, From Lithium to
Uranium: Elemental Tracers of Early Cosmic Evolution, (Paris,
France, May 22-28).
Kobayashi, C.: 2005, Simulating Cosmic Chemical Enrichment,
MPA Workshop, From Simulations to Surveys, (Ringberg,
Germany, June 26-July 1).

Kobayashi, C.: 2005, Supernova Feedback and Galaxy
Formation, Japanese-German Symposium 2005, The
Formation and Co-Evolution of Black Holes and Galaxies,(Regensburg, Germany, Sept. 18-22).
Kobayashi, C.: 2005, Cosmological simulation with Hypernova
Feedback, Workshop on Measuring the Diffuse Intergalactic
Medium, (Hayama, Japan, Oct. 10-12).
Kobayashi, C.: 2005, Galactic and Cosmic Chemical Evolution
with Hypernovae, International Symposium on Origin of
Matter and Evolution of Galaxies, (Tokyo, Japan, Nov. 8-11).
Kobayashi, H.: 2005, East Asia VLBI Network, Japan-Korea
VLBI Meeting 2005, (Ishigaki Island, Japan, Nov. 10-11).
Kobayashi, H.: 2005, Future plan of VERA, Japan-Korea VLBI
Meeting 2005, (Ishigaki Island, Japan, Nov. 10-11).
Kobayashi, H.: 2005, Status of VERA antenna, Japan-Korea
VLBI Meeting 2005, (Ishigaki Island, Japan, Nov. 10-11).
Kobayashi, K.: 2005, East Asia VLBI Network, The 1st East
Asia VLBI CORE Observatories work shop, (Hongo, Japan,
Sep. 26).
Kobayashi, K.: 2005, VERA system, The 9th Asian-PacificRegional IAU Meeting 2005, (Bali, Indonesia, July 26-29).
Kobayashi, K.: 2006, East Asian VLBI network, The 2nd
Meeting of East Asia Core Observatories Association(EACOA), (Tokyo, Japan, Mar. 7).
Kodama, T., et al.: 2005, Panoramic View of Cluster Evolution,
Japanese-German Symposium 2005 “The Formation and CoEvolution of Black Holes and Galaxies”, (Regensburg,
Germany, Sept. 18-22).
Kodama, T., et al.: 2005, Panoramic View of Cluster Evolution,
MPE Workshop “Stellar Populations, A Rosetta Stone for
Galaxy Formation”, (Ringberg Castle, Munich, Alemania, July
4-8).
Kokeyama, K., Sato, S., Kawazoe, F., Somiya, K., Fukushima,M., Kawamura, S., Sugamoto, A.: 2005, Downselect of thesignal extraction scheme for LCGT, 6th Edoardo Amaldi
Conference on Gravitational Waves, (Okinawa, Japan, June
20-24).
Kokubo, E.: 2005, From Protoplanets to Terrestrial Planets, Early
Earth Symposium, (Makuhari, Japan, May 20).
Kokubo, E.: 2005, From Protoplanets to Terrestrial Planets:
Statistical Properties of Assembled Planets, 37th Annual
Meeting of the AAS Division for Planetary Sciences,(Campbridge, UK, Sep. 4-9).
Kokubo, E.: 2005, Formation of Terrestrial Planets and the Originof Water on the Earth, International Symposium on Origins ofLife and Astrobiology, (Niigata, Japan, July 1).
Komiyama, Y.: 2006, Hyper Suprime: design and current status,
Probing the Dark Universe with Subaru and Gemini,(Waikoloa, Hawaii, Nov. 6-9).
Kono, Y., Murata, Y., Hirabayashi, H., Wajima, K., Mochiduki,N., Toda, T., Kawaguchi, N.: 2006, Broadband VLBI Data
Downlink of VSOP-2, XXVIIth General Assembly ofInternational Union of Radio Science (URSI), (New Delhi,
India, Oct. 23-29).
Kubo, M.: 2005, Magnetic Correspondence between Moving
Magnetic Features and Penumbral Magnetic Fields, The 6th
Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
Kudoh, T.: 2005, MHD Numerical simulation of clouds and jets
in star forming regions, The joint conference of 19thInternational Conference on Numerical Simulation of Plasmas
and Asia Pacific Plasma Theory Conference, (Nara, Japan, July

12-15).
Kurayama, T.: 2005, Current Status of VERA: Data Analysis
System, Japan-Korea VLBI Meeting 2005, (Ishigaki Island,
Japan, Nov. 10-11).
Kusakabe, M.: 2005, The p-Process in the Carbon Deflagration
Model for Type Ia Supernovae and Chronology of the Solar
System Formation, Origin of Matter and Evolution of Galaxies(OMEG05), (Tokyo, Japan, Nov. 8-11).
Kuwabara, K., Tanikawa, K.: 2005, Departure from the free-fallthree problem, in Few-Body Problem: Theory and Computer
Simulations, A Workshop in celebration of the 60th Birthdayof Professor Mauri Valtonen, (Turku, Finland, July 4-9).
Lopez, J. R. C.: 2006, Morphology and Kinematics of Peculiar
Virgo Cluster Galaxies, Perspective of Submillimeter
Astronomy with Atacama Submillimeter Telescope
Experiment (ASTE), (Tokyo, Japan, Mar. 16-17).
Lopez, M. S. R.: 2006, Molecular gas and star formation in the
Magellanic clouds, Perspective of Submillimeter Astronomy
with Atacama Submillimeter Telescope Experiment (ASTE),(Mitaka, Japan, Mar. 16-17).
Machida, M., Matsumoto, R.: 2005, MHD simulations of X-ray
Flares in Black Hole Accretion Disks, Magneto hydrodynamic
Phenomena in Galaxies, Accretion Disks and Star Forming
Regions, (Chiba, Japan, Nov. 17).
Maezawa, H.: 2006, Submillimeter-wave Band Observation ofPlanetary Atmosphere, Perspective of Submillimeter
Astronomy with Atacama Submillimeter Telescope
Experiment (ASTE), (Mitaka, Japan, Mar. 16-17).
Masaki, Y., Matsuzaka, S., and Tamura, Y.: 2006, Local tie
survey at VERA Ogasawara station at site Chichijima, IVS
2006 General meeting, (Concepción, Chile, Jan. 9-12).
Matsui, H., Habe, A., Saitoh, R. T.: 2005, A Massive Black Holeand Nuclear Star Burst, Island Universes - Structure andEvolution of Disk Galaxies, (Netherland).
Matsumoto, K., Hanada, H., Tsuruta, S., Kawano, N., Iwata,T., Namiki, N., Rowlands, D.: 2005, A simulation study for
anticipated accuracy of lunar gravity filed model by SELENE
tracking data, Dynamic Planet 2005, (Cains, Australia, Aug.
22-26).
Matsumoto, K., Sato, T., Tamura, Y., Fujimoto, H., Nishino,
M., Hino, R., Higashi, T., and Kanazawa, T.: 2005, Ocean
bottom pressure observations off Sanriku of Japan Comparison with tide models, altimeter data and ECCO model-, Dynamic Planet 2005, (Cairns, Australia, Aug. 22-26).
Matsumoto, K., Shum, C. K., Yi, Y., Wang, Y.: 2005, Southern
Ocean Tide Modeling Based on TOPEX/POSEIDON and
ERS, International Geoscience And Remote Sensing
Symposium 2005 (IGARSS 2005), (Seoul, Korea, July 25-29).
Matsuo, H.: 2005, Development of superconductive imaging
submillimeter-wave camera (SISCAM), Workshop on
Submillimeter Astronomy and Receiver Technologies,(Yanjing, China, Dec. 8-10).
Matsuo, H.: 2005, Future Prospect of Superconducting Detectors
in Terahertz Frequencies, 11th International Woekshop on Low
Temperature Detectors, (Tokyo, Japan, July 31-Aug. 5).
Matsuo, H., Ariyoshi, S., Yamakura, T., Ezawa, H., Kobayashi,J., Mori, Y., Nagata, H., Otani, C., Shimizu, H. M.: 2005,
Superconducting Imaging Submillimeter-wave Camera(SISCAM) for Atacama Submillimeter Telescope Experiment,
11th International Woekshop on Low Temperature Detectors,(Tokyo, Japan, July 31-Aug. 5).
71

Matsuo, H., Nagata, H., Ezawa, H., Mori, Y., Kobayashi, J.,
Ariyoshi, S.: 2005, Development of Terahertz Imaging Arrayusing SIS Photon Detectors, International Workshop on
Terahertz Technology, (Osaka, Japan, Nov. 16-18).
Matsuo, H., Ohta, I., Hattori, M., Takahashi, J., Miyamoto, H.:
2005, Development of a Multi-Fourier TransformInterferometer, XXVIIIth General Assembly of International
Union of Radio Science, (New Delhi, India, Oct. 23-29).
Minamidani, T.: 2006, Submillmeter observations of LMC/SMC,
Perspective of Submillimeter Astronomy with Atacama
Submillimeter Telescope Experiment (ASTE), (Mitaka, Japan,
Mar. 16-17).
Moriguchi, Y., Tamura, K., Tawara, Y., Sasago, H., Yamamoka,
K., Onishi, T., Fukui, Y.: 2005, ASTE and NANTEN
Observations toward the TeV Gamma-Ray SNR G347.3-0.5,
Submillimeter Astronomy In the Era of the SMA, (Harvard
University, Cambridge, MA, USA, June 13-16).
Muraoka, K.: 2005, ASTE Observations of the CO 3-2 Emission
Toward the Disk Region of the Barred Spiral Galaxy M83,
Submillimeter Astronomy In the Era of the SMA, (Harvard
University, Cambridge, MA, USA, June 13-16).
Muraoka, K.: 2006, CO(J＝3-2) wide area imaging of M83 using
ASTE, Perspective of Submillimeter Astronomy with Atacama
Submillimeter Telescope Experiment (ASTE), (Tokyo, Japan,
Mar. 16-17).
Nagasawa, M., Lin, D. N. C.: 2005, Formation of terrestrial
planets from protoplanets in a dissipating protoplanetary disk,
Joint meeting for Earth and Planetary Science, Theinternational session: Earliest History of the Earth and Planets,(Makuhari, Japan, May 23).
Nagasawa, M., Lin, D. N. C.: 2005, Dynamical evolution of shortperiod planets in the multiple systems during the host-stars
contraction to the Main sequence, 36th Meeting of the AAS
Division on Dynamical Astronomy, (Santa Barbara, CA, USA,
Apr. 10-14).
Nagasawa, M., Lin, D. N. C., Thommes, E.: 2005, Formation ofterrestrial planets in a dissipating protoplanetary disk, Early
Earth Symposium: Discussion Meeting, (Makuhari, Japan,
May 20-22).
Nagasawa, M., Thommes, E., Lin, D. N. C.: 2005, The Final
Formation of Terrestrial Planets Induced by the Sweeping
Secular Resonance, AAS 37th Annual Meeting of the Division
for Planetary Sciences, (Cambridge, UK, Sep. 4-9).
Nagasawa, M., Thommes, E., Lin, D. N. C.: 2005, The Final
Formation of Terrestrial Planets in a Dissipating Protoplanetary
Disk: The Role of Secular Resonances, Protostars and Planets
V, (Waikoloa, HI, USA, Oct. 24-28).
Nagashima, M., Yahagi, H., Enoki, M., Yoshii, Y., Gouda, N.:
2006, Numerical Galaxy Catalog: a semi-analytic galaxy
formation model with high-resolution N-body simulations, The
9th Asian-Pacific Regional IAU Meeting 2005, (Bali, Indnesia,
July 26-29).
Nagata, H., Kobayashi, J., Matsuo, H., Akiba, M., Fujiwara, M.:
2005, Cryogenic GaAs Readout Circuits for Low Temperature
Detectors, XXVIIIth General Assembly of International Union
of Radio Science, (New Delhi, India, Oct. 23-29).
Nagata, H., Kobayashi, J., Matsuo, H., Akiba, M., Fujiwara, M.:
2005, Cryogenic Readout Integrated Circuits for submillimeter
Camera, The Joint 30th International Conference on Infrared
and Millimeter Waves and 13th International Conference on
Terahertz Electronics, (Virginia, USA, Sep. 19-23).
72

Nagata, H., Kobayashi, J., Matsuo, H., Akiba, M., Fujiwara, M.:
2005, Cryogenic Readout Integrated Circuits for
Submillimeter-wave Camera, 11th International Woekshop on
Low Temperature Detectors, (Tokyo, Japan, Jul. 31-Aug. 5).
Nakagawa, N., Arai, K., Kuroda, K., and TAMA collaboration:
2005, Influence of radio frequency harmonics in demodulation
on a laser interferometer, 6th Edoardo Amaldi Conference on
Gravitational Waves, (Okinawa, Japan, June 20-24).
Nakajima, T.: 2005, A Coronagraphic Search for Brown Dwarfs
and Planets around Nearby Stars, Ultralow-Mass Star
Formation and Evolution, (La Palma, Spain, June 28-July 1).
Nakamura, K.: 2005, Second Order Gauge Invariant Perturbation
Theory and Cosmological Perturbations, 15th workshop on
general relativity and gravitation in Japan, (Tokyo, Japan, Nov.
28-Dec. 2).
Nakamura, K.: 2006, Second Order Gauge Invariant Perturbation
Theory, The international workshop on “Black hole, spacetime
singularities, and cosmic censorship”, (Mumbai, India, Mar. 38).
Nakata, F., Bower, R. G., Balogh, M. L., Wilman, D. J.: 2005,
The Evolution of [OII] Emission from Cluster Galaxies, The
9th Asian-Pacific Regional IAU Meeting 2005, (Bali,
Indonesia, July 26-29).
Nishikawa, J., Murakami, N.: 2005, Combination of nullinginterferometer, nulling coronagraph, and modified pupil
method, IAU Colloquium 200, (Villefranche-sur-mer, France,
Oct. 3-7).
Noda, H., Hanada, H., Iwata, T., Namiki N., Tsubokawa T.,
Araki, H., Tazawa, S., Kawano, N.: 2005, Current status ofselenodetic mission in SELENE, EGU General Assembly,(Vienna, Austria, Apr. 25-29).
Noda, H., Inoue, M., Kawano, N., LLFAST: 2005, Low
frequency observations on the Moon, The 6th International
Workshop on Planetary and Solar Radio Emissions (PRE6),(Graz, Austria, Apr. 20-22).
Noda, H., Kawano, N., Inoue, M., Iwata T., Ono, T., Kondo, T.,
Takeuchi, H., Tsuchiya, F., Tokumaru, M., Hirosaki, T.,
Matsufuji, Y., Matsumoto, K., Misawa, H., Miyahara, A.,
Morioka, A.: 2005, Very Low Frequency Observation On The
Moon, International Lunar Conference 2005, (Toronoto,
Canada, Sep. 18-23).
Noguchi, T.: 2005, SIS junction fabrication at NAOJ, Workshop
on Submillimeter Astronomy and Reciever Technologies /Joint Workshop with the 6th Workshop on SubmillimeterWave Receiver Technologies in Eastern Asia, (Nanking,
China, Dec. 8-10).
Noguchi, T., Ueda, A., Sekimoto, Y., and Ishiguro, M.: 2005,
Photonic Local Oscillator for SIS Mixers, 18th Annual
Meeting of the IEEE Lasers and Electro-Optics Society,(Sydney, Australia, Oct. 23-27).
Noumaru, J.: 2005, Present and future perspective of Subaru
Instrumentation, The 9th Asian-Pacific Regional IAU Meeting
2005, (Bali, Indonesia, July 26-29).
Ohishi, M., Shirasaki, Y., Tanaka, M., Honda, S.,
Kawanomoto, S., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.: 2005,
Development of Japanese Virtual Observatory(JVO):
Experience on Interoperation with other Virtual Observatories
and its Future Plan, Astronomical Data Analysis Software andSystem XV, (San Lorenzo de El Escorial, Spain, Oct. 2-5).
Ohishi, N.: 2005, Interferometric Observation of a RapidlyRotating Star, Altair, Active OB-Stars: Laboratories for Stellar& Circumstellar Physics, (Sapporo, Japan, Aug. 29-Sep. 2).
Ohta, I. S., Hattori, M., Takahashi, J., Matsuo, H.: 2005, The first
astronomical mm and submm observation with Multi-Fourier
Transform interferometer, The Joint 30th International
Conference on Infrared and Millimeter Waves and 13th
International Conference on Terahertz Electronics, (Virginia,
USA, Sep. 19-23).
Okamoto, T.: 2005, The effect of feedback on the morphology ofgalaxy discs, The Formation of Disk Galaxies, (Ascona,
Switzerland, June 27-July 1).
Omukai, K.: 2005, Formation of the First- and Second-generation
Stars, IAU 9th Asian-Pacific Regional Meeting, (Bali,
Indonesia, July 26).
Omukai, K.: 2005, Formation of the First- and Second-generation
Stars, Stellar Evolution at Low Metallicity, (Tartu, Estonia,
Aug. 17).
Ootsubo, T., Watanabe, J., Hideyo, K.: 2005, Grain Properties ofOort cloud Comets:Modeling the Mineralogical Compositionof Cometary Dust from IR Emission Features, AOGS 2nd
Annual meeting, (Singapore, June 20-24).
Otsuka, M., Tamura, S., Tajitsu, A.: 2005, Highly Resolved
Spectroscopic Study of the PNe with HIDES, Planetary
Nebulae as astronomical tools, (Gdansk, Poland, Jun. 28-Jul.
2).
Oyama, T., Deguchi, S., Miyoshi, M., Kobayashi, H., Imai, H.,
Shen, Z.-Q.: 2005, Accurate Measurements of Proper Motionsof Maser Objects around the Galactic Center, The Paradoxes ofMassive Black Holes: A Case Study in the Milky Way, (Santa
Barbara, CA, USA, Apr. 14-16).
Petrov, L.: 2005, Accuracy of determination of coordinates of a
VLBI array, Japan-Korea VLBI Meeting 2005, (Ishigaki
Island, Japan, Nov. 10-11).
Rodriguez, J. A. P.: 2006, Sources, sinks and migrations patternsof dark veneers in the northern polar deposits of Mars, 37th
Lunar and Planetary Science Conference, (Houston, USA, Mar.
14).
Rosat, R., Watada, S., Sato, T., and Tamura, Y.: 2005,
Information on the Earth’s Deep Interior Conveyed by the2004 Sumatra-Andaman Earthquake Using Superconducting
Gravimeter Data, American Geophysical Union Fall Meeting,(San Francisco, CA, USA, Dec. 11-15).
Rosat, S., Sato, T., Fukushima, T., and Tamura, Y.: 2005,
Application of a Non-Linear Harmonic Analysis to the search
for the surface gravity effect of the translational motion of theinner core, Europian Geosciences Union General Assembly
2005, (Vienna, Austria, Apr. 24-29).
Rosat, S., Sato, T., Tamura, Y., Imanishi, Y., Hinderer, J.,
McQueen, H., Doi, K., Shibuya, K., Ohashi, M.: 2005, Lowfrequency seismic modes analysis after the Mw＝9 Sumatra
earthquake using superconducting gravimeters, Europian
Geosciences Union General Assembly 2005, (Vienna, Austria,
Apr. 24-29).
Saigo, K.: 2006, Evolution of first cores with mass accretion &possibility of observation, East-Asian Molecular CloudWorkshop, (Tokyo, Japan, Feb. 6-8).
Saigo, K., Tomisaka, K.: 2005, The Evolution of the First Core in
Rotating Molecular Cloud Core, Protostars and Planets V,(Waikoloa, HI, USA, Oct. 24-28).
Saito, M. M., Tanikawa, K.: 2005, The periodic orbits in therectilinear three-body problem, in Few-Body Problem: Theory

and Computer Simulations, A Workshop in celebration of the60th Birthday of Professor Mauri Valtonen, (Turku, Finland,
July 4-9).
Sakata, S., Kawamura, S., Sato, S., Somiya, K., Arai, K.,
Fukushima, M., Sugamoto, A.: 2005, Study of a quantum
nondemolition interferometer using ponderomotive squeezing,
Australia-Italy workshop on gravitational wave detection,(Gingin, Western Australia, Oct. 4-6).
Sakata, S., Kawamura, S., Sato, S., Somiya, K., Arai, K.,
Fukushima, M., Sugamoto, A.: 2005, Study of a quantum
nondemolition interferometer using ponderomotive squeezing,
6th Edoardo Amaldi Conference on Gravitational Waves,(Okinawa, Japan, June 20-24).
Sakurai, T.: 2005, Solar-B Modelling, Stereo/Solar-B Science
Planning Workshop, (Turtle Bay, Oahu, Hawaii, Nov. 15-18).
Sakurai, T.: 2005, Solar-B SWG Recap, Stereo/Solar-B Science
Planning Workshop, (Turtle Bay, Oahu, Hawaii, Nov. 15-18).
Sasaki, S.: 2005, Observation of Itokawa by a Small Surface
Rover MINERVA, Asia Oceania Geoscience Society 2005,(Singapore, July 20-24).
Sasaki, S.: 2005, Laboratory Simulation of Space Weathering toConnect a Missing Link between Asteroids and Meteorites,
Asia Oceania Geoscience Society 2005, (Singapore, July 2024).
Sasaki, S.: 2005, Space Weathering and Spectral Change on
Mercury, Asia Oceania Geoscience Society 2005, (Singapore,
July 20-24).
Sasaki, S.: 2005, In-situ exploration of the surface of asteroid
Itokawa by MINERVA engineering rover on board
HAYABUSA, Asteroids, Comets, Meteors 2005, (Buzios,
Brazil, Aug. 8-12).
Sasaki, S.: 2005, Spectral Observation of a New-Born Asteroid
832 Karin: A Body with Old and New Surfaces, Asteroids,
Comets, Meteors 2005, (Buzios, Brazil, Aug. 8-12).
Sasaki, S.: 2005, HAYABUSA Mission to Asteroid Itokawa: InSitu Observation and Sample Return, Dust in Planetary
Systems, (Kauai, USA, Sep. 26).
Sasaki, S.: 2005, Summary of Observation of Interplanetary andInterstellar Dust by Mars Dust Counter on Board NOZOMI,
Dust in Planetary Systems, (Kauai, USA, Sep. 27).
Sasaki, S.: 2006, Space Weathering: A Lesson from Itokawa,
Misasa International Symposium MISASA-2, The Evolution of
Early Stage of Earth and Solar System, (Kurayoshi, Japan, Feb.
25).
Sasaki, S.: 2006, Space Weathering of Rock Surface Without
Regolith: Laboratory Simulation of Spectral Change, 37th
Lunar and Planetary Science Conference, (Houston, USA, Mar.
13).
Sasaki, S.: 2006, Observations of 25143 Itokawa by the Asteroid
Multiband Imaging CAmera (AMICA) of HAYABUSA:
Morphology of Brighter and Darker Area, 37th Lunar andPlanetary Science Conference, (Houston, USA, Mar. 17).
Sasaki, S., Sasaki, T., Watanabe, J., Yoshida, F., Ito, T.,
Sekiguchi, T., Takato, N., Kawakita, H., Miyasaka, S.: 2005,
Spectral observation of a new-born asteroid 832 Karin: a bodywith old and new suefaces, IAU Symposium 229: Asteorids,
Comets, Meteors, (Brazil, Aug. 7-12).
Sasaki, T., Sasaki, S., Watanabe, J., Sekiguchi, T., Yoshida, F.,
Ito, T., Kawakita, H., Fuse, T., Takato, N., Dermawan, B.:
2005, Difference in Degree of Space Weathering on Newborn
Asteroid Karin, AOGS 2nd Annual Meeting, (Singapore, June73

20-24).
Sato, T.: 2005, Low-frequency Earth’s normal modes and tsunami
excited by the 2004 Sumatra-Andaman earthquake Observation from the superconducting gravimeters of GGP -,Asian Academic Seminar JASS05, (Nagoya, Japan, Sep. 26Oct. 5).
Sato, T., Boy, J. P., Tamura, Y., Matsumoto, K., Asari, K.,
Plag, H.-P., and Francis, O.: 2005, Gravity tide and seasonal
gravity variation at Ny-Alesund, Svalbard in Arctic, Europian
Geosciences Union General Assembly 2005, (Vienna, Austria,
Apr. 24-29).
Sato, T., Imanishi, Y., Fukuda, Y., Ikeda, H., Tamura, Y., Rosat,
S., and Ohashi, M.: 2005, Cooperative observation ofsuperconducting gravimeters at Kamioka and Matsushiro inJapan, Europian Geosciences Union General Assembly 2005,(Vienna, Austria, Apr. 24-29).
Sato, T., Imanishi, Y., Fukuda, Y., Ikeda, H., Tamura, Y., Rosat,
S., and Ohashi, M.: 2005, Cooperative observation ofsuperconducting gravimeters at Kamioka and Matsushiro inJapan -In the cause of detection of the core oscillation-,
IAG/IAPSO Joint Symposium, Dynamic Planet 2005, (Cairns,
Australia, Aug. 22-26).
Sato, T., Rosat, S., Tamura, Y., and Matsumoto, K.: 2006, An
attempt to improve the estimation accuracy of the atmosphericpressure effect, Joint Workshop on Analysis of GGP Data fromSuperconducting Gravimeters and Earth Deformation
Regarding Geodynamic Signals and Environmental Influences,(Jena, Germany, Mar. 27-31).
Sato, Y.: 2005, Subaru/Suprime-CAM observations of the
UKIDSS DXS fields: ELAIS N1 and Lockman Hole,
Panoramic near-Infrared Astronomy, (UK, Nov. 10-11).
Sato. S., Arai, K., Akutsu, T., and the TAMA collaboration:
2005, Analysis of transfer mechanism of laser noises throughmultiple optical systems, 6th Edoardo Amaldi Conference on
Gravitational Waves, (Okinawa, Japan, June 20-24).
Sawada, T.: 2006, CO J＝3-2 Survey of the Galactic Plane,
Perspective of Submillimeter Astronomy with Atacama
Submillimeter Telescope Experiment (ASTE), (Tokyo, Japan,
Mar. 16-17).
Sekii, T.: 2005, Solar-B SOT helioseismology program, TimeDistance Helioseismology and Helioseismic Holography
Workshop, (Stanford, USA, Aug. 17-19).
Sekii, T.: 2005, On time-distance approch to g-mode detection,
Phoebus Workshop, (Bern, Switzerland, Oct. 31-Nov. 4).
Sekii, T.: 2005, SOT time-distance helioseismology in and around
active regions, The 6th Solar-B Science Meeting, (Kyoto,
Japan, Nov. 8-11).
Sekii, T.: 2006, Local helioseismology at small scales, HMI/AIA
Science Meeting, (Monterey, MA, USA, Feb. 13-17).
Sekimoto, Y., et al.: 2005, Developments for ALMA Band 8 (385
- 500 GHz) Prototype Cartridges, Submillimeter Receiver
Workshop, (Nanjing, China, Dec. 8-10).
Sekimoto, Y., et al.: 2005, Evaluation of 385 - 500 GHz balanced
mixer, Submillimeter Receiver Workshop, (Nanjing, China,
Dec. 8-10).
Shan, W.: 2005, Development of the ALMA band-8 & band-10
WG SIS mixers, Workshop on Submillimeter Astronomy andReciever Technologies / Joint Workshop with the 6thWorkshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nanjing, China, Dec. 8-10).
Shan, W., Asayama, S., Kamikura, M., Noguchi, T., Shi, S.,
74

and Sekimoto, Y.: 2005, Development of a 385 - 500GHz SIS
Mixer for ALMA Band 8, 16th International Symposium onSpace Terahertz Technology, (Göteborg, Sweden, May 2-4).
Shibasaki, K.: 2005, Plasma Diamagnetism and Solar Coronal
Activity, The 6th Solar-B Science Meeting, (Kyoto, Japan,
Nov. 8-11).
Shibasaki, K.: 2005, Hot Plasma Confinement Mechanism at the
Loop Top, 11th European Solar Physics Meeting, (Leuven,Sep. 11-16).
Shibasaki, K.: 2005, Nobeyama Radioheliograph and its Recent
Results, URSI-GA2005, (New Delhi, Oct. 23-29).
Shimojo, M., and SOLAR-B MODA Working Group: 2005,
Archiving, Distribution and Analysis of Solar-B Data, The 6th
Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
Shimojo, M., Tsuneta, S., and SOLAR-B Project/NAOJ: 2005,
The SOLAR-B Science Center in Japan, The 6th Solar-B
Science Meeting, (Kyoto, Japan, Nov. 8-11).
Shirasaki, Y.: 2005, JVO Publishing/Searchable Registry
Implementation Experience, IVOA Interoperability meeting,(Kyoto, Japan, May 16-20).
Shirasaki, Y.: 2005, Common Interface for Astronomical Data
Service, IVOA Interoperability meeting, (Kyoto, Japan, May
16-20).
Shirasaki, Y.: 2005, ADQL WD update, IVOA Interoperability
meeting, (San Lorenzo de El Escorial, Spain, Oct 6-7).
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Mizumoto, Y., Ohishi, M., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.: 2005,
Japanese Virtual Observatory (JVO): implementation of VO
standard protocols, Astronomical Data Analysis Software &Systems 2005, (San Lorenzo de El Escorial, Spain, Oct. 2-5).
Shitov, S.: 2005, Development of the ALMA band-10 QO SIS
mixer, Workshop on Submillimeter Astronomy and Reciever
Technologies / Joint Workshop with the 6th Workshop on
Submillimeter-Wave Receiver Technologies in Eastern Asia,(Nanjing, China, Dec. 8-10).
Shitov, S.: 2006, Development of a SIS receiver for ALMA band10, 4th ESA workshop on Millimetre Wave Technology andApplications, (Espoo, Finland, Feb. 17).
Shitov, S., Noguchi, T., Matsunaga, T., Tamura, T., Uvarov, A.,
Cohn, I., and Hasegawa, T.: 2005, A SIS Mixer for ALMABand 10: Development Concept, 16th International
Symposium on Space Terahertz Technology, (Göteborg,
Sweden, May 2-4).
Skopal, A., Otsuka, M., Tamura, S., Vittone, A., Errico, L., Wolf,
M.: 2005, Broad H-Alpha Wings in Active Symbiotic Stars
The Case of Z Andromedae, 7th Pacific Rim Conference on
Stellar Astrophysics, (Seol, Korea, Nov. 1-5).
Snedden, S. A., et al.: 2005, An SDSS Survey of Galactic
Planetary Nebulae: Target Selection and Preliminary Results,
AAS Meeting 207, (Washington, D.C., USA, Jan. 8-12).
Sôma, M.: 2005, Results from the recent lunar occultations of
upsilon Geminorum and Antares, Journées 2005, Earth
Dynamics and Reference Systems, (Warsaw, Poland, Sep. 1921).
Sôma, M., Tanikawa, K.: 2005, Abrupt changes of the Earth’s
rotation speed in ancient times, Journées 2005, Earth Dynamics
and Reference Systems, (Warsaw, Poland, Sep. 19-21).
Suematsu, Y.: 2005, Solar-B/SOT, STEREO/Solar-B Science
Planning Workshop, (Turtle Bay, Oahu, Hawaii, Nov. 15-18).
Suematsu, Y.: 2005, On the Evaluation of Optical Performace of

Observing Instruments, International Workshop The 6th SolarB Science Meeting, (Kyoto, Japan, Nov. 8-11).
Suematsu, Y., Yatini, C. Y.: 2005, Change in Sunspot Proper
Motion and Its Relation to Flare Onset, International Workshop
The 6th Solar-B Science Meeting, (Kyoto, Japan, Nov. 8-11).
Suematsu, Y., Ichimoto, K., Shimizu, T., Otsubo, M., Nakagiri,M., Noguchi, M., Tamura, T., Katsukawa, Y., Kato, Y.,
Hara, H., Miyashita, M., Tsuneta, S., Kubo, M., Sakamoto,Y., Matsushita, T., Kawaguchi, N., Nakaoji, T., Nagae, K.,
Shimada, S., Takeyama, N., and SOT team: 2005, Optical
Performance of Optical Telescope Assembly of SOT:
Confirmation of Diffraction-Limited Performance,
International Workshop The 6th Solar-B Science Meeting,(Kyoto, Japan, Nov. 8-11).
Sugimoto, M.: 2005, ACA Front-End (7m optics studies), The 6thWorkshop on Submillimeter-Wave Receiver Technologies in
Eastern Asia, (Nanjing, China, Dec. 8-10).
Sugita, S., Kadono, T., Ootusbo, T., Honda, M., Sako, S., Miyata,T., Sakon, I., Yamashita, T., Kawakita, H., Fujiwara, H.,
Fujiyoshi, T., Takato, N., Fuse, T., Subaru/Comics Deep
Impact Observation Team: 2006, A High-Resolution Mid-IR
Observation of the Collision Between Deep Impact Projectile
and Comet 9P/Tempel 1, 37th Annual Lunar and Planetary
Science Conference, (Texas, USA, Mar. 13-17).
Sugiyama, N.: 2006, Constraining the EoR with High resolution
CMB Data, Reionizing The Universe, (Groningen,
Netherlands, June 27-July 1).
Sumiyoshi, K.: 2005, Core-collapse supernovae, r-process
nucleosynthesis, and the physics of unstable nuclei, Second
Joint Meeting of the Nuclear Physics Divisions of the Americal
Physical Society and The Physical Society of Japan, (Maui,
Hawaii, USA, Sep. 18-22).
Sumiyoshi, K., Suzuki, H., and Yamada, S.: 2005, Neutrinonucleus interactions and supernova modeling, 4th International
workshop on neutrino-nucleus interactions in the few-GeV
region (NuInt05), (Okayama, Japan, Sep. 26-29).
Sumiyoshi, K., Suzuki, H., and Yamada, S.: 2005, Fate of corecollapse supernovae: formation of neutron star and black hole,
International Symposium on Origin of Matter and Evolution of
Galaxies (OMEG05) New Horizon of Nuclear Astrophysics
and Cosmology, (Tokyo, Japan, Nov. 8-11).
Suzuki, I., Sakurai, T., and Ichimoto, K.: 2005, Three
Dimensional Motion of Plasmas Associated with Coronal Mass
Ejections Observed with NOrikura Green-line Imaging System(NOGIS), International Workshop The 6th Solar-B Science
Meeting, (Kyoto, Japan, Nov. 8-11).
Takahashi, R.: 2005, Seismic Attenuation System (SAS) for
TAMA, 6th Edoardo Amaldi Conference on Gravitational
Waves, (Okinawa, Japan, June 20-24).
Takahashi, S.: 2006, ASTE mapping observation of Large-scale
Outflow associate with Intermediate-mass Protostars,
Perspective of Submillimeter Astronomy with Atacama
Submillimeter Telescope Experiment (ASTE), (Mitaka, Japan,
Mar. 16-17).
Takakuwa, S.: 2006, ASTE Observations of Low-mass
Protostellar Envelopes, East-Asian Workshop “Evolution of
Molecular Clouds: Recent Observational and Theoretical
Results and Prospects”, (Mitaka, Japan, Feb. 6-8).
Takakuwa, S.: 2006, ASTE Observations of Warm Gas in Lowmass Protostellar Envelopes, Perspective of Submillimeter
Astronomy with Atacama Submillimeter Telescope

Experiment (ASTE), (Mitaka, Japan, Mar. 16-17).
Takano, S.: 2005, Molecular Abundances in Galaxies,
Astrochemistry - From Laboratory Studies to Astronomical
Observations (Pacifichem 2005: Symposium 47), (Hawaii,
USA, Dec. 15-20).
Takano, S.: 2006, Observations of ammonia in galaxies:
Extremely high-velocity motion in Arp220, New Horizons of
Astrochemistry and Laboratory Spectroscopy, (Ibaraki, Mito,
Mar. 15-17).
Takeda, M.: 2005, Mixer development in NICT, Workshop on
Submillimeter Astronomhy and Receiver Technologies,(Nanjing, China, Dec. 8).
Takeda, T., and Ohtsuki, K.: 2005, Angular momentum transfer
in the collision between rubble pile objects, IAU 9th Asian
Pacific Regional Meeting, (NusaDua, Bali, Indonesia, July 2629).
Takeda, T., and Ohtsuki, K.: 2005, Angular momentum transfer
in the collision between rubble pile objects, Protostar andPlanet V, (The Big Island, Hawaii, America, Oct. 24-28).
Tamura, M.: 2005, Subaru Exploration of Exo-Solar Planets andDisks, 40 years of Infrared Astronomy: A Tribute to Eric
Becklin, (Los Angeles, USA, Apr. 1-2).
Tamura, M.: 2005, NIR studies of disks and companions YSOs
using the Subaru telescope, Star Formation Workshop, (Taipei,
Taiwan, Dec. 11-14).
Tamura, M.: 2006, Direct explorations of exoplanets and theirbirth places with Subaru, International Workshop on the 10th
gravitational microlensing and ralated topics, (Nagoya, Japan,
Jan. 16-19).
Tamura, M., Abe, L., and Subaru HiCIAO/SPICA
coronagraph/JTPF teams: 2005, Direct Explorations of
Exoplanets with the Subaru Telescope and Beyond, Direct
Imaging of Exoplanets: Science & Techniques, Proceedings
IAU Colloquium 200, (Villefranche-sur-Mer, France, Oct. 37).
Tamura, N., Sharples, R. M., Arimoto, N., Onodera, M., Ohta,
K., Yamada, Y.: 2006, A Subaru/Suprime-Cam wide-fieldsurvey of globular cluster populations around M87, Globular
Clusters: Guides to Galaxies, (Universidad de Concepcion,
Chile, Mar. 6-10).
Tamura, Y.: 2006, An Application of Non-Linear Harmonic
Analysis Method to the Development of Tidal Potential, Joint
Workshop on Analysis of GGP Data from Superconducting
Gravimeters and Earth Deformation Regarding Geodynamic
Signals and Environmental Influences, (Jena, Germany, Mar.
27-31).
Tanaka, M.: 2005, JVO use of Globus toolkit, IVOAInteroperability meeting, (Kyoto, Japan, May 16-25).
Tanaka, M., Shirasaki, S., Kawanomoto, S., Honda S., Ohishi,M., Mizumoto, Y., Yasuda, N., Ishihara, Y., Tsutsumi, J.,
Nakamoto, H., Kobayashi, Y., Sakamoto, M.: 2005, Web
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Astronomical Data Analysis Software and System XV, (San
Lorenzo de El Escorial, Spain, Oct. 2-5).
Tanaka, S., Nakagawa, T., Kataza, H., Enya, K., Tamura, M.,
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Tatematsu, K.: 2006, ASTE observation of SNR, East-Asian75

Workshop “Evolution of Molecular Clouds: Recent
Observational and Theoretical Results and Prospects”, (Mitaka,
Japan, Feb. 6-8).
Tatematsu, K.: 2006, ALMA, East-Asian Workshop “Evolutionof Molecular Clouds: Recent Observational and Theoretical
Results and Prospects”, (Tokyo, Japan, Feb. 6-8).
Tatematsu, K.: 2006, Observation of Southern SNRs, Perspectiveof Submillimeter Astronomy with Atacama Submillimeter
Telescope Experiment (ASTE), (Tokyo, Japan, Mar. 16-17).
Tatsumi, D.: 2005, Questions posed in the analysis ofgravitational wave detector data, Statistics for Gravitational
Wave Data Analysis, (Penn. State Univ., USA, May 19-21).
Tsujimoto, T.: 2005, Implications of the Mysterios Elemental
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Tsujimoto, T.: 2005, Implications of Elemental Abundances in
Metal-Poor Stars, Carbon-rich Ultra Metal-Poor Stars of the
Galactic Halo, (Ringberg, Germany, Nov. 28-Dec. 2).
Tsujimoto, T.: 2006, Interpretation of Abundance Patterns in
Dwarf Spheroidals, Local Group Cosmology, (Aspen, USA,
Feb. 5-11).
Tsukagoshi, T.: 2006, ASTE observations of proto-planetarydisks, Perspective of Submillimeter Astronomy with Atacama
Submillimeter Telescope Experiment (ASTE), (Tokyo, Japan,
Mar. 16-17).
Tsuneta, S.: 2005, Summary talk I, The 6th Solar-B Science
Meeting, (Kyoto, Japan, Nov. 8-11).
Tucker, D. L., et al.: 2005, The SEGUE Open Cluster Survey,
AAS Meeting 207, (Washington, D.C., USA, Jan. 8-12).
Ujihara, H.: 2005, Development of Film Lens Antennas for Large
Aperture Radio Telescopes, XXVIIIth URSI General
Assembly, (New Delhi, India, Oct. 23-29).
Usuda, T.: 2006, SUBARU Telescope: Overview, SUBARU East
Asia Youth Seminar, (Kona, Hawaii, USA, Mar. 13-17).
Uzawa, Y.: 2005, Band-10 cartridge development, Workshop on
Submillimeter Astronomhy and Receiver Technologies,(Nanjing, China, Dec. 9).
Wada, K.: 2005, Fueling for the nuclei: Starburst-AGN
connection and structure of the ISM, Superunification of
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Wang, Z.: 2005, Current status of NbN technique at NICT for
ALMA band-10 development, Workshop on Submillimeter
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8).
Watanabe, J.: 2005, The connection of meteoroids andcomets:recent progress, AOGS 2nd Annual meeting,(Singapore, June 20-24).
Watanabe, J., Kawakita, H., Honda, M., Ootsubo, T., Fuse, T.,
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Watanabe, J., Sato, M.: 2005, Phoenicids in 1956 revisited,
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Watanabe, J., Sugawara, K.: 2005, Dust tail of Comet 9P/Tempel
1 after the Deep Impact: Prediction, AOGS 2nd Annual
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Watanabe, T.: 2005, The Solar-B Mission, Stereo/Solar-B
76

Science Planning Workshop, (Turtle Bay, Oahu, Hawaii, Nov.
15-18).
Yamada, M.: 2005, Synthetic Observation of Turbulent Flows inInterstellar Medium, Inaugural Japan-Taiwan ALMA Science
Workshop, (Taiwan, Dec. 15-16).
Yamada, M.: 2006, Wideband millimeter-submillimeter wave
source for ALMA telescope calibration, New Horizon of
Astrochemistry and Laboratory Spectroscopy, (Mito, Japan,
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Yamada, T.: 2006, Extended Lya Blobs: Massive Forming
Galaxies I Growing Large-Scale Structures, The Fabulous
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Yamada, T.: 2006, From Subaru To ALMA, Inaugural JapanTaiwan ALMA Science Workshop, (Taiwan, Dec. 15-16).
Yamada, T., Mastdua, Y., Hayashino, T., Yamauchi, R.: 2005,
Lya Blobs: Tracing Formation of Massive Galaxies at HighRedshift, Japanese-German Symposium 2005 “The Formation
and Co-Evolution of Black Holes and Galaxies”, (Regensburg,
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Yamaguchi, N.: 2005, CS 7-6 Observations Towards Southern
Massive Star-Forming Regions with ASTE, Submillimeter
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Yamaguchi, N.: 2006, A Survey of Massive Dense Clumps in theSouthern Sky, Perspective of Submillimeter Astronomy with
Atacama Submillimeter Telescope Experiment (ASTE),(Tokyo, Japan, Mar. 16-17).
Yamaguchi, N.: 2005, A Survey of Massive Dense Cores in theSouthern Sky, Inaugural Japan-Taiwan ALMA Science
Workshop, (Taipei, Taiwan, Dec. 15-16).
Yamamoto, T. T., Sakurai, T., Yokoyama, T., and Kusano, K.:
2005, Helicity Injections in Regions of Various Magnetic
Fluxes, International Workshop The 6th Solar-B Science
Meeting, (Kyoto, Japan, Nov. 8-11).
Yamamoto, T. T., Sakurai, T., Yokoyama, T., Kusano, K., andMaeshiro, T.: 2006, nflow velocities and coronal magnetic fieldstrength estimated from the GOES X-ray light curve, Solar
Activity and its Magnetic Origin, IAU symp. 233, (Cairo,
Egypt, Mar. 31-Apr. 4).
Yamazaki, D. G.: 2005, Constraint of Primordial Magnetic Field
from CMB, the Workshop on Nonlinear Cosmology:
Turbulence and Fields, (Trieste, Italy, May 17-21).
Yamazaki, D. G.: 2005, Constraint of Cosmological Magnetic
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Inflating horizon of particle astrophysics and cosmology,(Tokyo, Japan, June 20-24).
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Cosmic Microwave Background, COSMO 05, (Bonn,
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Yamazaki, D. G.: 2006, Effect of Primordial Magnetic Field on
Large Scale Structure, East Asian Young Astronomers Meeting
2006, (Kiyosato, Japan, Feb. 13-18).
Yonekura, Y.: 2006, High resolution observations of massive-star
forming clumps in the Carina Arm, Perspective of
Submillimeter Astronomy with Atacama Submillimeter
Telescope Experiment (ASTE), (Tokyo, Japan, Mar. 16-17).
Yoshida, F., Dermawan, B., Nakamura, T., Ito, T., Takahashi,
S., Ibrahimov, M. A., Malhotra, R., Ip, W. H., Chen, W. P.:
2005, Photometric observations of Karin family asteroids, IAU
Symposium 229: Asteorids, Comets, Meteors, (Brazil, Aug. 712).

Yoshida, F., Dermawan, B., Nakamura, T., Ito, T., Takahashi,
S., Ibrahimov, M. A., Miyasaka, S., Fukushima, H., Sato, H.,
Yanagisawa, T., Malhotra, R., Ip, W. H., Chen, W. P.: 2005,
Photometric observations of Karin family asteroids, AOGS 2nd
Annual Meeting, (Singapore, June 20-24).
Yoshida, F., Nakamura, T.: 2005, Subaru Main-Belt Asteroids

Survey: SMBAS, AOGS 2nd Annual Meeting, (Singapore,
June 20-24).
Yoshida, M., Kawabata, K. S., and Ohyama Y.: 2005,
Spectropolarimetry of the superwind filaments of the starburst
galaxy M82: Kinematics of the dust outflow, Asian-PacificRegional IAU Meeting 2005, (Bali, Indonesia, July 26-29).

77