Table of Contents

PrefaceI

Norio KAIFU
Director General
National Astronomical Observatory of Japan

Scientific Highlights April 2004 - March 2005 ······················································· 1

II Publications, Presentations····················································································· 55
1. Refereed Publications ························································································ 55
2. Publications of the National Astronomical Observatory of Japan ····················· 67
3. Report of the National Astronomical Observatory of Japan ······························ 67
4. Other Publications······························································································ 67
5. Presentations ······································································································ 75

PREFACE
We present a report of annual achievement of NAOJ
through the FY 2004.
The FY 2004 was a special and memorable year for NAOJ
in many ways. Firstly NAOJ started the construction of
Atakama Large Mm- and submm-wave Array (ALMA) under
the three-party cooperation with European countries (ESO)
and North American consortium. The developments of highprecision antennas, mm- and submm-wave receivers of
Atakama Compact Array (ACA) and other contributions by
Japan for ALMA have started and been going quite well. The
construction of ALMA atop Atakama Plateau, Chile,
continues until 2011. By that time NAOJ prepares theJapanese ALMA Research Center in the NAOJ headquarters
at Mitaka as an active center of East Asian mm- andsubmm-wave astronomy.
Secondly 2004 was the first year of NAOJ as a member ofa newly established inter-university research agency “National Institute of Natural Sciences (NINS)”.
NINS is composed of five inter-university research institutes; NAOJ, National Institute for Fusion
Science, Institute for Molecular Science, National Institute for Basic Biology and National Institutefor Physiological Science which are core institutes in each field of science in Japan, and aims tocreate new sciences by mutual cooperation as well as the powerful promotion of science in eachfield.
Thirdly from 2004 we NAOJ started new operational system based on a set of various projects.
Seven NAOJ observatories and stations under operation like Nobeyama Radio Observatory andSubaru Telescope are re-defined as “C-Project” with clear mission and limited life. ALMA, Solar-B
and gravitational detectors which are in construction phase are defined as “B-Project”. “A-Project” isdefined for promising and possible future project to be developed and 3 projects (Space VLBI,JASMINE and MIRA) were designated as A-Projects. Other four new A-projects (4D2U, Exo-Solar
Planets Search, HOP, and ELT) were examined by review committee and were established in 2005.
The re-organization of all national universities and inter-university research institutes (including
NAOJ) to “agencies” from national organizations was carried out as one of the process of setting
Japanese finances in order and naturally brought some difficulty and risks as well as some extent of
freedom to the universities and research institutes. The future of Japanese science and technology
highly depends on the outcome of this re-organization. Such outcome will not be visible within shortterm especially in the field of science. Therefore we need deep thinking and innovative works toward
bright future of Japanese science under this new system.
Re-organization of NAOJ itself to the new internal operation system was, on the other hand, a self
reform aiming at more effective and conscious style of research in astronomy. We feel that our new
system is generally going well, growing better awareness of mission by project members and clearerplans by project managements. The new employment system gave NAOJ another benefit which
made it possible for us to get skilled staff especially in the field of engineering. The Post Doc system
which had been relatively complicated before was also made simple and clear. We still have,
however, some unnecessary restraints as remnants of the former system and some portions still need
to be improved. We are starting discussion of after-two-year’s review of the effects and outcome of
our new operation system toward 2006.
The NAOJ also achieved superior scientific and development activities in many fields ofastronomy through this fluctuating year 2004. In addition to the ALMA developments mentioned

above, we enjoyed a number of exciting observational results from the 8.2m Subaru telescope in
Hawaii. The VERA system with four 20m antennas under operation over the Japan Islands isapproaching the final goal of extremely high angular resolution to achieve the triangulation
measurements of distance to maser stars through the Milky Way galaxy.
As a new instrument the 10m submm-wave telescope ASTE has started the cutting-edge
observations of molecular clouds and star forming regions on the 4,800m altitude ALMA site. The
space Solar telescope SOLAR-B and the Lunar exploration mission SELENE are in the final phaseof developments under the cooperation with JAXA. All of those scientific and engineering activities
including Hawaii, Nobeyama, Okayama, Mizusawa, Norikura and other projects and three centers
are summarized in this report.

Norio Kaifu
Director General.of NAOJ

I

Scientific Highlights(April 2004-March 2005)

1. New Method of Measuring Phase Characteristics
of Antenna Using Doppler Frequency Measurement Technique·······································································LIU et al.
2. Internal Structure and Librations of the Moon································································································· GUSEV et al.
3. Down-sizing in Galaxy Formation at z∼1 in the Subaru/XMM-Newton Deep Survey ·································KODAMA et al.
4. Fe-bearing crystalline olivine around Vega-like star : material proof for planetesimals? ································ HONDA et al.
5. Flare Ribbon Expansion and Energy Release Rate ······························································································ ASAI et al.
6. Downflow Motions Associated with Impulsive Nonthermal Emissions ······························································ ASAI et al.
7. Global Structures of Optically Thin Black Hole Accretion Flows Obtained
from Direct Magnetohydrodynamic Simulations··················································································MACHIDA et al.
8. Nuclear starbursts in Seyfert 1 and 2 galaxies ······················································································· IMANISHI, WADA
9. A buried AGN in the infrared luminous galaxy NGC 4418 ········································································ IMANISHI et al.
10. Discovery of a Young Brown Dwarf Companion around DH Tau ······································································ ITOH et al.
11. High Resolution Near-Infrared Imaging Polarimetry of HL Tau ····································································· LUCAS et al.
12. Flared Disks and Silicate Emission in Young Brown Dwarfs··································································· MOHANTY et al.
13. SIRIUS Observations of Massive Star Forming Regions: W3 Main and NGC 7538 ·········································· OJHA et al.
14. Solar Polarimetry in the Hα line with a Ferroelectric Liquid Crystal Polarimeter ·············································· HANAOKA
15. Derivation of DEM Distribution using YOHKOH/SXT······················································································· SHIMOJO
16. The Subaru Deep Field: The Optical Imaging Data·············································································· KASHIKAWA et al.
17. Near infrared imaging observations of the N159/N160 complex in the LMC :Large clusters of Herbig Ae/Be stars and sequential cluster formation ··············································· NAKAJIMA et al.
18. JASMINE Simulator···································································································································YAMADA et al.
19. Radio Observations of the Afterglow of GRB 030329 ······················································································ KUNO et al.
20. Stellar Mass dependence of Color Evolution of Galaxies in the HDF-N·········································KAJISAWA, YAMADA
21. Okayama Astrophysical Observatory Project: Toward Clarifying the Originof the Abundance Peculiarities in Planet-Harboring Stars ······································································ TAKEDA et al.
22. CCD Centroiding Experiment for JASMINE (Japan Astrometry Satellite Mission)and ILOM (In-situ Lunar Orientation Measurement)··················································································· YANO et al.
23. VLBI Observations of Narrow Bandwidth Signals from the Spacecraft ·······················································KIKUCHI et al.
24. Determination of the Equation of State of the Universe Using∼0.1Hz Gravitational Wave Detectors··············································································TAKAHASHI, NAKAMURA
25. Effects of Dust in the Photosphere on the Spectral Classificationand Effective Temperature of Brown Dwarfs ····················································································· NAKAJIMA et al.
26. Search for 17µm H2 Pure Rotational Emission from Circumstellar Disks···························································SAKO et al.
27. Detection of a deep 3-µm absorption feature in the spectrum of Amalthea (JV) ··········································· TAKATO et al.
28. Near-Infrared Unidentified-Line Morphology of the Planetary Nebula NGC 7027 ·································· OKUMURA et al.
29. A Subaru Search for Lyα Blobs in and around the Proto-Cluster Region at Redshift z=3.1 ······················· MATSUDA et al.
30. Spiral Structure in the Disk around AB Aur ···························································································FUKAGAWA et al.
31. Reverberation Radius of the Central Dust Hole in NGC 5548································································SUGANUMA et al.
32. Gravitational Waves from Coalescing Supermassive Black Hole Binaries
in a Hierarchical Galaxy Formation Model ································································································ ENOKI et al.
33. The origin of light neutron-capture elements in very metal-poor stars···························································· HONDA et al.
34. The mm-Wave Detection of a Radio Source following the 27 December 2004 Giant Flarefrom SGR 1806-20······························································································································MIYAZAKI et al.
35. Results of Gravitational Wave Search with TAMA300 detector ······························································· FUJIMOTO et al.

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36. Intra-day Variation of Sagittarius A* at mm-Wavelengths ········································································MIYAZAKI et al.
37. Asymmetric Surface Brightness Distribution of Altair Observedwith the Navy Prototype Optical Interferometer························································································ OHISHI et al.
38. The Qualification Model of ALMA Band 8 Cartridge Receiver ······································································ SATOU et al.
39. Cartridge-Type 800 GHz Receiver for the ASTE·····················································································SUGIMOTO et al.
40. Photometric Observations of a Young Family Asteroid (832) Karin ···························································YOSHIDA et al.
41. Evaluation of ALMA 12-m Prototype Antenna·································································································SAITO et al.
42. Detection of New Molecules in a Bright Leonid Fireball ····················································································· ABE et al.
43. Progress and Status of the Development of the Band 4 Cartridge Reciever ···············································ASAYAMA et al.
44. The First Build-up of the Solar-B Flight Models······························································································· HARA et al.
45. Discovery of evidence for the nucleosynthesis processby photodisintegration reactions in supernova explosions ······························································· HAYAKAWA et al.
46. Start of regular geodetic VLBI observations within VERA network ···································································· JIKE et al.
47. Hemispheric Sign Rule of Magnetic Helicity on the Sun ····································································HAGINO, SAKURAI
48. Some Coronal Loops have Cooler Loop-Tops ································································································· SINGH et al.
49. A CME onset observed with Norikura NOGIS coronagraph ···············································································HORI et al.
50. Completion of Solar-B/Optical Telescope Flight Model ········································································· SUEMATSU et al.
51. Generalized Horseshoes in the Standard Mapping ·································································TANIKAWA, YAMAGUCHI
52. Metallic abundances of the 2002 Leonid meteor deduced from visible - ultraviolet spectra·························· KASUGA et al.

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New Method of Measuring Phase Characteristics of Antenna
Using Doppler Frequency Measurement Technique
LIU, Qinghui, TSURUTA, Seiitsu, ASARI, Kazuyoshi, PING, Jinsong, KIKUCHI, Fuyuhiko,
MATSUMOTO, Koji, KAWANO, Nobuyuki(NAOJ)The irregularities in phase characteristics of an antenna
on a spin satellite, such as the relay satellite and the VLBI
satellite of SELENE, create erroneous Doppler frequency
measurements. Precise measurements of antenna phasecharacteristics are thus required. We developed a new technique to measure phase characteristics of antennas [1], thatis different from the conventional range methods. The antenna being tested is rotated at a rate of fsp and its phasecharacteristics are calculated from the harmonic components of fsp during time variations in the Doppler frequency of radio waves emitted from the rotating antenna,
rather than by comparing phase delays as used in conventional techniques. The accuracy of measuring phase characteristics is mainly influenced by the instability of frequency, system noise, and ground echo signals. We thus
used a precise oscillator (H-Maser), and only used the harmonic components of fsp to calculate the phase characteristics, which reduced the influence of system noise. In addition, a parabolic antenna was used as the receiving antenna, which reduced the influence of ground echo signals,
and obviated the need for an anechoic chamber used in conventional techniques.
We applied the proposed method to the patch antennaloaded on the relay satellite of SELENE. The patch antenna was placed on a platform, and rotated clockwise at
a rate of fsp =0.105 Hz around the axis through its geometrical center. A right-handed circularly polarized wave witha frequency in the S-band was transmitted, and received by
the main beam of the parabolic antenna.
Fig. 1(a) plots an example of the spectra for time varitions in the Doppler frequency. The spectra for the harmonics of mfsp , m=1,2...7, were detected, which were causedby irregularities in the phase characteristics of the patch
antenna. Fig. 1(b) plots time variations in the harmonics
of mfsp , which were detected with eight digital band passfilters. The center frequencies of these filters were set tom×0.105 Hz, where m=1,2...8. As we can see, the profiles
during every period Tp =9.5 s were similar. Fig. 1(c) plots
phase characteristics obtained by integrating the time variations in the harmonics of fsp . As we can see in the figure,although they varied over a range of about ±1 degrees, theprofiles of phase variations during every period were very
similar. Fig. 1(d) plots the averaging phase characteristics
Φ(θ) with respect to azimuth angle θ, which were calculated from Fig. 1(c).
We also obtained the three-dimensional phase characteristics of the antenna from the phase characteristics obtained with different elevation angles ψ (Fig. 2). Here, thez-axis shows elevation angle ψ and the x-y plane shows
variations in azimuth angle θ. As we can see from Fig. 2,
the phase characteristics of the antenna were very irregular.
The range of variation in phase characteristics was about±3 degrees for 0◦ < ψ <20◦ , and about ±8 degrees for20◦ < ψ <90◦ . The reasons for this may be because when
ψ is small, radio waves emitted from the entire patch antenna are received almost simultaneously, and phase variations in radio waves are averaged. When ψ is large, only
radio waves emitted from the patch edges facing the receiving antenna are received, and the phases of radio waves
vary for different edges.
The three-dimensional phase characteristics of the antenna were obtained with a root-mean-square error of about
0.5 degrees, which demonstrates the efficacy of the method.

Figure2: Three-dimensional phase characteristics of patch antenna.
Figure1: (a) Spectrum for time variation in Doppler frequency. (b) time
variation in the harmonics of fsp , (c) phase characteristics
obtained by integrating the time variations shown in (b), (d)averaging phase characteristics.

Reference[1] Liu, Q., et al.: 2004, IEEE Trans., Antenna and Propa., 52, 3312.

3

Internal Structure and Librations of the MoonGUSEV, Alexander, KAWANO, Nobuyuki

PETROVA, Natasha(NAOJ)(Kazan University, Russia)

The idea is to detect fine variations in its rotation caused
by a complex stratigraphy of lunar interior, using the highprecision astronomical observations of the lunar rotation in
the forthcoming mission SELENE. An occurrence of additional oscillations in the polar motion of the Moon is oneof manifestations of heterogeneous of a lunar body on its
Eulerian (free) rotation (Fig. 1)[1] .
The first estimations of the lunar Free Core Nutation(FCN) period for a two-layer Moon (rigid mantle/solidcore) have given the value about 140 - 190 years in inertial frame. There are reasons to view the Moon as a threelayer body: solid mantle/fluid outer / solid inner core. As
result, new modes in free rotation appear. The fluid coredoes not share the rotation of the solid mantle: it can only
weakly mimic the precession mantle motion. The resulting
few cm/sec velocity difference at the core-mantle boundary
causes a torque and dissipation energy [2].
For a planet with a solid inner core and a liquid outer
core, there are four rotational normal modes. This numbers
is reduced to two for a planet without inner core, and to one
for a planet without liquid core [3]. For a planetary modelwith three homogeneous ellipsoidal layers the Hamiltonian
analytical method for the calculation of the rotation variations gives magnitudes of these normal mode frequencies:
they depend on a presence and on dimension of the innercore within the outer core, of their dynamical flattening.
All types of modes are result of non-coincidence of rotation axes of mantle, outer and inner core (Fig. 2).
The Chandler Wobble (CW), which is a motion of therotation axis of the Moon around its dynamical figure axisof the Moon around its body. It is the only global rotational mode for completely solid planet. For the Moon it
has a long period 74.6 year in a frame tied to the Moon andis prograde (i.e. in the direction of lunar rotation). Thismode was detected from LLR observation as 3”×8” elliptical component in the oscillation (Williams, 2001).
The Free Core Nutation (FCN), which represents a differential rotation of the liquid core relative to the rotationof the mantle. This mode does exist only if a core is liquid. It has a quasi-diurnal period in a frame connect to theMoon and is retrograde. The lunar FCN would have a long
period in space of about 144 year, if dynamical figure of acore is similar to that of the mantle or about 186 year forcore with ellipticity 4×10−4 .
The Free Inner Core Nutation (FICN), which represents
a differential rotation of the inner core with respect to theouter layers of the Moon. The mode does exist only if thelunar two-layer core contains outer liquid and inner solid
portions. It has a quasi-diurnal period in a frame connect tothe Moon and is prograde. As preliminary estimation show,4

the lunar FICN would have a very long period in space isin the range of 500-600 years for the core’s radius 350 km.
The Inner Core Wobble (ICW), which represents a differential rotation of the figure axis of the lunar core withrespect to the rotation axis of the Moon and is due to theequatorial bulge of the inner core, having an excess of density with respect to the liquid core. This mode does exist
only if there is an ellipsoidal solid inner core within a liquid core in the Moon. It has a long period greater than 100
years for the core’s radius 350 km in a frame tied to theMoon and is prograde.

Figure1: Lunar interior as the result of different kind of observations
and of theoretical modeling.

Figure2: The cross-section of the Moon along the rotational axis, A
and C are momenta of inertia for mantle and core. FOC; Fluid
outer core, SIC; Solid inner core.
References[1] Gusev, A., Kawano, N., Petrova, N.: 2003, A&A Trans., 22, 141–147.
[2] Williams, J. G., Boggs, D., Yoder, Ch., Ratcliff, J., Dickey, J.: 2001,
Geoph. Res., 106, E11, 27933–27968.
[3] Getino, J., Gonzales, A. B., Escapa, A.: 2000, Cel. Mech. and Dyn.
Astr., 76, 1–21.

Down-sizing in Galaxy Formation at z ∼ 1
KODAMA, Tadayuki(NAOJ)The SXDS team
It is known that the galaxy properties depend on massor luminosity as well. Using the SDSS data, [1] and [2]have shown an interesting break mass at 3×1010 M above
which the dominant population is red passively evolving
galaxies, while below that mass the contribution of blue
active galaxies becomes dominant. Morphological mix ofgalaxies is also known to be strongly luminosity (or stellarmass) dependent [3]. It is therefore indicative that the formation of massive galaxies and less massive galaxies arequite different, in the sense that massive and/or early-typegalaxies form early in the Universe, while dwarf and/or
late-type galaxies form later on average or are still formingstars at present day. Such mass dependent star formation
history is referred to as “down-sizing” [4].
Given the down-sizing seen in the local Universe, at highredshifts, we expect to go beyond the formation epoch ofsmall galaxies or towards the early stage of their formation,
as well as to approach the formation epoch of more massive
galaxies. To test this hypothesis, we investigate the galaxy
colours at z ∼ 1 as a function of luminosity (or stellarmass) by utilizing the unique Suprime-Cam imaging dataset (BRi z  ) on the Subaru/XMM-Newton Deep Survey
(SXDS). These data are both sufficiently deep (zAB=25,

Figure1: Field-corrected colour-magnitude diagram for the z ∼ 1galaxies in high density regions in SXDS [6]. The solid line
shows the expected location of colour-magnitude sequence atz ∼ 1 assuming a passive evolution with zform =5 [7]. A
deficit of blue galaxies at the bright/massive end, and a deficitof red galaxies at the faint/less-massive end, are both clearly
identified. The stellar masses are scaled using the Kennicutt’s
IMF [8].

6-10σ) and wide (1.2 deg2 ), which enable us for the firsttime to investigate the photometric properties of statisticalsample of galaxies at z ∼ 1 down to ∼M ∗ +3 with respect
to the passive evolution. We first identify five z ∼ 1 highdensity regions by applying colour cuts at 1.7<R−z  <2.0
and 0.8<i −z  <1.1, which correspond to the colours ofpassively evolving galaxies at z ∼ 1. We then combine
these five regions (amounting to 141 arcmin2 in total) andsubtract off the low density regions at z ∼ 1 sampledfrom the same data-set and scaled to the same area. We
do this subtraction on the colour-magnitude diagram [5]and isolate the z ∼ 1 galaxies in a statistical sense. Thismethod should work since both high and low density regions at z ∼ 1 are expected to have the same amount offoreground/background contaminations.
The field-corrected colour-magnitude diagram thus constructed for z ∼ 1 galaxies in high density regions is shownin Fig. 1. The most striking feature in the galaxy distribution on this diagram is that the galaxies are separated
into two distinct populations, ‘bright+red’ and ‘faint+blue’.
More precisely, we show a deficit of red and faint galaxies
below M ∗ +2 or 1010 M in stellar mass and a lack of blue
massive galaxies above M ∗ −0.5 or 8×1010 M in stellar mass. The down-sizing in star formation is therefore
also seen at high redshift, where star formation in massive
galaxies takes place early in the Universe and is alreadytruncated by z ∼ 1, while almost all of small galaxies arestill forming stars at z ∼ 1 [6], [9], [10]. It is puzzling thatthe galaxy formation takes place in “down-sizing” fashion
as apparently opposed to the currently favoured “bottomup” scenario. It is required to accerelate the formation ofmassive galaxies (both star formation and mass assembly),
and at the same time to delay the formation of small galaxies. Some critical physical mechanisms in galaxy formation may be still missing in the current models. It is interesting to see whether the break luminosity or mass getbrighter with increasing redshift by going even higher redshifts with future wide-field NIR observations.
References[1] Kauffmann, G., et al.: 2003, MNRAS, 341, 54.
[2] Baldry, I. K., et al.: 2004, ApJ, 600, 681.
[3] Treu, T., et al.: 2003, ApJ, 591, 53.
[4] Cowie, L. L., et al.: 1996, AJ, 112, 839.
[5] Kodama, T., Bower, R. G.: 2001, MNRAS, 321, 18.
[6] Kodama, T., et al.: 2004, MNRAS, 350, 1005.
[7] Kodama, T., et al.: 1998, A&A, 334, 99.
[8] Kennicutt, R. C.: 1983, ApJ, 272, 54.
[9] Poggianti, B. M., et al.: 2004, ApJ, 601, 197.
[10] De Lucia, G.: 2004, ApJ, 610, 77.

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Fe-bearing crystalline olivine around Vega-like star:material proof for planetesimals?
HONDA, Mitsuhiko, KATAZA, Hirokazu

OKAMOTO, K. Yoshiko(ISAS/JAXA)(Ibaraki Univ.)

YAMASHITA, Takuya, FUJIYOSHI, Takuya(NAOJ)MIYATA, Takashi, SAKO, Shigeyuki, ITO, Meguru, OKADA, Yoko, SAKON, Itsuki, ONAKA, Takashi(Univ. of Tokyo)
We report Subaru/COMICS spectroscopic observationsof Vega-like stars to investigate dust composition around
Vega-like stars [1].
Vega-like stars are the main-sequence stars with circumstellar dust emission. We obtained the 8-13 µm spectrum of
the Vega-like star HD145263, and found evidence for the
crystalline silicate grains (Fig. 1). This is the second example of crystalline silicate grains around Vega-like stars afterβ Pictoris.
Detailed analysis of the silicate feature of HD145263
indicates that Fe-bearing cyrstalline olivine grains([Fe, Mg]2 SiO4 ) can be present around Vega-like star
HD145263, which are not present in the protoplanetarydisks around T Tauri stars and Herbig Ae/Be stars (seeFig. 1 and Fig. 2). Crystalline silicate in the protoplanetarydisks is supposed to be Mg-rich olivine and pyroxene.
Why can Fe-bering crystalline olivine grains be present
around Vega-like stars?
In fact, Fe-bearing crystalline olivine is ubiquitous in themeteorites. Meteorites are supposed as a fragment of muchlarger parent-body (similar to planetesimals) and haverecords of various processes happened at the early phase of
the solar system formation. From the studies of meteorites,
Fe-bearing crystalline olivine is probably formed throughalteration in the planetesimals, not from condensation ofgas [3]. Therefore, if planetesimals are present around
Vega-like stars and formation of dust through planetesimalcollision occurs, Fe-bearing crystalline olivine grains canbe present around Vega-like stars.
Originally, presence of planetesimals around Vega-likestars is suggested through discussion of grain survival
timescale [4]. Thus presence of Fe-bearing olivine grains
probably originated from planetesimals is consistent withthe planetesimal hypothesis for the origin of dust around
Vega-like star and can be a material proof for the presenceof planetesimals.
References[1] Honda, M., et al.: 2004, ApJ, 610, L49.
[2] Koike, C., et al.: 2003, A&A, 399, 1101.
[3] Krot, A. N., et al.: 2000, Protostars & Planets IV, 1019.
[4] Lagrange, A. –M., et al.: 2000, Protostars & Planets IV, 639.

6

Figure1: 8-13 µm spectra of Vega-like star HD145263 and T Tauri starHen3-600A. The longer wavelength ”shoulder” of the silicate
feature of the Hen 3-600A exhibits at 11.24 µm, while that of
the HD145263 shows 11.44 µm. The presence of Fe-bearing
crystalline olivine can account for this wavelength shift (seealso Fig.2).

Figure2: Absorption spectra of olivine grains measured at laboratory[2]. The feature peak wavelength shifts to longer wavelength
as Fe-content of olivine increases (from the top spectrum tothe bottom one).

Flare Ribbon Expansion and Energy Release Rate
ASAI, Ayumi, SHIMOJO, Masumi

YOKOYAMA, Takaaki(Nobeyama Solar Radio Observatory, NAOJ)(University of Tokyo)

MASUDA, Satoshi KUROKAWA, Hiroki, SHIBATA, Kazunari(Nagoya University)(Kyoto University)

Figure1: Left: An Hα image taken with Sartorius. The overlaid HXR
contour image was obtained by Yohkoh/HXT. Right: A photospheric longitudinal magnetogram obtained by SOHO/MDI.
The white and black colors show the positive and negative
magnetic polarities, respectively.

We have examined the relation between the evolution of
the Hα flare ribbons and the released magnetic energy ina solar flare which occurred on 2001 April 10. See [1] formore details. Where and when does the energy release occur in a solar flare? In addition, how much energy is released? They are very important questions to answer inorder to understand the trigger mechanisms of solar flares.
The magnetic reconnection model has suggested that magnetic field lines successively reconnect in the corona, andcan explain several well-known features of solar flares suchas the growth of flare loops and the formation of the Hα
two-ribbon structures at their footpoints. The Hα flare ribbons are caused by the precipitation of nonthermal particles
and the effect of thermal conduction. As the magnetic fieldlines reconnect, newly reconnected field lines have theirfootpoints further out than those that have already reconnected. Therefore, the apparent separation motion of theflare ribbons is seen (Fig. 1).
Based on the reconnection models, the energy release
rate can be expressed in terms of the coronal magnetic fieldstrength and the inflow velocity into the reconnection region [2]. However, it is very difficult to measure the coronal magnetic field strength and the inflow velocity directly.
Consequently, an indirect method is needed to evaluate theenergy release rate quantitatively by using observable values.
We examined the relation between the expanding motions of the Hα flare ribbons and the magnetic energy released during a flare. We estimated the released magnetic
energy by using the magnetic field strengths at the photospheric level and the separation speed of the flare ribbons, instead of direct coronal values. We used the Hα dataobtained with Sartorius Telescope at Kwasan Observatory,

Figure2: Temporal variations of the physical parameters. From top tobottom: distance between the outer edge of the ribbon and themagnetic neutral line; separation speed of the ribbon; photospheric magnetic field strength at the outer edge of the ribbon;
reconnection rate; Poynting flux; microwave correlation plot
obtained with NoRH; hard X-ray count rate measured with
the Yohkoh/HXT. The enhancements of the estimated reconnection rates and the Poynting fluxes, which are accompaniedby the HXR bursts, are seen.

Kyoto University, and the magnetogram taken with MDI1
onbord SOHO satellite. Then, we compared the variationof the released energy with the temporal and spatial fluctuations in the nonthermal radiation observed in hard X-rays
and microwaves (Fig. 2). Hard X-ray and microwave data
were taken with Yohkoh/HXT2 and Nobeyama Radioheliograph, respectively. Hard X-ray and microwave bursts appear when strong energy releases occur, and the sites of theradiation sources indicate where the energy is released. The
HXR and the nonthermal microwave intensities are thought
to be well correlated with the energy release rate. The
estimated energy release rate well reconstructed the light
curves of the nonthermal emissions. We also found that theestimated energy release rates in the Hα kernels associatedwith the hard X-ray sources are locally large enough to explain the difference between the spatial distribution of theHα kernels and the hard X-ray sources.
References[1] Asai, A., et al.: 2004, ApJ, 611, 557.
[2] Isobe, H., et al.: 2002, ApJ, 566, 528.
1 Michelson Doppler Imager
2 Hard X-ray Telecsope7

Downflow Motions Associated with Impulsive Nonthermal
Emissions
ASAI, Ayumi, SHIMOJO, Masumi(Nobeyama Solar Radio Observatory, NAOJ)

YOKOYAMA, Takaaki

SHIBATA, Kazunari(University of Tokyo)(Kyoto University)

Figure1: Model of the downflows and plasmoid ejections. (a) Many
plasmoids are created inside current sheet (gray region). (b)The current sheet is modified due to some instabilities.

We examined in detail downflow motions above flare
loops observed in the 2002 July 23 flare [1]. The finding of supra-arcade downflow motions (downflows) is oneof the most important results achieved with Yohkoh/SXT1 .
These dark features move sunward from the high corona
with speeds of about 200 km/s [2]. A few temperature
analyses performed on the downflows suggest that they
are “moving voids” which consist of such low density andhigh temperature plasma. These voids are pushed downward because of magnetic reconnection which occurred at
higher altitudes, and therefore, they are thought to be newobservational and morphological evidence of magnetic reconnection. However, there still remain many problems on
downflows. So far, almost all the downflows have been
observed in long duration event flares, and many of themwere observed after the peak times of SXR light curves.
If downflows are really related to magnetic reconnection,
they are expected to be observed even in the impulsive
phase, when magnetic reconnection occurs vigorously. We
have examined in detail the evolution of a big two-ribbon
flare which occurred on 2002 July 23 near◦ the south-east
solar limb. The extreme-ultraviolet (195A) images wereobtained with TRACE2 satellite. They show dark downflow features above the post-flare loops. By using the
TRACE images, with spatial resolution higher than with
Yohkoh/SXT, we found that the downflows are seen not
only in the decay phase, but also in the impulsive and main
phases. Therefore, we concluded that the downflow phenomenon is not specific in the decay phase of a flare as had
been thought.

Figure2: Top left: an EUV image of the flare obtained with TRACE.
The yellow line illustrates the position of the slit. Top right:
time-sequenced EUV (195 Å) images obtained with TRACE
along the slit line. The horizontal axis is time, and the verticalaxis is the space along the slits. Bottom: microwave (17 GHz)and HXR (50 - 100 keV) light curves obtained with NoRH
and RHESSI, respectively.

Moreover, the hard X-ray and the microwave data of
the flare were also obtained with RHESSI3 satellite andNobeyama Radioheliograph, respectively, which allowed
us to examine the relationship between downflows and nonthermal emissions which implies strong energy release. We
found that the times when the downflow motions start to be
seen correspond to those when bursts of nonthermal emissions in hard X-rays and microwave are emitted. This result
implies that the downflow motions occurred when strong
magnetic energy was released, and suggests that they arecorrelated with reconnection outflows. Thus, we have beenable to add a new piece of observational evidence to themodel that downflows are reconnection outflow.
As another piece of observational evidence of reconnection outflows, the X-ray plasmoid ejections have been studied. The observations revealed a close relationship between
plasmoid ejections and HXR emissions. From these results, we suppose that both the downflows and the plasmoid
ejections are reconnection outflows (Fig. 1). Plasmoids are
generated in the current sheet, and are ejected as downward(downflows) and upward (X-ray plasmoid ejections), whenstrong energy releases occur. Therefore, the correlations
between plasmoid ejections, or downflow, and HXR bursts
represent a plasmoid-induced, nonsteady reconnection [3].
References[1] Asai, A., et al.: 2004, ApJ, 605, L77.
[2] McKenzie, D. E., & Hudson, H. S.: 1999, ApJ, 519, L93.
[3] Shibata, K.: 1999, Ap&SS, 264, 129.

1 Soft X-Ray Telescope
2 Transition Region And Coronal Explorer

8

3 Reuven Ramaty High Energy Solar Spectroscopic Imager

Global Structures of Optically Thin Black Hole Accretion Flows
Obtained from Direct Magnetohydrodynamic Simulations
MACHIDA, Mami

NAKAMURA, Kenji MATSUMOTO, Ryoji(Division of Theoretical Astronomy, NAOJ)

Figure1: Comparison between the radial structures obtained by 3D
global MHD simulations (solid curves) and global steadytransonic solution of non-radiative black hole accretion flow
(dashed curves). The surface density (a) and integrated pressure (b) were computed by integrating the quantities in therange 0 < z < (0.4 + 6). The radial velocity (c) andsound speed (d) were averaged in 0 < z < 1.

We compare the global structures of optically thin radiatively inefficient accretion flows obtained by global 3D
magnetohydrodynamics (MHD) simulations with steady,one-dimensional global transonic solutions of black holeaccretion flows assuming α-viscosity [1].
Optically thin advection dominated accretion flows(ADAFs) onto a balck hole have been studied extensively to explain the broad spectrum and activities in the
low/hard state of galactic black hole candidates and in lowluminosity AGNs. In the conventional theory of accretion
disks, the basic equations are derived by assuming stationarity and axisymmetry and assuming constant α-viscosity.
This phenomenological approach was useful to construct
disk models without knowing the exact mechanism of theangular momentum transport. However, we now know thatthe angular momentum of the disk is efficiently transportedby Maxwell stress created by the MHD turbulence driven
by magneto-rotational instability (MRI). Thus we carriedout global 3D MHD suimulations of optically thin blackhole accretion flows and compared the numerical resultswith global steady transonic solutions of optically thin onetemperature ADAFs.
The initial state of our numerical simulation is an equilibrium model of an axisymmetric MHD torus threaded byweak toroidal magnetic fields. As MRI grows, the torus
deforms itself into an accretion disk. Fig. 1 compares theradial structure of the accretion flow obtained by 3D MHD
simulations with the one-temperature steady transonic solution of nonradiative accretion flows. The latter solution is
obtained by taking into account the radial dependence of α
because simulation results indicate that the Maxwell stress(Matsue NCT)

(Chiba Univ.)

Figure2: Correlation between the surface density and the massaccretion rate obtained by global MHD simulations. The red
and green symbols denote the quantities at various times at
 = 2.5 and 5, respectively. The blue and pink line shows
the transonic solution at  = 2.5 and 5, respectively.

depends on the radius, especially near to the centeral blackhole and is approximated by α ∼ exp [1/(2)] − 0.99.
Figs. 1a, 1b, 1c, and 1d show the radial profile of the surface density, vertically integrated pressure, averaged radial
velocity, and averaged sound velocity in the azimuthal direction and in time, respectively. In order to avoid any contamination of coronal plasma, the radial velocity and soundspeed were averaged only near to the equatorial plane. The
solid curves show the simulation results, and the dashedcurves show the steady transonic ADAF solution. The
steady transonic solution approximately coincides with thesimulation results.
In Fig. 2, we plot the correlation of mass accretion rateand surface density obtained from direct global simulations. The symbols show the mass accretion rate and surface density. When the mass accretion rate increases withtime, the surface density becomes larger. The solid curves
show the correlation expected from a steady transonic solution. The relation at  = 2.5 coincides with the transonicsolution, because at this radius almost all the mass (about
99.8%) is accreting toward the central black hole. However, at  = 5.0, the coincidence is less clear because theradial oscillation of the disk is overlaid.
In conclusion, the global structure of the optically thinblack hole aaccretion flows obtained by direct 3D global
MHD simulations agrees fairly well with global steadytransonic solutions of conventional radiatively inefficientaccretion disks unlike the self-similar ADAF solutions
which are often claimed to disagree with 3D global MHD
simulation results.
Reference[1] Machida, M., et al.: 2004, PASJ, 56, 671

9

Nuclear starbursts in Seyfert 1 and 2 galaxies
IMANISHI, Masatoshi(Division of Optical and Infrared Astronomy, NAOJ)

WADA, Keiichi(Division of Theoretical Astronomy, NAOJ)
Seyfert galaxies are the most numerous class of Active
Galactic Nuclei (AGNs) in the local universe, and their nuclear luminosities are believed to be powered by central
mass-accreting supermassive black holes. There are two
types of Seyfert galaxies, type-1 (which show broad opticalemission lines) and type-2 (which do not), but the current
AGN unification paradigm predicts that both types are intrinsically the same, but the central engines of type-2 aremerely obscured by torus-shaped dust and molecular gas(the so-called dusty torus).
Since the dusty torus is rich in molecular gas, it is a plausible site for starbursts to occur. Such nuclear starbursts
have been detected in type-2 Seyferts, but their detection
rate in type-1 Seyferts has been surprisingly lower than
type-2 Seyferts. One possible reason for this differenceis the intrinsic difficulty in finding nuclear starburst signatures in type-1, because of the dilution by strong AGN
emission. However, it is possible that nuclear starbursts
can inflate the torus due to an energy input, and thereby agalaxy with such an inflated torus tends to be observed asa type-2. This modified unification paradigm predicts that
nuclear starbursts are intrinsically stronger in type-2 thanin type-1.
Infrared 3-4 µm slit spectroscopy is a powerful means
to distinguish between these two scenarios. First, the 3.3µm polycyclic aromatic hydrocarbon (PAH) emission feature is detected only in starbursts and not in AGNs, making
its luminosity a good measure of starburst activity. Second,the 3.3 µm PAH emission from starbursts is intrinsicallyso strong that the signatures of even weak starbursts aredetectable in normal (S/N ∼ 20) spectra. Third, dust extinction is much lower than at shorter wavelengths, and so
the absolute magnitudes of starbursts are reasonably quantifiable from the observed 3.3 µm PAH luminosities.
We have obtained infrared 3-4 µm slit spectra of 23 type1 Seyferts in the CfA and 12 µm samples (Fig. 1), and compared them with those of 32 type-2 in the same samples,previously obtained by ourselves [1]. We found the following main conclusions. (1) There is no systematic differencein nuclear starburst luminosities, relative to AGN powers,
between type-1 and -2 Seyferts (Fig. 2). (2) The luminosities of nuclear starburts and AGNs positively correlate inboth type-1 and -2 Seyferts, suggesting the physical connections between these kinds of activity [2].
References[1] Imanishi, M.: 2003, ApJ, 599, 918.
[2] Imanishi, M., and Wada, K.: 2004, ApJ, 617, 214.

10

Figure1: Examples of infrared 3-4 µm spectra of Seyfert 1 nuclei. The
abscissa is observed wavelength in µm, and the ordinate is Fλin 10−15 W m−2 µm−1 . The left source shows a clear 3.3µm PAH emission feature, while the PAH emission feature is
not detected in the right source.

Figure2: The ordinate is the 3.3 µm PAH emission luminosities measured in our slit spectra and reflects the absolute magnitudes
of nuclear starbursts. The abscissa is some luminosities thatare thought to trace AGN powers. (a) IRAS 12 µm luminosities. (b) IRAS 25 µm luminosities. (c) Nuclear N -band(λ =10.5 µm) luminosities (<10 arcsec). (d) Nuclear N band luminosities (1.5 arcsec). (e) Core radio luminosity at
8.4 GHz. In all the plots, there in no systematic difference inthe distribution of Seyfert 1 and 2 galaxies, and statistical correlations are found between the luminosities in the abscissa
and ordinate.

A buried AGN in the infrared luminous galaxy NGC 4418
IMANISHI, Masatoshi(Divison of Optical and Infrared Astronomy, NAOJ)

NAKANISHI, Kouichiro, KUNO, Nario

KOHNO, Kotaro(Nobeyama Radio Observatory)(University of Tokyo)

Infrared luminous galaxies radiate very large luminosities (L > 1011 L ) as infrared dust emission, and thus
possess powerful energy sources hidden behind dust. To
understand these galaxies, it is essential to distinguishwhether the primary energy sources are starbursts or active
galactic nuclei (AGNs).
If powerful AGNs are present and obscured by dust in a
torus geometry, such AGNs are detectable through optical
spectroscopy. However, since the nuclear regions of infrared luminous galaxies are very dusty, putative AGNs inthese galaxies may be obscured by dust along all sightlines.
Such buried AGNs are elusive, but its evaluation is fundamental to understanding the true nature of these galaxies.
To find such buried AGNs, observations at wavelengthsof low dust extinction are clearly necessary. We thus performed near-infrared spectroscopy and millimeter interferometric observations of NGC 4418 [1], an infrared luminous galaxy which has been suspected to contain a buried
AGN.
Our near-infrared K-band (λ = 2 µm) spectrum reveals
strong emission lines of hydrogen molecule (Fig. 1). Theirline ratios are indicative of a thermal origin. Millimeter interferometric observations using the Nobeyama Millimeter Array detected HCN (J=1–0) and HCO+ (J=1–0)
emission lines (Fig. 2, upper). By combining these datawith CO (J=1–0) data in the literature, we found that NGC
4418 shows line ratios typical of AGNs with no detectablestarburst activity (Fig. 2, lower). If an AGN, a strong Xray emitter, is present deeply buried in dust and moleculargas, strong thermal emission lines of hydrogen molecule
are expected, through X-ray heating. Furthermore, arounda buried AGN, X-ray dissociation regions [2] should develop, which is predicted to produce a large HCN(J=1–0)
to HCO+ (J=1–0) line ratio. Our results not only support
the presence a powerful buried AGN in NGC 4418, but also
clearly demonstrates that our method is effective in finding
elusive buried AGNs. We are extending this successful approach to other infrared luminous galaxies.

Figure1: Near infrared K-band spectrum of NGC 4418. Strong emission lines of hydrogen molecule (H2 ) are seen. The equivalent width of H2 1–0 S(1) line is the second largest observed
to date in an external galaxy.

References[1] Imanishi, M., et al.: 2004, AJ, 128, 2037.
[2] Maloney, P. R., et al.: 1996, ApJ, 466, 561.
Figure2: Upper: Millimeter spectrum of NGC 4418 core obtained with
the Nobeyama Millimeter Array. Lower: Line ratios in brightness temperature. NGC 4418 shows line ratios typical of an
AGN-powered galaxy.

11

Discovery of a Young Brown Dwarf Companion around DH Tau
ITOH, Yoichi

HAYASHI, Masahiko, TAMURA, Motohide

TSUJI, Takashi(Kobe University)(NAOJ)(University of Tokyo)

OASA, Yumiko

FUKAGAWA, Misato(Kobe University)(University of Tokyo)

SDPS team
NAOJ, collaborating with Kobe and Tokyo universities
as well as other groups, is currently conducting a systematic survey of young stars in and around the Taurus molecular cloud to seek for circumstellar disks and/or young
low-mass companions. Here we present the detection of ayoung brown dwarf companion, DH Tau B, associated withthe classical T Tauri star DH Tau [1]. Near-infrared coronagraphic observations with CIAO on the Subaru Telescope
have revealed DH Tau B with H∼15 mag located 2. 3 (330AU) away from the primary, DH Tau A (Fig. 1). Comparing its position with a Hubble Space Telescope archive
image, we confirmed that DH Tau A and B share a common proper motion, suggesting that they are physically associated with each other. The near-infrared color of DH
Tau B is consistent with those of young stellar objects. The
near-infrared spectra of DH Tau B (Fig. 2) show deep water
absorption bands, a strong K absorption line, and a moderate Na absorption line. We derived its effective temperature and surface gravity of Teﬀ = 2700-2800 K and logg =4.0±4.5, respectively, by comparing the observed spectrawith synthesized spectra of low-mass objects [2]. The location of DH Tau B on the H-R diagram gives its mass of
40±10 Jupiter masses.

Figure1: CIAO 2.2 micron coronagraph image of DH Tau and its young
brown dwarf companion. The field of view is 10 ×10 .

References[1] Itoh, Y., et al.: 2005, ApJ, 620, 984.
[2] Tsuji, T., et al.: 2004, ApJ, 607, 511.

Figure2: Near-infrared spectra of DH Tau B. Optical broadband fluxes
were measured from the HST archive data.

12

High Resolution Near-Infrared Imaging Polarimetry of HL Tau
LUCAS, P.

FUKAGAWA, Misato

TAMURA, Motohide(University of Hertfordshire)(University of Tokyo)(NAOJ)

CIAO/AO team
Near infrared coronagraph instrument CIAO for the
Subaru telescope is equipped with polarimetric capability [1]. We present high-quality near-infrared imaging polarimetry of HL Tau at 0.4-0.6 arcsec resolution, obtainedwith Subaru/CIAO and UKIRT/IRCAM [2]. HL Tau is atransitional object from a protostar to a T Tauri star [3].
Three-dimensional Monte Carlo modelling with aligned
oblate grains is used to probe the structure of the circumstellar envelope and the magnetic field, as well as the dust
properties. At the J band, the source shows a centrosymmetric pattern dominated by scattered light (Fig. 1). In the
H and K bands, the central source becomes visible and its
polarization appears to be dominated by dichroic extinction, with a position angle inclined by ≈ 40◦ to the disk
axis (Fig. 2). The polarization pattern of the environs onscales up to 200 AU is consistent with the same dichroic
extinction signature superimposed on the centrosymmetricscattering pattern. These data can be modelled with a magnetic field which is twisted on scales from tens to hundredsof AU [4], or alternatively by a field which is globally misaligned with the disk axis.

References[1] Tamura, M., et al.: 2000, SPIE, 4008, 1153.
[2] Lucas, P. W., et al.: 2004, MNRAS, 352, 1347.
[3] Hayashi, M., et al.: 1993, ApJ, 418, L71.
[4] Tamura, M., et al.: 1995, ApJ, 448, 346.

Figure1: (a) CIAO 2.2 micron surface brightness contour and polarization map, and (b) its polarized intensity contour. Contour levels are normalized tounity at the peak. The spatial scale and polarization degree scale are also shown.

13

Flared Disks and Silicate Emissionin Young Brown Dwarfs
MOHANTY, S. JAYAWARDHANA, R. NATTA, A.
(CfA)(Univ. of Tronto)(INAF)FUJIYOSHI, Takuya, TAMURA, Motohide NAVASCUES, D. Barrado y(NAOJ)(INTA)
It has been suggested that there are numerous candidates of young brown dwarfs and even planetary mass objects (aka, sub-brown dwarfs) in nearby star forming regions [1]. How are such very low-mass objects borne?
Are they formed just like solar-mass stars (like T Tauristars)? Are they originally companion objects which aresomehow separated and mass accretion is terminated? Or
are they formed in protoplanetary disks around more massive stars? Given the much lower mass and intrinsic luminosity of brown dwarfs relative to T Tauri stars, the preceding discoveries raise intriguing questions about how thedetailed properties of brown dwarf disks compare to thoseof T Tauri disks. Observations in the mid-infrared, where
optically thick disk emission dominates over the substellar
photosphere, can provide important constraints on the disk
models [2], [3]. We present mid-infrared photometry of
three very young brown dwarfs located in the rho Ophiuchi
star-forming region–GY 5, GY 11, and GY 310–obtainedwith the Subaru 8.2 m telescope [4]. All three sources weredetected at 8.6 and 11.7 µm, confirming the presence ofsignificant mid-infrared excess arising from optically thickdusty disks. The spectral energy distributions of both GY
310 and GY 11 exhibit strong evidence of flared disks; flat
disks can be ruled out for these two brown dwarfs (Fig. 1).
The data for GY 5 show large scatter and are marginallyconsistent with both flared and flat configurations. Inner
holes a few substellar radii in size are indicated in all threecases (and especially in GY 11), in agreement with magnetospheric accretion models. Finally, our 9.7 µm flux for GY
310 implies silicate emission from small grains on the disk
surface. Our results demonstrate that disks around young
substellar objects are analogous to those girdling classicalT Tauri stars and that they exhibit a similar range of disk
geometries and dust properties.

14

Figure1: Observed fluxes and model predictions for GY 310, GY11,
and GY 5 (from top to bottom). The blue circles are from thiswork, and the red circles and the black curve from previous
space observations. The magenta curve shows the predictionof a flared disk model with small grains. The blue curve shows
the prediction of a flared disk model with large grains, and thegreen curve is the SED of a flat blackbody disk. The photospheric flux for the adopted substellar parameters is in yellow.

References[1] Tamura, M., et al.: 1998, Science, 282, 1095.
[2] Natta, A., et al.: 2002, A&A, 393, 597.
[3] Klein, R., et al.: 2003, ApJ, 593, L57.
[4] Mohanty, S., et al.: 2004, ApJ, 609, L33.

SIRIUS Observations of Massive Star Forming Regions:
W3 Main and NGC 7538
OJHA, D. K., TAMURA, Motohide, NAKAJIMA, Yasushi(NAOJ)SIRIUS Star Formation TeamSIRIUS is a simultaneous JHKs camera developed
jointly by Nagoya University, NAOJ, and other institutions,and serves as an excellent tool for studies of star formation.
Here we report near-infrared (JHKs-band simultaneous)observations of two massive star forming regions (SFRs),
W3 Main and NGC 7538 (Fig. 1). A number of new YSO
candidates are found and infrared nebulae associated with
YSOs are detected; some show intricate color variations
and morphology. A several hundreds of low-mass YSOs
are formed with the formation of massive YSOs. Based on
NIR-color classification, we found that each group of these
YSOs shows clearly separate spatial distributions; Class
I-like protostars distribute toward the dense cloud regions
and Class II-like YSOs around or in optical (diffuse) HII

regions [1], [2]. The distribution in NGC 7538 is most
likely to be a signature of sequential star formation process. Other publications from SIRIUS in this school year
include [3], [4], [5], [6], [7].
References[1] Ojha, D. K., et al.: 2004, ApJ, 608, 797.
[2] Ojha, D. K., et al.: 2004, ApJ , 616, 1042.
[3] Baba, D., et al.: 2004, ApJ, 614, 818.
[4] Ita, Y., et al.: 2004, MNRAS, 353, 705.
[5] Nakajima, Y., et al.: 2005, AJ, 129, 776.
[6] Nagayama, T., et al.: 2004, MNRAS, 350, 980.
[7] Nishiyama, S., et al.: 2005, ApJ, 621, L105.

Figure1: <Left> SIRIUS JHKs composite images of W3 Main (top) and NGC 758 (bottom). <Middle> Identifications of main IR sources with radiosources, HII regions, compact HII regions, ultra-compact HII regions, and massive YSOs. <left> Spatial distribution of YSO candidates. Blue
corresponds to Class II sources, green Class I sources, and red embedded res sources (H-Ks>2). Note that their spatial distributions are distinct.

15

Solar Polarimetry in the Hα line with a Ferroelectric Liquid
Crystal Polarimeter
HANAOKA, Yoichiro(Solar Observatory, NAOJ)
The solar polarimetry with chromospheric absorption
lines such as the Hα line is the key to understand– the magnetic field in the chromosphere, which is close to
the corona where the solar active phenomena actually takeplace,– the high-energy particles which are accelerated in flaresand penetrate into the chromosphere.
However, the chromospheric lines show weak polarization
only, and therefore, their detection has been difficult.
The most significant source of errors in the polarization
measurements is the cross-talk caused by the seeing effect.
However, this can be reduced with high-speed polarization
modulation. Therefore, we developed a polarimeter consisting of ferroelectric liquid crystals (FLC) and a highspeed CCD camera, of which the frame-rate is 500–1000
frame s−1 [1]. This polarimeter realized high-speed polarization modulation, and improved the sensitivity of the polarization measurements much. Now the crosstalk due tothe seeing effect is negligible. Fig. 1 shows the FLC polarimeter. We installed it into the Solar Flare Telescope at
Mitaka to observe the polarization in the Hα line.

– The Stokes V/I weakening is observed persistently in thesunspot umbra, though the polarization weakening (or reversal) in umbrae has so far been considered as a transientphenomenon. Our result suggests that the Stokes V/I weakening is caused by the atmospheric structure of the umbral
chromosphere. This is one of the keys to understand theatmospheric structure above sunspots.
– The Stokes signals at the different wavelength offsetsfrom the Hα center correspond to the magnetic fields ofthe different atmospheric layers. The photospheric magnetic field data have been used to study the solar magnetic
field, but they are considered to show only two-dimensional
magnetic information at a specific height. However, chromospheric magnetic field data (and the combination withthe photospheric magnetic field data) have a potential toshow the three-dimensional structure of the solar magnetic
field.

Figure1: The ferroelectric liquid crystal polarimeter for the Solar Flare
Telescope.

With this polarimeter, we can measure the polarization of
the fast varying phenomena such as impulsive flares withthe sensitivity of the order of 0.1 %. In the case of themeasurement of the polarization due to the Zeeman effect,
which changes slowly, the integration realizes the sensitivity of 10−4 , with which we can derive the vector magnetic fields in the chromohsphere. Fig. 2 shows an example of the results of the measurement of the chromosphericmagnetic field. In this figure, region NOAA 0596, whichappeared in 2004 April, is shown. Fig. 2(c) shows a fullStokes map, which corresponds to the vector magnetic mapof the chromosphere. We studied the Stokes V/I data of thisregion, and obtained the following results [2].
16

Figure2: Images of region NOAA 0596 on 2004 April 22. (a–c) Hαimage, Stokes V/I map, and a close-up full-Stokes map of
the sunspot, where the linear polarization signals are shownwith sticks, respectively. All images were taken by the Solar
Flare Telescope. (d) Photospheric magnetogram taken with
the MDI of the SOHO. The squares in panels (b) and (d)shows the area displayed with the different scales to avoid
saturation.
References[1] Hanaoka, Y.: 2004, Solar Phys. 222, 265.
[2] Hanaoka, Y.: 2005, PASJ, 57, 235.

Derivation of DEM Distribution using Yohkoh/SXTSHIMOJO, Masumi(Nobeyama Solar Radio Observatory, NAOJ)

Figure1: The DEM Distribution of the central part of NOAA 6919.
Dash-dot line shows the result of fitting and dashed line shows
the temperature range for the fitting.

The Sun has many mysteries. Among them, why thesolar corona is heated to be so high in temperature is along standing question, and understanding of the coronalheating mechanism is one of the most difficult problems
to be tackled, partly because we do not know yet thermal structures of the solar corona precisely. Using soft Xray images, like those taken by Yohkoh/Soft X-Ray Telescope (SXT)[1], we often derive single temperatures of thecorona by a filter-ratio technique, simply neglecting multithermal structures of the solar corona, namely, its Differential Emission Measure (DEM) distributions.
Usually, we estimate the DEM distributions from EUV
emission lines observed with EUV spectrometer (e.g. [2]),but it is difficult to derive the DEM distribution at higher
temperature range (>2 MK), since the emissivities ofthese EUV lines become weak at these temperatures.
On◦the other hand, soft X-ray lines (∼ 15A) are emitted athigh temperature, but we do not have the instruments thatobserve the soft X-ray spectra and resolve these X-raylines. Strong et al.[3] show the possibility of deriving theDEM distributions between 2 MK and 20 MK from Xray images observed with Yohkoh/SXT using WithbroeSylwester method [4], [5]. In this paper, we derive theDEM distributions from the SXT images of NOAA 6919
by Withbroe-Sylwester method.
Yohkoh/SXT observed NOAA 6919 using 5 X-ray filters from 05:10 UT to 06:06 UT on 18 November, 1992.
The period corresponds to the day time during a spacecraft
revolution. The spatial and time resolutions of the data are
5 arcsec and about 10 second, respectively. No apparent
activity took place around the center of the active region
during the period. We integrated for total of 344 seconds,
and for the area of 150 arcsec × 150 arcsec. Hence, X-ray
photon noises are rather negligibly smaller than the uncer-

Figure2: The DEM distributions obtained from SOHO/CDS and SXT.
Dotted line indicates the DEM distribution of an active region
observed with SOHO/CDS on 9 April, 1996 (Landi & Landini 1996). Dashed line show 100 × DEM distribution from
CDS. Solid line shows the DEM distribution of NOAA 6919
obtained from YOHKOH/SXT data.

tainties in the ionization balance models.
Figure 1 is the result of the calculation. We derive theDEM distribution from 2 MK to 10 MK. The DEM distribution shows a power-law like distribution and the distribution from 2.8 MK to 8.9 MK fits the power-law function
with an index of −4.95 ± 0.25.
In order to compare our result with other results of DEM
analysis, we show the DEM distribution obtained from
SXT and that of SOHO/CDS data (Fig. 2). The DEM distribution from SOHO/CDS data is obtained by Landi &Landini (1998) using the Arcetri method [6]. Discontinuity in active region DEMs might partly come from theinaccuracies of the absolute calibrations of the both instruments and the difference of abundance and ionization balance models. Furthermore, some observations show humps
in the DEM distribution at temperatures of several MK [7],[8]. Therefore, it is not absolutely necessary to shift upwards the DEM obtained by SOHO/CDS, by two ordersof magnitude, to have a continuously declining distribution
above 2 MK.
References[1] Tsuneta, S., et al.: 1991, Solar Phys., 136, 37.
[2] Vernazza, J. E., & Reeves, E. M.: 1978, ApJS., 37, 485.
[3] Strong, K. T., et al.: 1991, Adv. Sp. Res., 11, 73.
[4] Withbroe, G. L.: 1975, Solar Phys., 45, 301.
[5] Sylwester, J., et al.: 1980, Solar Phys., 67, 285.
[6] Landi, E., & Landini, M.: 1997, A & A., 327, 1230.
[7] Brosius, J. W., et al.: 1996, AAS., 28, 880.
[8] Drake, J. J., et al.: 2000, ApJ., 545, 1074.
[9] Shimojo, M.: 2004, ASP Conf. Ser., 325, 313.

17

The Subaru Deep Field: The Optical Imaging Data
KASHIKAWA, Nobunari(Division of Optical and Infrared Astronomy, NAOJ)

Subaru Deep Field team
Deeper and wider-field observations are required to understand the universe from a longer baseline of time andspace. A large galaxy survey is a simple and essential
method in today’s astronomy for this purpose. However, an
unprecedentedly large galaxy survey is made possible onlywith the combination of some distinctive resources, such asa large telescope, a unique and efficient instrument basedon advanced technologies, and a large amount of telescope
time created by the cooperation of many people who appreciate the value of the survey. In particular, such extremely
deep and wide galaxy surveys to collect a statistically robust number of high-z galaxies beyond z =3 are definitely
needed. The previous high-z galaxy surveys are sometimes
not wide enough to overcome the effect of cosmic variancein deriving the universal nature of these high-z populations,or sometimes not deep enough to catch a faint signal fromthese distant populations.
The Subaru Deep Field (SDF) project is a program of
Subaru Observatory to carry out a deep galaxy survey overa blank field as large as 34 × 27 . The program consists ofvery deep multi-band optical imaging, near-infrared imaging for smaller portions of the field, and follow-up optical spectroscopy. The major scientific goals of the project
are to construct large samples of Lyman-break galaxies atz  4 − 5 and Lyman alpha emitters at z  5.7 and 6.6,
and to make detailed studies of these very high-redshift
galaxy populations. In this paper, we describe the opticalimaging observations and data reduction, presenting mosaicked images and object catalogs in seven bandpasses [1].
The optical imaging was made through five broad-band filters, B, V , R, i , z  , and two narrow-band filters, NB816◦◦(λc = 8150A) and NB921 (λc = 9196A) with almost 10
hour integrations for each band. The limiting magnitudes
measured at 3σ on a 2 aperture are B =28.45, V =27.74,
R = 27.80, i = 27.43, z  = 26.62, NB816 = 26.63, and
NB921=26.54 in the AB system (Fig. 1).
The object catalog constructed for each of the sevenbands contains more than 105 objects. The galaxy number counts corrected for detection incompleteness and starcount contributions are found to be consistent with previous results in the literature (Fig. 2). The initial discoveryof two Lyman alpha emitters at z =6.6 on the SDF was reported [2]. Mosaicked images and catalogs of all the bands
have been made open to the public on Oct. 1, 2004 on the
SDF project website at http://soaps.naoj.org/sdf/.

18

Figure1: Completess estimate for our final SDF sample as a functionof the magnitudes.

Figure2: Galaxy number counts in the R-band. The open (red) circles
show the raw number counts from the SDF catalog, filled (red)circles show the galaxy number counts corrected with completeness and subtracted star counts, and other symbols fromthe literature. The solid line shows the predicted star counts of[3]. The error bars shown in the SDF counts are based on thesimple Poisson errors. We have derived the number counts ofgalaxies for all the five broad bands.

References[1] Kashikawa, N., et al.: 2004, PASJ, 56, 1011.
[2] Kodaira, K., et al.: 2003, PASJ, 55, 17.
[3] Robin, A. C., et al.: 2003, A&A, 409, 523.

Near infrared imaging observations of the N159/N160
complex in the LMC : Large clusters of Herbig Ae/Bestars and sequential cluster formation
NAKAJIMA, Yasushi, TAMURA, Motohide, IWATA, Ikuru(Division of Optical and Infrared Astronomy, NAOJ)

NAGATA, Tetsuya, SATO, Shuji, NAGAYAMA, Takahiro, NAGASHIMA, Chie
KATO, Daisuke, KURITA, Mikio, BABA, Daisuke(Department of Astrophysics, Faculty of Sciences, NagoyaUniversity)

SUGITANI, Koji
(Institute of Natural Sciences, Nagoya City University)

ITA, Yoshifusa(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency)

NAKAYA, Hidehiko(Subaru Telescope, NAOJ)

TANABE, Toshihiko(Institute of Astronomy, The University of Tokyo)
The Large Magellanic Cloud (LMC) is one of the ideal
targets for cluster formation studies, because it harbors
large young clusters such as 30 Doradus, and dynamical environments like highly turbulent interstellar medium (e.g.,[1]) and super-shells (e.g., [2]).
We carried out deep near-infrared imaging observationsof the N159/N160 complex star forming region in the Large
Magellanic Cloud (LMC). We observed an area of ∼ 380
arcmin2 (∼ 80,000 pc2 at the distance of the LMC) in theJ, H, and Ks bands. The observations are deep enough todetect down to ∼ 3 M Herbig Ae/Be stars in the LMC.
We discovered a total of 338 and 464 candidates of Herbig Ae/Be and OB stars, respectively, based on the nearinfrared colors and magnitudes. The Herbig Ae/Be starcandidates constitute 10 clusters, while the OB star candidates 13. We discovered an embedded Herbig Ae/Be cluster in the N159E giant molecular cloud (GMC), N159-Y4,
and a Herbig Ae/Be cluster at a north-east tip of the N159S
GMC, N159S-Y1 (Fig. 1). Together with neighboring two
H II regions, the Herbig Ae/Be cluster N159S-Y1 indicates a hint of the beginning of sequential cluster formationin N159S. Spatial distributions of the Herbig Ae/Be andOB clusters, in conjunction with previously known opticalclusters and embedded massive stars, indicate (1) sequential cluster formation within each of the N159 and N160
star forming regions, and (2) large scale sequential cluster formation over the entire observed region from N160
to N159S [4]. Possible triggers for the large scale sequential cluster formation are a supergiant shell SGS19 and an
expanding superbubble. Some Herbig Ae/Be clusters in
the N159/N160 complex are significantly larger in spatial
scale than pre-main sequence clusters of similar age in the
Galaxy. Highly turbulent gas motion in the LMC is probably responsible for forming the large young clusters.

Figure1: Blue and black points denote the Herbig Ae/Be and OB starcandidates, respectively. The solid contours show surface
number density of the stars. The lowest level and the interval are 1 star/(10pc)2 . Dashed contours show 12 CO(1-0) integrated map [3].

References[1] Kim, S., et al.: 1998, ApJ, 503, 674.
[2] Meaburn, J.: 1980, MNRAS, 192, 365.
[3] Johansson, L. E. B., et al.: 1998, A&A, 331, 857.
[4] Nakajima, Y., et al.: 2005, AJ, 129, 776.

19

JASMINE Simulator
YAMADA, Yoshiyuki KUWABARA, Takashi(Kyoto Univ.)(Niigata Univ.)

UEDA, Seiji(The Graduate University for Advanced Studies)

GOUDA, Naoteru, YANO, Taihei(NAOJ)We explain simulation tools in the JASMINE project [1](JASMINE simulator). The JASMINE project stands at thestage where its basic design will be determined in a few
years. Then it is very important to simulate the data stream
generated by astrometric fileds at JASMINE in order tosupport investigations of error budgets, sampling strategy,
data compression, data analysis, scientific performances,
etc. We find that new software technologies, such as Object Oriented (OO)[2] methodologies and Unified Modeling Language (UML) are ideal tools for the simulation system of JASMINE (JASMINE simulator).
The simulation system should include all objects in JASMINE such as observation techniques, models of instruments and bus design, orbit, data transfer, data analysis etc.
in order to resolve all issues which can be expected beforehand and make it easy to cope with some unexpected
problems which might occur during the mission of JASMINE. Furthermore many researchers in various fields including engineering of the bus system should participate
in developing the simulator. Then the simulator include
many objects and furthermore flexibility and interaction isneeded to cope with the objects. On the other hand, calibrations must be protected from unintentional modificationfor each model of the objects. Then we conclude that the
OO methodologies are ideal for demands described abovein the simulator. High maintainability and reusability of theOO approarch is very useful in making the simulator system. At the present time, the framework of the JASMINE
simulator is completed. These new software technologies
are used also in other space astrometry projects, GAIA and

Figure1: UML diagram for JASMINE Simulator Framework.

20

Figure2: Simulated image observed by JASMINE.

SIM, and are recognized to be important in other big science missions.
Programming of such a large software project starts fromabstraction of components. For example,
Galaxy model Sources of lights
Optical system The component which require light as input and provide light as output.
Detector The component which convert light to electric
signals.
Data Processor The component which convert electric
signals to numeric data.
By this abstraction, JASMINE may be considered as aset of components which get information from other component, processing (including diffraction etc.), and provide
information to other component.
Schematic UML diagram of our proto type simulator isshown in Fig. 1 In our implementation of proto type simulator, each components, such as optical systems or detectors are inherited from an abstract class “model”. A class“container” which manages dependnecy graph has the class“model”. The structure ensures extendability of modules.
Simulated image by JASMINE observation is also shownin Fig. 2.
We are now starting collaboration with satellite systemgroup in Univ. of Tokyo and JAXA and constructing individual components.
References[1] Gouda, N., et al.: 2003, SPIE, 4850, 1161.
[2] O’Mullane, W., and Lindegren, L.: 1999, Baltic Astronomy, 8, 57-72.
[3] Yamada, Y., et al.: 2004, Report of the NAOJ, 7 (3, 4), 41.
[4] Yamada, Y.: 2004, IPSJ Magazine, 45 (12), 1234.

Radio Observations of the Afterglow of GRB 030329
KUNO, Nario, NAKAI, Naomasa(Nobeyama Radio Observatory, NAOJ)

SATO, Naoko

NAKANISHI, Hiroyuki(Hokkaido University)(University of Tokyo)

YAMAUCHI, Aya

KAWAI, Nobuyuki(Kyushu University)(Tokyo Institute of Technology/RIKEN)In the fireball model, afterglows of gamma-ray bursts aredescribed by synchrotron radiation from a relativistic blast
wave. Radio observations of the afterglow of gamma-ray
bursts at millimeter wavelengths are very important, since
they can trace the time evolution of the synchrotron spectrum directly, and make it possible to derive physical parameters of gamma-ray bursts.
GRB 030329 is one of the closest events. Its redshift isz = 0.168. The afterglow of GRB 030329 was so brightthat light curves at various frequencies, from X-ray to radio, have been obtained. Furthermore, a connection between the GRB and a supernova was confirmed.
We conducted radio observations of the afterglow of
GRB 030329 at 23.5 GHz, 43 GHz, and 90 GHz with
the Nobeyama 45-m telescope. The light curves show asteep decline after a constant phase (Fig. 1). The difference in the start time of the decline can be seen. Namely,
the decay started earlier at the higher frequency. The time
evolution of the spectrum shows a decay of the peak frequency and the peak flux. These results are qualitatively
consistent with the fireball model. We compared the radio
data with three models (ISM model, wind model, and jet
model). Among the three models, the wind model and thejet model are relatively consistent with the observed data.
Reference[1] Kuno, N., et al.: 2004, PASJ, 56, L1.

Figure1: Light curves of the radio afterglow at (a) 23.5 GHz, (b) 43
GHz, and (c) 90 GHz. The upper limits are 3 σ. The solidlines are the results of a power-law fitting of the decline of thelight curves [F (23.5 GHz) ∝ t−1.38 , F (43 GHz) ∝ t−1.13 ].

21

Stellar Mass dependence of Color Evolution of Galaxies in the
HDF-N
KAJISAWA, Masaru, YAMADA, Toru
(Division of Optical and Infrared Astronomy, NAOJ)

Figure1: Rest U − V color distribution of galaxies in the Hubble Deep Field North as a function of stellar mass. dashed line and dotted line show thefitting results for low-mass (M∗ < 5 × 109 M ) and high-mass (M∗ > 5 × 109 M ) sample at 0.3 < z < 0.7.

Using the very deep Subaru/CISCO imaging data and
HST archival data, we investigated the relation between
the stellar mass and rest-frame color of distant galaxies [1].
Here we report these results briefly.
For the Hubble Deep Field North field, there are very
deep HST WFPC2/NICMOS U, B, V, I, J, H-band data.
In order to study the evolution of the stellar mass and rest
U − V color of field galaxies back to z ∼ 3 and to low
mass limit (∼ 108 − 109 M ), we performed the very deep
(10 hour exposure) K-band imaging with Subaru/CISCO
in this field.
In Fig. 1, we show the rest U − V color distributionof galaxies as a function of stellar mass for each redshift
range. From the figure, it is seen that at z < 2, the highermass galaxies tend to have the redder U − V color atM∗ > 5 × 109 M , while most galaxies show blue color
and there is only weak (or no) correlation between stellar
mass and U − V color at lower-mass region (dashed line
and dotted line in Fig. 1). These results about the stellar
mass dependence of color distribution are consistent withthe results for galaxies in the present universe derived fromthe large surveys such as SDSS [2].
Further, we estimated the degree of evolution of the
U − V color distribution as a function of stellar mass, andfound that the rest-frame U − V color distribution of lowmass galaxies becomes gradually bluer with redshift, while22

the relation between the stellar mass and rest U − V colorof galaxies with M∗ > 5×109 M does not seem to change
significantly.
The blue U − V color of the low-mass galaxies indicatesthat active star formation occurs in these galaxies and that
their average stellar age is relatively young. Since most of
the galaxies with M∗ < 5 × 109 M have such blue U − Vcolors at any redshift between z ∼ 0.3 and z ∼ 2.7, thesegalaxies have a relatively long characteristic timescale ofstar formation (or recurrent star formation activities withshort duty cycle timescale such that these galaxies keep
blue color). Their bluer color of galaxies at higher redshifts indicates that their average stellar age is younger. We
found that the color prediction from the simple constantstar formation rate model with formation redshift of 4 canreproduce the rest U − V color distribution of low-massgalaxies at each redshift relatively well [1].
From these results, we guess that the low-mass galaxies
continue to form stars at relatively constant rate since relatively early epoch (z ∼ 4 or so), while the galaxies withhigh stellar mass have been suppressed their star formation
activities at early evolutionary stage and their average stellar age became higher.
References[1] Kajisawa, M., & Yamada, T.: 2005, ApJ, 618, 91.
[2] Kauffmann, G., et al.: 2003, MNRAS, 341, 54.

Okayama Astrophysical Observatory Project: Toward Clarifying
the Origin of the Abundance Peculiarities in Planet-Harboring
Stars
TAKEDA, Yoichi, AOKI, Wako, ANDO, Hiroyasu, IZUMIURA, Hideyuki
KAWANOMOTO, Satoshi, SATO, Bun’ei, HONDA, Satoshi, MASUDA, Seiji
MIYAMA, Shoken, WATANABE, Etsuji, YANAGISAWA, Kenji(NAOJ)KAMBE, Eiji

OHKUBO, Michiko, YASAKA, Yoshiro(National Defense Academy)(Kyoto University)

TAKADA-HIDAI, Masahide

SADAKANE, Kozo

(Tokai University)(Osaka-Kyoiku University)

The project “Spectroscopic Study of Planet-Harboring
and Related Stars (PI: Y. Takeda)” was carried out in 2000–
2003 at Okayama Astrophysical Observatory by using the
new HIgh-Dispersion Echelle Spectrograph (HIDES), withaims of confirming the existence of abundance peculiarity (e.g., metal-rich tendency) reported for planet-harboringstars and clarifying its origin.
In carrying out this project, we paid special attention to(1) observing a sufficient number of non-planet-harboringstars to be used as standard stars, and (2) realizing the highprecision determination of relative abundances, in view ofthe fact that delicate abundance differences are involved
with this problem. We eventually obtained high-dispersion
specra of 160 stars (including ∼ 30 planet-harboring stars)
in three specral regions of green–yellow, red, and nearIR. These data were made open to the public at the ftp
site [1] of the Astronomical Data Center, NAOJ, in orderto provide anyone an opportunity to use our data as reference standards [2]. In addition, the atmospheric parameters (Teﬀ , log g, vt , [Fe/H]) of these 160 program stars
were spectroscopically determined by using the equivalent
widths of Fe I and Fe II lines, and discussed in detail incomparison with the published values in the literature [3].
Based on these data, several studies related to thephotospheric abundances of planet-host stars were carriedout with successful results described as follows:— It was confirmed that stars with planets tend to be metalrich (though not a few exceptions exist) compared to those
without planets [3].
— A detailed investigation on the photospheric lithium
abundances revealed that a difference is observed between
planet-harboring and non-planet-harboring stars only in the
narrow Teﬀ region of 5800–5900 K, in the sense that Li
tends to be deficient in the former compared to the latter.
This implies that some mechanism of reducing the photospheric Li, which is related to the existence of planets, may
have acted in this narrow “transition” region where the Liabundance shows a large dispersion and thus may be sensitive to any external effect [4].
— We carried out an extensive abundance study on the representative volatile elements, C, N, and O, and found thatthe abundance ratios of these elements with respect to Fe(the representative of refractory metals) are essentially indiscernible between planet-host stars and non-planet-hoststars. This conclusion may lend support to the “primordial” interpretation (i.e., planet-harboring stars tend to form
more easily from comparatively metal-rich gas), rather thanthe hypothesis of “acquired”characteristics due to the mixing of solid planetesimals (self-enrichment), as the expla-

nation for the origin of their metal-rich tendency [5].
— With the help of a newly developed efficient method forestablishing the differential parameters between two similar stars with very high accuracies, the differences between
the two components (A and B) of 16 Cyg were studied indetail, where B is known to harbor a planet while A is not.
It was then found that the [Fe/H] values in these two components are essentially the same to a precision of within
0.01 dex. This conclusion contradicts the recent report of
the USA group, who claimed the detection of a small but
significant difference of 0.03 dex in favor of the “acquired”
hypothesis (see above)[6].
After the completion of the project mentioned above,
another new OAO project “Search for Extrasolar Planets around G-giant Stars (PI: B. Sato)” started since2004, which aims at detecting planets by monitoringradial-velocities of evolved G-giant stars with an ultimate purpose of studying the planet-formation mechanism
around intermediate-mass stars [7]. This project has already yielded a successful result of detecting a new planetharboring G-giant HD 104985. Since it will become an
important task in the near future to discuss the abundance
characteristics of planet-harboring G-giants, we carried out
an extensive abundance study on 57 G-giants (the first sample of the monitoring targets), and found the following results [8].
(i) The abundances of C, O, Na show appreciable signsof anomaly presumably caused by mixing of the dredgedup H-burning products, and thus are not adequate for discussing the primordial compositions.
(ii) The abundance of Fe tends to be slightly subsolar on
the average. Since this tendency is typically seen for stars
which were A-type main-sequence stars in the past, there
is a possibility that these stars might have been metal-poor
λ Boo stars while a part of their abundance anomaly stillretained without being completely erased.
References[1] ftp://dbc.nao.ac.jp/DBC/ADACnew/J/other/PASJ/57.13/.
[2] Takeda, Y., et al.: 2005, PASJ, 57, 13.
[3] Takeda, Y., et al.: 2005, PASJ, 57, 27.
[4] Takeda, Y., and Kawanomoto, S.: 2005, PASJ, 57, 45.
[5] Takeda, Y., and Honda, S.: 2005, PASJ, 57, 65.
[6] Takeda, Y.: 2005, PASJ, 57, 83.
[7] Sato, B., et al.: 2005, PASJ, 57, 97.
[8] Takeda, Y., et al.: 2005, PASJ, 57, 109.

23

CCD Centroiding Experiment for JASMINE (Japan Astrometry
Satellite Mission) and ILOM (In-situ Lunar Orientation
Measurement)
YANO, Taihei, GOUDA, Naoteru, KOBAYASHI, Yukiyasu, TSUJIMOTO, Takuji
NAKAJIMA, Tadashi, HANADA, Hideo, KAN-YA, Yukitoshi(NAOJ)YAMADA, Yoshiyuki(Kyoto Univ.)

ARAKI, Hiroshi, TAZAWA, Seiichi, ASARI, Kazuyoshi
TSURUTA, Seiitsu, KAWANO, Nobuyuki(NAOJ)INTRODUCTIONJASMINE and ILOM are space missions which are in
progress at the National Astronomical Observatory ofJapan. JASMINE will measure trigonometric parallaxes,
positions and proper motions of stars with the precision of
10 microarcsec in order to obtain more accurate data than
we have ever had. ILOM will also measure the positions ofstars in order to obtain the lunar physical libration and thefree librations directly from the lunar surface. Both projects
use a common astrometric technique to obtain precise positions of stars. In order to accomplish this aim, we must
determine the accurate center of star images on the detector. In order to determine the centers of stars, an imageof the point source must be focused onto the CCD arraywith a spread of a few pixels. The distribution of photons(photoelectrons) over a set of pixels enables us to estimate
positions of stars with accuracy of sub-pixel. We modify
the algorithm to estimate the real positions of stars fromthe photon weighted mean, which is originally developedby the FAME (Full-Sky Astrometric Mapping Explorer)group. Then we experiment whether we obtain the subpixel accuracy of positions of stars by using our algorithm[1].
ALGORITHM
In order to estimate the precise distance of two point
sources in image frames to sub-pixel accuracy, the following algorithm is proposed. Here, we show the algorithm
used in this experiment. Before the analysis, each image
frame is bias subtracted and flat fielded.
First of all, we pick up two stars to measure the distance.
Next we seek the pixel in which a number of photons is
maximum in each star. Then we pick up a square subset of
5 × 5 pixels around the peak pixel of each star image. Accordingly, the number of photons is the maximum values atthe center of pixels in both two stars. Only the pixel valuesof the two subsets are used to measure the distance of the24

two stars. We calculate the photon weighted mean of eachstar.
The photon weighted means (xc , yc ) are different fromthe real positions (xa , ya ). Here, we assume that the difference between the photon weighted mean and the real position is proportional to the deviation of the photon weighted
mean from the center of the pixel.
xa − xc = kxc ,(1)

where k is a coefficient for the correction of the position ofa star.
We calculate parameters, k, by using the least square
method. Then we obtain the real position xa from the estimated parameter, k.
RESULTS
We have taken twenty image frames by sliding the CCD
array. The interval of sliding is 1µm, that is, twenty steps
correspond to 1 pixel. From these twenty image frames, weestimate the distance of two stars, star1 and star2, using thealgorithm shown above. An image of the point spread function (PSF) of a star is focused onto the CCD array with aspread of about three pixels using our equipment. According to the results from the experiment, the variance of theestimated distances of two stars is about 1/300 pixel, thatis, the error of the estimation is 1/300 pixel for one measurement, which is almost ideal one given by the Poissonnoise of photons.
We also investigate accuracy of estimation with a different size of PSF, using a different lens system. An image
size of the PSF is about 1 pixels. In this case also, the accuracy of estimation is about 1/300 pixel.
Reference[1] Yano, T., et al.: 2004, A&A, 116, 667.

VLBI Observations of Narrow Bandwidth Signals
from the Spacecraft
KIKUCHI, Fuyuhiko

KONO, Yusuke(Graduate University for Advanced Studies/NAOJ)(Space VLBI Promotion Office, NAOJ)

LIU, Qinghui, MATSUMOTO, Koji, ASARI, Kazuyoshi, TSURUTA, Seiitsu,
HANADA, Hideo, KAWANO, Nobuyuki(Mizusawa Observatory, NAOJ)

PING, Jinsong(Shanghai Astronomical Observatory, Chinese Academy of Sciences)

YOSHIKAWA, Makoto, MURATA, Yasuhiro(Institute of Space and Astronautical Science,Japan Aerospace Exploration Agency)

SEKIDO, Mamoru(Kashima Space Reserch Center, National Institute of Information and Communications Technology)

OHNISHI, Masafumi(Fujitsu Limited)

Figure1: The residual fringe phases of the main carrier wave and two
range tones for USUDA-KASHIMA baseline.

Gravity measurement of the Moon is one of the methods
to know the internal structure, and gravity field has been
investigated by Doppler measurement. However, the gravity field of the rim of the Moon was not clearly investigated like the near side because the Doppler measurement
is only sensitive to the direction of the line of sight (LOS).
In contrast, VLBI measurement is sensitive to the direction perpendicular to LOS. So, we apply VLBI (very long
baseline interferometry) technique in VRAD (the differential VLBI Radio sources) mission of Japanese lunar exploration project SELENE (SELenological and ENgineering
Explorer) in addition to a conventional 2-way Doppler andnewly applied 4-way Doppler measurement. In association with this plan, we have developed a narrow bandwidth
sampling and recording system for VLBI and a correlation
software and conducted VLBI observation of Japanese explorer Nozomi to confirm the performance and capabilityof these system and software. The VLBI stations involvedin this observation were USUDA, KASHIMA, and MIZUSAWA. In ranging mode, Nozomi transmitted a main carrier wave and two range tones with frequencies of 515kHz
apart from that of the main carrier. So we record these threesignals for group delay analysis.
As a result of software correlation, the residual fringe
phases (RFP) of the main carrier wave in each baseline
were continuously obtained at every 1.3 seconds as shownin Fig.1. In contrast, the RFP of two range tones were obtained only for the USUDA-KASHIMA baseline because
their SNR were far less than that of the main carrier wave.
The SNR of range tones were also decreased when the ambiguity tones were added to the downlink signal, and the
RFP were not obtained during this period (A in Fig. 1).
Therefore the group delay analysis could only be carriedout during the period B in Fig. 1.

Figure2: The difference between the geometric delays in this VLBI observation and those calculated from the orbital motion estimated from the range and Doppler measurements.

Figure 2 shows the difference between the geometric delays derived by the group delay analysis and the geometric delays determined by the range and Doppler measurements. The RMS of them is 13 nsec. This result is inconsistency with the error expected from the SNR of therange tone, which is 19 for 40 seconds integration in average. From this results, it could be expected that if the SNRof the range tones are as large as the main carrier wave andthe frequency intervals are 20MHz, the accuracy of the position of Nozomi would be improved to be less than 1.4
km. This accuracy would satisfy the requirement of the orbit determination of the spacecraft (s/c).
We suppose the feasibility of the VRAD from the resultof Nozomi considering the C/N of each observation. In
VRAD, three carrier waves in S-band and one in X-band
will be received to obtain the precise phase delay. In order to obtain the phase delay without the cycle ambiguity,
the phase error of the RFP are required to be less than 4.3
degrees. From the result of this observation, the requirement of VRAD would be achieved by integrating the RFP
for 12 seconds. This result indicates that the position of thes/c around the Moon will be determined within an error of
20cm.
These result reveal a capability of precise threedimensional positioning of an s/c and give us a new possibility for next deep space mission.
References[1] Kikuchi, F., et al.: 2004, Earth Planets Space, 56, 1041.

25

Determination of the Equation of State of the Universe Using ∼ 0.1
Hz Gravitational Wave Detectors
TAKAHASHI, Ryuichi

NAKAMURA, Takashi(NAOJ)(Kyoto University)

Figure1: Sensitivity of DECIGO/BBO.

Laser interferometers have begun to search for astrophysical gravitational wave sources over a broad frequency
band. For the higher frequency band 10 − 103 Hz, groundbased interferometers such as LIGO, TAMA are currently
in operation. For the lower frequency band 10−4 − 10−1
Hz, the space-based interferometer LISA (the Laser Interferometer Space Antenna) should be launched around2014. To fill the frequency gap for the range 10−2 − 10
Hz between the frequency of the ground-based detectors
and LISA, a space-based decihertz laser interferometer isplanned to be constructed sometime around 2020. Thisdetector is called the DECIGO (DECihertz Interferometer
Gravitational wave Observatory) by the Japanese group [1]and the BBO (Big Bang Observer) in the NASA SEU 2003
Roadmap “Beyond Einstein.”
The major scientific objectives of the decihertz antenna
are as follows: (i) To observe the primordial gravitational
wave background. (ii) To detect ∼ 105 chirp signals of coalescing binary neutron stars and stellar mass black holes
per year. By analyzing the signals from these binaries atcosmological distances, it may be possible to determine theexpansion rate of the universe and the equation of state fordark energy [1]. (iii) To observe the merger of intermediate
mass black holes (102 − 105 M ), which would be helpful
to understand the formation and growth history of supermassive black holes. In this report, we discuss the second
objective, i.e. the determination of the expansion rate of theuniverse using a decihertz gravitational wave detector [2].
We plot the sensitivity of the practical DECIGO andBBO in Fig. 1. We also plot that of LIGO II (or LCGT).
The sensitivity of the ultimate DECIGO is 1000 times better than that of the practical DECIGO (h ∼ 10−27 at
f = 0.1 Hz), which is determined by the quantum limit
26

Figure2: The acceleration parameter X(z) as a function of the redshift. The solid curve represents the case of ΛCDM cosmology (H0 = 75 km/sec/Mpc, Ωm = 1 − ΩΛ = 0.3).
The filled circles and the error bars indicate the mean valuesof X(z) and the estimation errors (1σ) for NS/NS binaries(M1 = M2 = 1.4M ) in bins of width ∆z = 0.1 bins.

sensitivity [1]. Here, we use the sensitivity curve of theultimate DECIGO. We consider NS/NS binaries (M1 =
M2 = 1.4M ) at a redshift z as the gravitational wave
sources. We assume a 1 yr observation before the coalescence.
The acceleration parameter X(z) is defined by [1]


1
H(z)
X(z) =
H0 −
,
(2)
2
1+z
where H(z) is the Hubble parameter at z. We compute theestimation error for X(z) for z = 0 − 2. Fig. 2 displays theacceleration parameter X(z) as a function of z. The solid
curve represents the case of ΛCDM cosmology (H0 = 75
km/sec/Mpc, Ωm = 1 − ΩΛ = 0.3). The filled circles andthe error bars indicate the mean values of X(z) and the estimation errors (1σ) for bins of width ∆z = 0.1. Thus, thecosmic acceleration rate for z = 0−2 would be directly determined by a 1 yr observation with the ultimate DECIGO.
We also found that a ten year operation of the ultimate DECIGO could determine the cosmic equation of state with
0.06% accuracies, while a one year operation could do sowith 3% accuracies.
References[1] Seto, N., et al.: 2001, Phys. Rev. Lett., 87, 221103.
[2] Takahashi, R., and Nakamura, T.: 2005, Prog. Theor. Phys., 113, 63.

Effects of Dust in the Photosphere on the Spectral Classificationand Effective Temperature of Brown Dwarfs
NAKAJIMA, Tadashi

TSUJI, Takashi(NAOJ)(IoA, Univ. of Tokyo)

YANAGISAWA, Kenshi(Okayama Astrophysical Observatory)
We report the results of near-infrared spectroscopy ofbrown dwarfs using Subaru [1], and their interpretation [2].
[1]. We have obtained near-infrared spectra of L dwarfs,
L-T transition objects, and T dwarfs using the Subaru telescope. The resulting spectra are examined in detail to study
their dependence on spectral types. One question is where
the methane feature appears: we suggest that it appears
at L8 and marginally at L6.5. We have obtained bolometric luminosities of the objects with known parallaxes inour sample, first by integrating the spectra between 0.85
and 2.5 µm, and second by the K-band bolometric correction. The bolometric luminosities obtained by both methods agree well, and this implies that the K-band bolometric correction, which is obtained using the Unified Cloudy
Models (UCMs)[2], can be applied to obtain the bolometric luminosities and effective temperatures of the L and T
dwarfs with known parallaxes in the literature. The relation between the effective temperature and spectral type derived from the K-band bolometric correction shows monotonic behavior throughout the L-T sequence. However wealso noticed that the effective temperature does not changemuch between L6 and T5 (Fig.1). This indicates that thebrown dwarf spectra are not characterized by a single parameter, effective temperature.
[2]. We report an attempt to interpret the spectra of L andT dwarfs with the use of the UCM. For this purpose, we
extend the grid of the UCMs to cases of log g = 4.5 and5.5. The dust column density relative to the gas column
density in the observable photosphere is larger at higher
gravities, and molecular line intensity is generally smaller
at higher gravities. The overall spectral energy distribution(SEDs) are fJ < fH < fK in middle and late L dwarfs,
fJ < fH > fK in early T dwarfs (L-T transition objects),
and finally, fJ > fH > fK in middle and late T dwarfs,
where fJ , fH and fK are the peak fluxes at J, H, and K
bands, respectively in fν units. This tendency is the opposite of what is expected for the temperature effect, but it canbe accounted for as the effect of thin dust clouds formed

deep in the photosphere together with the effect of thegaseous opacities, including H2 (collision induced absorption), H2 O, CH4 , and K I. Although the UCMs are semiempirical models based on a simple assumption that thin dust
clouds form in the region of Tcr ≤ T ≤ Tcond (T ≈ 1800K
is only an empirical parameter, while Tcond ≈ 2000K isfixed by the thermodynamic data), the major observations,
including the overall SEDs and the strengths of the major
spectral features, are consistently accounted for throughout
L and T dwarfs. In view of the formidable complexities of
the cloud formation, we hope that our UCM can be of someuse as a guide for future modeling of ultracool dwarfs andfor interpretation of observed data of L and T dwarfs.

Figure1: Relation between spectral type and effective temperature.
There exists a region between L6 and T5, where the effective
temperature does not change much despite the drastic changeof spectra. This implies that the effective temperature alone is
not enough as an atmospheric parameter to specify the spectral type [1]. In order to interpret this behavior, the criticaltemperature, Tcr , which specifies the thickness of the dust
layer in the photosphere, needs to be introduced [2].

References[1] Nakajima, T., et al.: 2004, ApJ, 607, 499.
[2] Tsuji, T., et al.: 2004, ApJ, 607, 511.

27

Search for 17µm H2 Pure Rotational Emission from Circumstellar
Disks
SAKO, Shigeyuki, MIYATA, Takashi

YAMASHITA, Takuya, FUJIYOSHI, Takuya(Institute of Astronomy, The University of Tokyo)(Subaru telescope, NAOJ)

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

OKAMOTO, K. Yoshiko(Institute of Astrophysics and Planetary Sciences, Ibaraki University)

ONAKA, Takashi(Department of Astronomy, The University of Tokyo)
We report spectroscopic observations of a pure rotationalemission of molecular hydrogen carried out by the Subaru
mid-infrared camera and spectrometer COMICS [1].
Studies of circumstellar disks around young stellar objects are important for the understanding of the formationof stars and planets. The presence of giant gaseous planets, which were recently found in some planet surveys, requires a substantial amount of gas in the disk to remain
until their cores become massive enough to retain the atmosphere. The survival time of the gaseous component is
one of the key issues for the planet formation.
Pure rotational line emission of H2 at 17.035 µm is radiated from warm gas at T > 150 K. Since such warm gas islocated at radii of < a few AU from the central star, the H2pure rotational line emission is a good tracer of the warm
gas in the inner region of the disk and an appropriate tool
to focus on the gaseous component in the inner disk region
where gaseous planets are formed. However, fluxes of thepure rotational line emissions are generally very weak because of prohibition of the dipole transition.

Figure1: (solid lines) COMICS spectra of four young stars around theH2 S(1) line at 17.035µm. (dotted lines) Line profiles obtained by the COMICS with a velocity resolution of 60 km
s−1 , when the widths of the emission lines from the objects
are sufficiently narrower than the resolution. Integrated fluxesof these line profiles correspond to those of the H2 S(1) line
emissions detected by the ISO [2].

28

Figure2: Schematic view of the flared passive disk model [3]. The
warm region in the surface layer is extended to radii larger
than that of the interior layer.

Detection of the pure rotational emissions toward the directions of 11 young stellar objects with the Infrared Space
Observatory (ISO) was reported by [2]. However, the beam
size of the ISO is much larger than the disk sizes of theirtargets. Thus, the fluxes measured by the ISO could containthe emission from extended components around the youngstars.
We carried out spectroscopy observations for the S(1)emission of molecular hydrogen toward disks aroundyoung stars, HD 163296, MWC 863, CQ Tau, and LkCa
15, for which the ISO observations detected the S(1)emission. The spectra were obtained with the COMICS
with the spectral resolution of ∆v ∼ 60 km s−1 on the
Subaru telescope.
The S(1) emissions of the molecular hydrogen were notdetected toward any stars of the present targets (Fig. 1).
The present beam size corresponds to a disk radius of 30 to
45 AU at the distances to the objects. If the S(1) emission
detected by the ISO was arising from the disk region, we
should have certainly obtained line profiles in the present
higher sensitivity observations. Thus, it can be concluded
that the H2 S(1) emissions detected by the ISO do not comefrom the region within the typical disk sizes for all the objects observed in the present study and are not directly related to the disk mass.
The upper limits of the disk masses estimated fromthe present observations are significantly lower than thewarm molecular hydrogen mass predicted by the passive
disk model of [3] (Fig. 2), suggesting that the opticallythick emission from dust dominates in the radiation fromthe disks in the mid-infrared wavelength.
References[1] Sako, S., et al.: 2005, ApJ, 620, 347.
[2] Thi, W. F., et al.: 2001, ApJ, 561,1074.
[3] Chiang, E. I., & Goldreich, P.: 1997, ApJ, 490, 368.

Detection of a deep 3-µm absorption feature in the spectrum of
Amalthea (JV)TAKATO, Naruhisa(Graduate University for Advanced Studies/Subaru Telescope, NAOJ)TERADA, Hiroshi, PYO, Tae-Soo(Subaru Telescope, NAOJ)

KOBAYASHI, Naoto

BUS, S.

(University of Tokyo)(University of Hawaii)

In addition to the Galilean moons, Jupiter has two othertypes of satellites: four small inner moons orbiting Jupiterwithin the orbit of Io, the inner most Galilean satellite, andat least fifty five small outer moons outside the orbit of Callisto, the outer most Galilean satellite. All the outer satellites have orbits that reveal that they must have been captured by Jupiter during or after the formation of the planet.
The origin of the four small inner moons remain a mystery, however. They have orbits compatible with the hypothesis that they formed in orbit around Jupiter like theGalilean moons. On the other hand, their small irregular shapes and their comparatively low reflectivity and low
densities resemble asteroids and suggest that they were
captured by Jupiter’s gravitational pull just like the outermoons.
We had obtained the first infrared spectrum of two of
Jupiter’s small inner moons, Amalthea and Thebe [1]. To
obtain a spectrum over a wide range of infrared wavelengths, we used two instruments on two telescopes. For
high resolution spectroscopy at wavelengths longer than
3 µm, the Infrared Camera and Spectrograph on the Subaru telescope was used. For shorter wavelengths, we used
SpeX on the NASA IRTF, which has broad wavelength
coverage.
A deep, broad absorption feature is seen at 3 µm in the
spectrum for the trailing side of Amalthea (Fig. 1). The
depth of this absorption feature is 65 ± 13 % of the continuum level at 2.5 µm. This 3-µm absorption feature is
an important diagnostic of the composition of Amalthea’s
surface. The absorption band near 3 µm indicates the hydroxyl (O–H) stretch fundamental or the first overtone of
the water (H2 O) stretch modes. The most likely locationof this water is within water containing hydrous minerals.
Such minerals typically form in low temperature environments.
According to current formation models of the jovian
satellites [2], temperatures of the circumjovian nebula at
the present location of Amalthea exceeded 800 K. Thismodel temperature is too high to form hydrous minerals.
Therefore our results suggest that Amalthea either formed
in a cooler region of the circumjovian nebula at a larger distance than its present orbit, or that it is a product of early
capture from a heliocentric (asteroidal) orbit.
A possible scenario is that Amalthea, and possibly Thebeand two other inner satellites Metis (JXVI) and Adrastea(JXV), were satellite embryos that formed near Callisto andthen migrated into inner region. Because the temperatureof the circumjovian subnebula near Callisto was cold forhydration, accretion or tidal heating may have occurred on
Amalthea.
Another possibility is that Amalthea is a captured planetesimal. Most of the asteroids with heliocentric distancesnear Jupiter are D-types. Thus, it is likely that planetesimals with the same origins as D-type asteroids were captured into the early jovian system, and spiraled inward under gas drag. Amalthea and the other three satellites can be
the remnants of these planetesimals.

Figure1: A Comparison of the Reflectivity of Amalthea, Thebe, Callisto and Asteroids. Amalthea (red line) and Thebe (blue line)
have reflective spectra similar to those seen in regionsof Callisto where there is little water ice (black line). The dip in the
spectrum around 3 µm indicates the presence of water containing minerals. The spectrum at wavelengths shorter than
2.5 µm is similar to ”D-type” asteroids (pink region), a typeof asteroid common in the vicinity of Jupiter’s orbit aroundthe Sun.

References[1] Takato, N., et al.: 2004, Science, 306, 2224.
[2] Canup, R. M., and Ward, W. R.: 2002, Astron. J., 124, 3404.

29

Near-Infrared Unidentified-Line Morphology of the Planetary
Nebula NGC 7027
OKUMURA, Shin-ichiro(Bisei Spaceguard Center, Japan Spaceguard Association)

MORI, Atsushi

YANAGISAWA, Kenshi(Nishi-Harima Astronomical Observatory)(Okayama Astrophysical Observatory, NAOJ)

In the near-IR K window, there remain some emission
lines to be unidentified. The two strong unidentified lines
near 2.199 and 2.287 µm (hereafter UIR1 and UIR2, respectively) were first detected in NGC 7027 [1], [2], andhave since been seen in other Planetary Nebulae (PNe).
However, they had not been identified for more than two
decades. Both UIR1 and UIR2 fall near the wavelengths ofvibrationally excited H2 lines. These spectral coincidences
prevent us from identifying of them. Also, unfortunately,
the lines may have been mistaken for these “high-v” H2lines, which are important indicators of fluorescent excitation.
Here, we present spatial information about UIR1 andUIR2 of NGC 7027 [3], which will bring us new information about the nature of their origins. The spectroscopic
data of NGC 7027 were obtained using Super-OASIS,
mounted on the 188 cm telescope at Okayama Astrophysical Observatory.
Fig. 1 shows the spatial distributions of emission lines,
along the east-west direction across the central position of
NGC 7027. The distributions of the ionized gas are very
similar to that of the continuum emission, whereas, that of
H2 differs from that of any other lines, because the H2 line
is emitted from the periphery of the ionized region. From
the figure, one can easily recognize that UIR1 and UIR2
originate in ionized elements.
The UIR1- and UIR2-emission regions are larger thanthat of HeII, implying that the ionization potentials of thecarriers of UIR1 and UIR2 are lower than that of HeII. In
the figure, the sizes of the UIR1- and UIR2-emission regions appear to be larger than that of Brγ, especially at thewest side of the western peak. It means simply that theionization potentials of their carriers are lower than that ofBrγ.
However, a similar appearance is seen in HeI 21 P –21 S,
though its ionization potential is higher than that of Brγ.
Beyond a critical density, the triplet 23 S (metastable) HeI
level is preferentially collisionally excited, and as a result,the strength of a 21 P –21 S transition is enhanced [4]. We
assume that electron-density is high at the edge in the ionized region, which results in the HeI 21 P –21 S flux enhanced at the edge of the nebula.
We examined the flux-ratio distributions of HeI, UIR1,and UIR2, relative to Brγ, as an index of collisional excitation (see [3] for more details). The ratios of UIR1 andUIR2 to Brγ are found to be somewhat high at the edge ofthe ionized region. Therefore, we speculate that the fluxenhancements of UIR1 and UIR2 (and the “expansion” oftheir emission regions) are caused by contamination of collisional excitation, not by lower ionization potentials of
their carriers.
We conclude that the ionization potentials of the carriersof UIR1 and UIR2 are lower than that of HeII, and compa-

30rable to or slightly higher than that of Brγ. We also notethat their carriers are excited by collisions in part, particularly at the edge of the ionized region. Our conclusions
support the recent proposals for the identifications of them[5], [6]. Further theoretical studies would be helpful to see
how much collisions contribute to their excitation mechanisms. They will provide useful information to identify
UIR1 and UIR2.

Figure1: Spatial distributions of selected emission lines, along the eastwest direction over the central position of NGC 7027. The
dashed lines in each panel show the distribution of the 2.16µm continuum emission.
References[1] Treffers, R. R.: 1976, ApJ, 209, 793.
[2] Smith, H. A., et al.: 1981, ApJ, 244, 835.
[3] Okumura, S. –I., et al.: 2004, PASJ, 56, 705.
[4] DePoy, P., & Shields, J. C.: 1994, ApJ, 422, 187.
[5] Dinerstein, H. L.: 2001, ApJ, 550, L223.
[6] Cox, P., et al.: 2002, A&A, 384, 603.

A Subaru Search for Lyα Blobs in and aroundthe Proto-Cluster Region at Redshift z=3.1
MATSUDA, Yuichi

YAMADA, Toru

(Tohoku University/NAOJ)(NAOJ)HAYASHINO, Tomoki, TAMURA, Hajime, YAMAUCHI, Ryosuke
TANIGUCHI, Yoshiaki, SHIOYA, Yasuhiro, MURAYAMA, Takashi
NAGAO, Tohru, AJIKI, Masaru, FUJITA, Shinobu(Tohoku University)

OKAMURA, Sadanori, SHIMASAKU, Kazuhiro, OUCHI, Masami(University of Tokyo)

OHTA, Kouji(Kyoto University)
Lyα blobs (LABs) are physically extended Lyα nebulae
larger than ∼100 kpc without strong radio sources. The
physical origins of LABs may be (i) photo-ionization bymassive stars, or by active galactic nuclei, or (ii) cooling radiation from gravitationally heated gas, or (iii) shock heating by starburst driven galactic superwind. Although LABs
are expected to be useful to examine the important physicalprocesses of galaxy formation, there have been only a few
LABs discovered in proto-cluster regions at high redshift.

We searched new LABs in and around the proto-cluster
region at redshift z = 3.1 in the SSA22 field [1].
We took panoramic(31 × 23 ) and deep narrow-band◦◦(NB497; 4977A/77A) imaging of the proto-cluster using the prime-focus camera on the Subaru telescope.
We identified 35 robust candidate LABs, which arelarger than 16 arcsec2 in isophotal area and brighter than
0.7 × 10−16 ergs s−1 cm−2 , including the two previously
known giant LABs (see Fig. 1 and Fig. 2).

Figure1: Color images of LABs. Green shows Lyα emission line. Eachpanel is 25 square (190kpc at z=3.1 in physical scale) withthe candidate centered. The two left-upper images show thepreviously known giant LABs.

Figure3: Sky map of Lyα blobs (LABs, blue squares) and relatively
compact Lyα emitters (LAEs, black points). Red line shows
average local surface density of LAEs.

Figure2: Distribution of isophotal area and magnitude on the continuum subtracted NB image for emitter candidates. We selected
the objects with the isophotal area larger than 16 arcsec2 (redline) as candidates of LABs (blue squares). The green line
shows the expected value for point sources. The dotted line
shows detection limit.

It was shown that the two previously known giant LABs
are the most luminous and the largest ones in our survey
volume of 1.3 × 105 Mpc3 . We revealed the internal structures of the two giant LABs and discovered some bubblelike features, which suggest that intensive starburst andgalactic superwind phenomena occurred in these objects
in the past (see Fig. 1). These 35 LABs show a continuous distribution of isophotal area and emission line flux
(see Fig. 2). The 90% of these LABs are located inside
the high surface density region of relatively compact Lyαemitters (see Fig. 3). Our results suggest that LABs larger
than several tens kpc may be common phenomena in dense
environment at high redshift [2].
References[1] Hayashino, T., et al.: 2004, AJ, 128, 2073.
[2] Matsuda, Y., et al.: 2004, AJ, 128, 569.

31

Spiral Structure in the Disk around AB Aur
FUKAGAWA, Misato(The University of Tokyo)

HAYASHI, Masahiko, HAYASHI, Saeko, TAMURA, Motohide(NAOJ)

other 19 co-authors

Figure1: H-band image of the circumstellar structure after the PSF
subtraction. The surface brightness is multiplied by the distance squared from the center for display so that the fainteroutskirts can be viewed with a high contrast. Directions
where the spider patterns affect the image are indicated bydashed lines. The inner area of 1. 7 diameter (r < 120 AU,
filled black circle) is photometrically unusable and is masked.
North is up and east is to the left.

We report the detection of a spiral structure in the protoplanetary disk around AB Aur [1].
Investigation of protoplanetary disks has primary importance to understand the formation of planetary systems. In
order to constrain the formation mechanism, it is indispensable to study the spatial structure of a disk, since it reflects
the physical environment where planets are formed. However, we have little knowledge about the real disk morphology because of the observational difficulty. High-spatialresolution and high-contrast are required for obtaining theimage of a small disk structure in the vicinity of a central
bright star. The number of resolved disks is therefore quite
limited at present.
AB Aur (d = 144+23−17 pc; A0 Ve, [2]) is one of the beststudied Herbig Ae/Be stars, with a mass of 2.4±0.2 M
and an age of 4±1 Myr. The circumstellar structure around
AB Aur consists of two components; a compact rotating
disk of 450 AU radius observed in CO [3] and an extended(> 1000 AU) envelope detected in the optical [4]. The HST
optical observations revealed the inner part of the circumstellar material with a spiral band structure [4], although
the spiral pattern was not very clear possibly because thescattering emission from the more extended material mingles with it.
The H-band (1.65 µm) observations of AB Aur werecarried out in 2004 January, using the stellar coronagraphic
camera CIAO on the Subaru Telescope. The AO was uti32

Figure2: Azimuthally averaged radial profile of the surface brightness(filled circles) after the assumed inclination of i = 30◦ wascorrected. Dashed line indicates a power-law fit with an index
of −3.0 to the brightness over the radial range between 120
and 580 AU. [1]lized, giving the spatial resolution of 0. 1. We occulted
AB Aur with a mask whose diameter was 0. 6. In orderto detect the faint structure buried in the bright halo of thecentral star, we observed the reference star without any circumstellar material, then subtracted the image of the reference star from that of AB Aur.
The obtained image shows extended emission seen fromthe edge of the occulting mask (r ∼ 60 AU) out to theradius of 580 AU (= 4. 0). The radial power-law dependence is r −3.0±0.1 , which is steeper than that of r −2 for the
optical nebulosity. The steeper slope in the NIR suggeststhat the detected light originates mainly from the disk itself
without significantly contaminated by the scattering emission in the envelope.
Of particular interest is a double spiral structure detected
at r =200–450 AU. We identified four major spiral arms,
which are trailing if the brighter, southeastern part of thedisk is the near side. Since the companion stars have notbeen found around AB Aur, the spiral structure could beformed via gravitational instability. The Toomre’s Q parameter can be around 2 at the disk outer edge, within thelarge uncertainty of dust opacity etc. The weak instability,
maintained for millions of years by continuous mass supply from the envelope, might explain the presence of the
spiral structure at the relatively late phase of the pre-mainsequence period.
References[1] Fukagawa, M., et al.: 2004, ApJ, 605, L53.
[2] van den Ancker, M. E., et al.: 1997, A&A, 324, L33.
[3] Mannings, V., and Sargent, A. I.: 1997, ApJ, 490, 792.
[4] Grady, C. A., et al.: 1999, ApJ, 523, L151.

Reverberation Radius of the Central Dust Hole in NGC 5548
SUGANUMA, Masahiro

YOSHII, Yuzuru(JASMINE Project Office, NAOJ)(Institute of Astronomy, School of Science, University of Tokyo)

KOBAYASHI, Yukiyasu

MINEZAKI, Takeo(Advanced Tchnology Center, NAOJ)(Institute of Astronomy, School of Science, University of Tokyo)

ENYA, Keigo(Institute of Space and Astronomical Science, Japan Aerospace Exploration Agency)

TOMITA, Hiroyuki

AOKI, Tsutomu(University of Tokyo/NAOJ)(Kiso Observatory, Institute of Astronomy, School of Science)

KOSHIDA, Shintaro

PETERSON, B. A.

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

Figure1: Our V (open circles) and K (filled circles) light curves of
NGC 5548 nucleus from 2001 March to 2003 July. The lagtime between V and K variations was calculated for the datataken during each of the periods A, B, and C. Inset: Our V
light curve (open circles) of NGC 5548 nucleus, together withthe optical continuum (λ5100Å) data for 13 years by International AGN Watch consortium (vertical lines).

Figure2: The CCFs between observed V and K light curves and the
ACFs of observed V light curves for each of the monitoring
periods A, B, and C. Solid lines and long-dashed lines show
CCFs calculated by two different methods based on linear interpolation scheme. Dot-dashed lines and short-dashed lines
show ACFs.

We report the first measurement of lag time between the
V and K light curves for NGC 5548 [1].
NGC 5548, which is a bright, nearby (z = 0.017)
Seyfert 1 galaxy, has been a target of intensive spectroscopic monitoring observations at ultraviolet and optical
wavelengths for the purpose of reverberation mapping of
the broad emission-line region. We carried out most intensive multicolor monitoring observations in the optical andnear-infrared wave-bands for this object using the multicolor imaging photometer mounted on the MAGNUM telescope [2]. During a monitoring period from 2001 March
to 2003 July, the V (0.55µm) and K(2.2µm) fluxes separately reached a minimum state twice. A delayed responseof light variations in the K band to those in the V band isseen in Fig. 1.
The lag time between the V and K light curves isevaluated by calculating their cross-correlation functions(CCFs). Fig. 2 shows the CCFs for two separate periods,
each containing one clear minimum state, such as (A) 2001
March - 2001 September and (B) 2001 December - 2003
July, and also for our entire monitoring period of (C) 2001
March - 2003 July. Generally, a time shift τpeak which
gives a peak value of the CCF is taken for the lag time. To
estimate the uncertainty of the lag time, Monte Carlo simulations were performed to generate a large number of artificial V and K light curves. The CCFs for any pairs of suchlight curves were calculated to give the frequency distribution of τpeak from which a range of lag time is derived. In
the simulation, we introduced a new technique of simulating the light curves to fill in the sampling gaps between theobservations. The measured lag time is ∆t = 48+3
−2 days indays
in thethe first minimum state (period A), ∆t = 47+5
−6
second minimum state (period B), and 42 − 53 days for thewhole monitoring period of C.
The absolute V -magnitude of the nucleus during themonitoring period is estimated as MV = −18.35 to−19.60, using the known redshift and the apparent magnitude observed in the monitoring period. This estimate
of MV against ∆t is located close to the correlation lineof L ∝ (∆t)2 shown in lag-time measurement of otherobjects in the literature together with our early result for
NGC 4151 [3]. Such a correlation is derived from a theory of dust reverberation, in which the ultraviolet and optical radiation from the central energy source of NGC 5548
is absorbed by the surrounding dust to be reprocessed to
the near-infrared thermal radiation at a temperature corresponding to the sublimation temperature of the dust. Furthermore, the lag time for hot dust is compared directlywith those for the broad emission lines of lower ionization
reported to date for NGC 5548, which the lag time for suchdust reverberation is found to be longer, indicating that the
inner radius of the dust torus corresponds to an outer edgeof the broad emission-line region in NGC 5548.
References[1] Suganuma, M., et al.: 2004, ApJ, 612, L113.
[2] Kobayashi, Y., et al.: 1998, SPIE, 3352, 120.
[3] Minezaki, T., et al.: 2004, ApJ, 600, L35.

33

Gravitational Waves from Coalescing Supermassive Black Hole
Binaries in a Hierarchical Galaxy Formation Model
ENOKI, Motohiro(Astronomical Data Analysis Center, NAOJ)

INOUE, Kaiki TaroNAGASHIMA, Masahiro(Kinki Univ.)(Kyoto Univ.)

SUGIYAMA, Naoshi(Division of Theoretical Astronomy, NAOJ)

Figure1: Black hole mass function of the model at a series of redshifts[2]. The symbols with errorbars are the observed black holemass function at z = 0 [3].

Figure2: Spectrum of gravitational wave background radiation, hc (f ),from SMBH binaries in different redshift intervals (a) and indifferent total mass intervals (b) [2].
-14 (a)(b)-18

ν > 1/5 yr-1

-20
-22
-4

-3

-2

log(fc [Hz])34

hinst (1/3 yr)
hinst (5 yr)

LISA noise (1 yr)-5

References[1] Enoki, M., et al.: 2003, PASJ, 55, 133[2] Enoki, M., et al.: 2004, ApJ, 615, 19[3] Salucci, P., et al.: 1999, MNRAS, 307, 637

ν > 3 yr-1

ν > 1 yr-1

-16

log(hburst)

We investigate the expected gravitational wave emission
from coalescing supermassive black hole (SMBH) binaries
in the mass range of 106 − 109 M resulting from mergers of their host galaxies. When their host galaxies merge,
SMBHs sink toward the center of the new merged galaxy
and form a SMBH binary subsequently. Then, it will evolveto the gravitational wave emitting regime and begin inspiraling, eventually coalesces with a gravitational wave burst.
An ensemble of gravitational waves from a number of inspiraling SMBH binaries can be observed as a gravitational
wave background radiation (GWBR). Future space interferometers such as the Laser Interferometer Space Antenna(LISA) might detect GWBR and gravitational wave bursts.
In order to estimate the amplitude of the expected
GWBR owing to inspiraling SMBH binaries and bursts
rates owing to the SMBH binary coalescence events, weemploy a semi-analytic model in which the SMBH formation model is incorporated into the galaxy formation model
based on the hierarchical clustering scenario [1], [2]. In
our model, it is assumed that a SMBH is fueled by accretion of cold gas during a major merger of host galaxies andthat SMBHs coalesce simultaneously when host galaxies
merge. Fig. 1 shows the black hole mass functions in ourmodel. The predicted mass function is quite consistent withthe observation.
We plot the spectrum of GWBR from binaries in different redshift intervals (Fig. 2(a)) and in different total massintervals (Fig. 2(b)). The GWBR spectrum for f ≤ 1µHz
has a characteristic strain hc (f ) ∼ 10−16 (f /1µHz)−2/3 .
From these figures, we have found that the GWBR mainly
comes from inspiraling SMBH binaries with total mass
Mtot ≥ 108 M at 0 < z < 1. Therefore, the GWBR
can be used as a probe of inspiraling SMBH binaries at low
redshift. Fig. 3 shows that the expected region for signal ofgravitational wave bursts and the instrumental noise threshold for LISA. We have also found that LISA might detect
intense bursts of gravitational waves owing to the SMBH
coalescence events at a rate 0.1 ∼ 1.0 yr−1 and that themain contribution to the rate comes from SMBH binary coalescence events at high redshift z ≥ 2. Comparing thesepredictions with observations in future, we can put a stringent constraint on SMBH formation and evolution models.

-1

0 -5

-4

-3

-2

-1

0

log(fc [Hz])Figure3: Expected signals of gravitational wave bursts from SMBH coalescence [2]. The solid, dot-dashed and the short dashedcurves indicate the instrumental noise threshold for 1 year,
5 year and 1/3 year of LISA observations, respectively.

The origin of light neutron-capture elements in very metal-poor stars
HONDA, Satoshi, AOKI, Wako, ANDO, Hiroyasu(Division of Optical and Infrared Astronomy, NAOJ)

KAJINO, Toshitaka

IZUMIURA, Hideyuki(Division of Theoretical Astronomy, NAOJ)(Okayama Astrophysical Observatory,NAOJ)

BEERS, Timothy C.

SADAKANE, Kozo

TAKADA-HIDAI, Masahide(Michigan State University)(Osaka Kyoiku University)(Tokai University)

It is known that the elements heavier than iron are synthesized by neutron-capture processes. However, there
still remains unsolved problems on the rapid process (rprocess), which is responsible for about half of neutroncapture elements in the solar system. In order to know
the nature of the r-process, an effective method is to investigate the abundances of metal-poor stars, because it
is believed that the heavy elements of metal-poor stars
were supplied only by a few supernavae, and the nucleosynthesis yields from individual processes, including rprocess, can be directly estimated from their abundance
patterns. We performed high resolution spectroscopy covering light neutron-capture elements (e.g., Sr[Z = 38]) to
heavy neutron-capture elements (e.g., Eu[Z = 63]), andfurther actinide (Th[Z = 90]), for metal-poor stars, anddetermined their abundances [1].
We have obtained spectra with resolving power of R =50,000 for 22 objects with the Subaru High Dispersion
Spectrograph (HDS). Our abundance analysis confirmedthat the abundance patterns of the elements with the atomic
number from 56 to 70 are similar in metal-poor stars in our
sample, and those are in agreement with the abundance pattern of the solar system r-process component. This resultmeans not only that these heavy elements are synthesized
by the r-process, but also that the abundance pattern produced by the r-process is universal.
However, the abundance ratios of the light neutroncapture elements (38 ≤ Z ≤ 46) relative to the heavier
ones (56 ≤ Z ≤ 70) exhibit a large dispersion. We here
adopt Sr (Z = 38) and Ba (Z = 56) as representativesof light and heavy neutron-capture elements. Fig. 1 shows
the abundance ratios as a function of metallicity. There isa large dispersion close to 2 dex in the abundance ratios at[Fe/H] = –3.

Since our sample shown in Fig. 1 is extremely metalpoor stars, the chemical composition is expected to reflecta small number of nucleosynthesis process. Therefore weshow the correlation between Sr and Ba abundances in Fig.
2, ignoring their metallicity dependence. This figure showsthat (1) there is no Sr-poor star with high Ba abundance,and (2) the dispersion of Sr abundance is remarkable in
Ba-poor stars. This trend can be explained by hypothesizing following two nucleosynthesis process. One is theprocess which produces Sr and Ba in similar proportions.
The elements of heavier than Ba would be synthesized bythis process in the early Galaxy (this process is sometimes
called as main r-process which is well known so far). The
other is the process producing Sr without Ba.
Fig. 2 suggests that the main r-process yields Sr and Ba
with the abundance ratio close to unity. Concerning thelatter process, recent observational and theoretical studies
have suggested its existence. Our observations clearly revealed the nature of this process. This process differs froms-process and main r-process which were known so far, andshould be an important source of the light neutron-capture
elements in the universe.
In order to understand the nature of this nucleosynthesis
process in detail, we quite recently investigated the correlation using the Y, Zr, La, and Eu which can be measured
more accurately than Sr and Ba [2]. We are also performing
more detailed abundance analysis for a few selected stars
that represent this process. These observations will give an
important indicator for modeling of this process.

Figure2: Correlation between abundances of Sr and Ba for objects with
[Fe/H] ≤ -2.5 from same sample in Fig. 1. Solid arrow showsthe enrichment of Sr and Ba (main r-process), dashed arrowshows enrichment of Sr (weak r-process).

Figure1: [Sr/Ba] as a function of [Fe/H] from previous studies (opencircles) and present work (filled circles).

References[1] Honda, S., et al.: 2004, ApJ, 607, 474.
[2] Aoki, W., et al.: 2005, ApJ, 632, 611.

35

The mm-Wave Detection of a Radio Source
following the 27 December 2004 Giant Flare from SGR 1806–20
MIYAZAKI, Atsushi(Shanghai Astronomical Observatory)

TSUBOI, Masato, OKUMURA, Sachiko(Nobeyama Radio Observatory, NAOJ)

KAWAI, Nobuyuki(Tokyo Institute of Technology)
On 27 December 2004, a giant flare was detected from
SGR (Soft Gamma-Ray Repeater) 1806–20 [1], [2]. Softgamma-ray repeaters (SGRs) are the remarkable transientson γ-ray, which are neutron stars with intense (≤ 1015 G)
magnetic fields (‘magnetars’), and these objects cause giant
flares rarely. Four objects were known in all sky until now.
SGR 0526–66 and SGR 1900+14 caused an enormous flarein 1979 and 1998, respectively. The present flare was thestrongest case in the history of γ-ray observation and saturated almost all γ-ray detectors of astronomical satellites.
It is a phenomenon as rare as once for ten years.
On 3 January 2005, a radio counterpart of SGR 1806–
20 was identified with the Very Large Array (VLA) at 1.4,
4.9, and 8.5 GHz and reported. The spectrum from thesedata can be modeled by a power law. Then we promptly
observed SGR 1806–20 using the Nobeyama Millimeter
Array (NMA) in order to detect the radio counterpart at
mm-wavelength and search a spectral break on the radio
spectrum. Fig. 1 (left panel) shows the intensity map toward SGR 1806–20 at 102 GHz at 4 January 2005. The delay from VLA to NMA observation is ∼8 hours. There is acompact peak with 16.3 ± 5.6 mJy at the map center. Thisis the first and unique detection of the radio counterpart at
mm-wavelength with confidence level of about 3σ. The radio spectrum from 0.2 GHz to 100 GHz on 4 January 2005
was obtained by combination of observations with NMA,
VLA, and GMRT (Fig. 2). The radio spectrum can be modeled by a single power law. The best fit spectral index isabout −0.6. There is no spectral break on the spectrum.
Continuing observation is necessary in order to monitor
the light curve at mm-wavelength of this radio afterglow.
However, we could not observe it by bad weather and tightschedule. The follow-up observations were performed at
12 and 13 January. Fig. 1 (right panel) also shows theresult. There is no significant peak in the map. The 1σ
upper limit is about 3 mJy. The counterpart at 102 GHz
was already fade out. We probably confirm a claim fromcm-wavelength observations that the radio afterglow fades

36

more rapidly at higher frequency. The result with NMA
was published as a part of an international monitoring program in Nature [3].

Figure1: Radio map at 102 GHz of SGR 1806–20 with NMA. The
epoch of the left panel is 4 January 2005, that of right panel is
13 January 2005.

Figure2: Radio spectrum of SGR 1806–20 (reconstructed from
Cameron et al. 2005 [3]). Red circles show results on 4 January 2005 with GMRT, VLA, and NMA. Blue diamonds show
results on 13 January 2005 with ATCA and NMA. The blue
horizontal bar at 102 GHz indicates 1σ upper limit by NMA.

References[1] Palmer, D. M., et al.: 2005, Nature, 434, 1107-1109.
[2] Terasawa, T., et al.: 2005, Nature, 434, 1110-1111.
[3] Cameron, P. B., et al.: 2005, Nature, 434, 1112-1115.

Results of Gravitational Wave Search with TAMA300 detector
FUJIMOTO, Masa-Katsu, KAWAMURA, Seiji, YAMAZAKI, Toshitaka
TAKAHASHI, Ryutaro, ARAI, Koji, TATSUMI, Daisuke, FUKUSHIMA, Mitsuhiro
SATO, Shuichi, TSUNESADA, Yoshiki, HAYAMA, Kazuhiro(TAMA Project Office, NAOJ)TAGOSHI, Hideyuki

ANDO, Masaki

KANDA, Nobuyuki(Osaka University)(University of Tokyo)(Osaka City University)

the TAMA Collaboration
Since 1999, the Japanese laser interferometric gravitational-wave (GW) detector TAMA300 has performed observations nine times until April of 2005. As a result, 3086
hours of data have been accumulated totally. The detector
sensitivity and its stability have been also improved gradually during the observation periods. In this article, we report the current status of several GW signal searches in the
TAMA300 data.
Chirp Signals from Neutron Star Binaries
We performed a coincidence analysis to search for inspiraling compact binaries with the LISM detector [1]. LISM isan interferometer originally developed at the Mitaka campus, and then was moved to the Kamioka mine in Gifu prefecture, Japan. The data used for the coincidence analysis
is 275 hours long. Both TAMA300 and LISM data were analyzed by matched filtering and candidate events were obtained. If there is a true gravitational wave signal, it should
appear in both data with consistent waveforms characterized by masses of stars, amplitude of the signal and the coalescence time. We introduced a set of coincidence conditions of the parameters, and searched for coincident events.
This procedure reduces the number of fake events considerably, by a factor of ∼ 104 compared with the number offake events in the single detector analysis. After imposing
the coincidence conditions, we found that the number of
selected events is consistent with the number of accidental
coincidences produced purely by noise. Thus, we found noevidence of gravitational wave signals. However, we obtained an upper limit of 0.046 events/hour (C.L.=90%) for
the galactic event rate within 1 kpc from the Earth.
Burst Signals from Supernova Explosion
Data-analysis targeting burst signals from stellar-core collapse events were also performed [2]. For the analysis, weused an excess-power filter for the extraction of gravitational wave candidates, because precise waveforms are notavailable. We developed two methods for the reduction of

fake events caused by nonstationary noises of the detector.
As a result, fake events were reduced by a factor of about1000 in the best cases. We set an upper limit of 5.0 ×103
events/sec on the burst gravitational wave event rate in our
Galaxy with a confidence level of 90%.
Ring-Down Signals from Black-Hole Quasi-Normal
Mode Oscillation
Gravitational radiation from a slightly distorted black holewith ringdown waveform is well understood in general relativity as a quasi-normal mode oscillation. It provides aprobe for direct observation of black holes and determination of their physical parameters, masses and angular momenta (Kerr parameters). For ringdown searches, matchedfiltering technique is useful. We studied on the matched filtering analysis in realistic gravitational wave searches using observational data [3]. To investigate them, we have
performed the matched filtering analysis for artificial ringdown signals which are generated with Monte-Carlo technique and injected into the TAMA300 observational data.
With the TAMA300 sensitivity, we found that the detection
probability for Galactic ringdown events is about 50% forblack holes of masses greater than 20M with SNR > 10.
The resolutions for black hole masses and the Kerr parameters are evaluated as a few % and 40%, respectively. They
can be improved up to < 0.9% and < 24% for events of
SNR > 10 by using fine-meshed template bank in the hierarchical search strategy.
References[1] Tagoshi, H., et al.: 2004, PRD, 70, 0042003.
[2] Ando, M., et al.: 2005, PRD, 71, 082002.
[3] Tsunesada, Y., et al.: 2005, PRD, 71, 103005.

37

Intra-day Variation of Sagittarius A∗ at mm-Wavelengths
MIYAZAKI, Atsushi(Shanghai Astronomical Observatory)

TSUTSUMI, Takahiro(NAOJ)TSUBOI, Masato(Nobeyama Radio Observatory, NAOJ)
We report our detection of intraday variation of Sagittarius A∗ at 140 GHz in the 2000 Mar flare using theNobeyama Millimeter Array (NMA) of the Nobeyama Radio Observatory [1].
Sagittarius A∗ (Sgr A∗ ) is the compact radio source located at dynamical center of the Galaxy, and is a supermassive black hole with ∼ 4 × 106 M . After its discovery,
Sgr A∗ was observed at many wavelengths, and, however,its emission mechanisms are not yet fully understood. Because this source is embedded in thick thermal material,
it is practically difficult to observe its fine structure. The
time variability observation is a powerful tool to probe thestructure and the emission mechanism, if the variability is
intrinsic. Sgr A∗ time variability at mm-wavelength was reported the first significant flux variation at 80 GHz in 1990[2], and we have detected a flare in Mar 1998 using NMA[3], [4].

We have performed the monitoring observations of theflux density of Sgr A∗ from 1996 to 2005 using NMA. The
monitoring observations of Sgr A∗ have been carried out atshot mm-wavelengths (100 and 140 GHz) bands over one
to several months on each observable season. We have detected several flares [3], [4], [5]. In particular, we foundintraday variation of Sgr A∗ in the 2000 Mar flare [6] . We
detected the about 30% increase in 30 minutes at 140 GHz
on 7 Mar 2000 (Fig. 1), and the twofold increase timescaleof the flare is estimated to be ∼ 1.5 hr. This intraday variation at mm-wavelengths has a similar increase timescaleas those in the X-ray and infrared flares (X-ray flare [6],infrared flare [7]) but has smaller amplitude. This shorttimescale variability suggests that the physical size of emitting region of the flare is compact at or below about 12 AU(≈ 150 Rs ; Rchwarzschild radius assuming a black holemass of 4 × 106 M ). Our result is consistent with theintraday variation detected at 3-mm using the OVRO mminterferometer in May 2002 [8]. There is asymmetry in
the light curve as the half decay timescale is much longer
than the flare increase timescale. A light curve with rapid
increase and slow decay obtained by our observations issimilar to that often observed in outburst phenomena withejections, for example, flares on the Sun, the 1972 outburstof Cyg X-3, etc.
References[1] Miyazaki, A., et al.: 2004, ApJL, 611, L97.
[2] Wright, M. C. H., & Backer, D. C.: 1993, ApJ, 417, 560.
[3] Miyazaki, A., et al.: 1999, Adv. Space Res., 23, 977.
[4] Tsuboi, M., et al.: 1999, in ASP Conf. Ser. 186, The Central Parsecsof the Galaxy, 105.
[5] Miyazaki, A., et al.: 2003, Astron. Nachr., 324, 363.
[6] Baganoff, F. K., et al.: 2001, Nature, 413, 45.
[7] Genzel, R., et al.: 2003, Nature, 425, 934.
[8] Mauerhan, J. C., et al.: 2005, ApJL, 623, L25.

Figure1: Light curves of the Sgr A∗ flare and the calibrators(NRAO 530, 1830-210) at 140 GHz band on 7 (red) & 8(blue) Mar 2000 with NMA [6]. The Sgr A∗ flux density at
146 GHz (red filled squares in bottom panel) increased from
3.5 to 4.7 Jy from 21:45 to 22:15 UT on 7 Mar. The horizontal
dashed line is the mean flux density at 140 GHz.

38

Asymmetric Surface Brightness Distribution of Altair
Observed with the Navy Prototype Optical Interferometer
OHISHI, Naoko(National Astronomical Observatory of Japan)

NORDGREN, T. E.

HUTTER, D. J.

(Redlands University)(U. S. Naval Observatory)

The star Altair (A7IV-V) is known to be a rapid rotatorwith v sin i ∼200km/s. Because the apparent disk diameterof the star is ∼3mas, it is difficult to resolve the star witha single telescope. However, recent development of optical and infrared interferometers have made it possible tosee its shape directly. In 2001, van Belle et al.[1] reported
the star is distorted because of rapid rotation based on thedata obtained with the PTI (Palomar Testbed Interferometer).We observed the star with the NPOI (Navy Prototype
Optical Interferometer) and found that the star is not only
elongated but also asymmetrically brightened. Altair is thefirst main sequence star for which direct measurement of
the asymmetry of surface brightness distribution have beenreported.
Characteristics of our observation are high resolution
with the longest baseline of 64m and the measurement ofclosure phases, which is a sensitive indicator of the asummetry of the brightness distribution of the source. simultaneous observation using three telescopes. A part of measured observables of Altair and Vega for comparison isshown in Fig. 1. While the observables of Vega are wellfitted with the limb darkening model with the diameter of
3.22mas, those of Altair are discrepant with the limb darkening model with the diameter of 3.32mas.

The discrepancy indicates that a small bright region is located on the stellar surface. Thus we made a simple modelwith a bright spot on a limb darkened ellipse and fittedwith the observables. As a result, this model (blue lines
in Fig. 1) explained the data better than the limb darkening
model. The surface brightness distribution of the modelwith the best fitted parameters is shown in Fig. 2.

Figure1: A model with a spot on a limb darkened ellipse with the major
axis of 3.29mas and the minor axis of 2.77mas.

Because of the rapid rotation of the star, the spot mentioned above indicates existence of a bright pole of a gravity darkened star. We intend to determine the physical parameters of the rotating star with Roche model.
References[1] van Belle, G. T., et al.: 2001, ApJ, 559, 1155.
[2] Ohishi, N., et al.: 2004, ApJ, 612, 463.

Figure2: Measured observables of Vega (upper) and Altair (lower) obtained in 2001 May 25.; From left to right, squared visibility amplitudes of baselineof 29m, 37m, 64m, triple amplitudes, and closure phase. Measured observables of Vega is well fitted with the limb darkening model with thediameter of 3.22mas (red lines). However, the triple amplitudes around the first zero and closure phaseof Altair are discrepant with the limb
darkening model with the diameter of 3.32mas.A spot on a limb darkened ellipse model (blue lines) reproduce the data better.

39

The Qualification Model of ALMA Band 8 Cartridge Receiver
SAITOU, Naohisa, IIZUKA, Yoshizo, ITO, Tetsuya, KAMBA, Toshiaki, SEKIMOTO, Yutaro(NAOJ)

SHAN, W. L.
(NAOJ/Purple Mountain Observatory)

KAMIKURA, Mamoru, TOMIMURA, Yu, SERIZAWA, Yasutaka, TOBA, Hiroyuki(University of Tokyo)

NOGUCHI, Taku, ASAYAMA, Shinichiro, SUGIMOTO, Masahiro(NAOJ)

Figure2: A photo of ALMA band 8 cartridge Qualification Model.
Figure1: Design of ALMA band 8 cartridge Qualification Model (QM).

We report design and development of the qualification
model of ALMA band 8 cartridge receiver.
The ALMA band 8 cartridge receives frequency from385 GHz to 500 GHz, which is 26 % bandwidth to the center frequency of 442.5 GHz. The development and production of the band 8 Cartridges is one portion of the Japanesecontribution to ALMA. We have developed the qualification model of ALMA band 8 cartridge as shown in Figures.
It receives linear dual polarization simultaneously by using a wire grid as a polarization splitter. It employs sideband separating mixers with a waveguide quadrature hybrid[1], which is a scaled model of ALMA band 4 cartridge.
The SIS mixers for the band 8 have very low noise as low
as 3 times quantum noise limit [2].
The receiver optics adopts a single mirror to couple thefeed horn in front of the mixer and the sub-reflector [3].
The merit of single mirror to two mirrors is relatively easy
to align optical components of horns, mirrors and a wire
grid [4]. The optical parameters were chosen as indepen40

dent at both the feed horn and the sub-reflector in the frequencies of between 385 and 500 GHz. The receiver optics is inclined 1.2 degree toward the subreflector. The
optics block was carefully designed mechanically to realize the optical parameters. The optics block and mirrors
were measured mechanically with a coordinated measuringmachine, Mitsutoyo LEGEX910 of the Advanced Technology Center of NAOJ, and consistent with designed values
within typically 20 µm.
It has been designed and developed on a column-type
cartridge structure, which has been described by Yokogawa
et al. [5]. Similar cartridge for 800 GHz band has been developed and demonstrated on the Atacama Submillimeter
Telescope Experiment by Sugimoto et al. [4].
References[1] Asayama, S., et al.: 2003, ALMA memo, 453.
[2] Shan, W. L., et al.: 2005, IEEE Trans. AS, 15, 503.
[3] Carter, M., et al.: 2004, SPIE, 5489, 1074.
[4] Sugimoto, M., et al.: 2004, PASJ, 56, 1115.
[5] Yokogawa, S., et al.: 2003, PASJ, 55, 519.

Cartridge-Type 800 GHz Receiver for the ASTE
SUGIMOTO, Masahiro, SEKIMOTO, Yutaro, TATEMATSU, Ken’ichi, KAMBA, Toshiaki
TOBA, Hiroyuki, NOGUCHI, Takashi, YAMAGUCHI, Nobuyuki, KANDORI, Ryo(NAOJ)OKUDA, Takeshi, KOHNO, Kotaro(University of Tokyo)

Figure1: (a) Photograph of the 800 GHz cartridge-type receiver. (b)Diagram of the cartridge-type receiver. A 3-stage Gifford
McMahon cryocooler is not shown in this diagram for simplicity.

We have developed a cartridge-type 800 GHz receiver
for the ASTE telescope in Atacama, Chile [1].
The receiver has been assembled with a cooled receiver
optics, a Nb-based SIS mixer, a local oscillator (LO) optics,
and IF components in a 170 mm diameter column-type cartridge as shown in Fig. 1. The cooled optics is composed ofa single ellipsoidal mirror to couple between the feed horn
and the subreflector of the antenna, and an LO coupler with
10% efficiency.
Cartridge-test cryostats that can cool one cartridge-type
receiver have been developed to evaluate the receivers inlaboratories [2]. Most performances of this receiver were
measured using this cryostat. Owing to its cartridge andcryostat structure [3], [4], [5], the mechanical vibrationsof the GM cryocooler are significantly reduced, and therefore the receiver is highly stable on the telescope. The receiver noise temperature, using a Nb-based SIS mixer anda 4 − 8 GHz HEMT amplifier, was attained to 1300 K in
DSB at an LO frequency of 815 GHz.
Three cartridge-type receivers including the 800 GHz receiver were integrated into the ASTE cryostat at the Mitaka
campus of the National Astronomical Observatory of Japan(NAOJ). We verified the conditions of evacuation, the cooling properties, the electronic properties, and mechanicalinterference of the three receivers. Finally, we confirmedthat their performance is almost the same as that measured
with the cartridge-test cryostat. After integration, the sys-

tem was shipped to the ASTE site.
Total power measurements scanning across the Moon
were performed to estimate the beam pattern of the telescope. The measured beam pattern was fitted withthree Gaussian components.
The half-power beamwidth (HPBW) of the main beam was determined to be
11. 8±3. 5. This value is consistent with the diffraction
limit (1.2 ·λ/D ∼ 9. 2) of a 10 m antenna at 806 GHz.
2nd and 3rd Gaussian components have amplitudes of −4and −8 dB, respectively. The observed error beams is consistent with a simulated error beam. It was calculated using
the surface error which is predicted by the Finite Element
Method (FEM). After the observations in 2003, a surface
adjustment was carried out considering the gravitational
deformation between the holography elevation of 5.7◦ andthe rigging elevation of 55◦ . The beam pattern measurement at observing elevations of 30–80◦ is expected to bebetter than those reported in the present paper.
The system noise temperature, Tsys , was typically 4000−
8000 K in DSB at an LO frequency of 812 GHz during operations, which depended on the atmospheric opacity. The
typical zenith opacity at an LO frequency of 812 GHz was∼ 1. A spectrum of the CO J = 7−6 line (806.6518 GHz)
toward Orion KL was successfully detected (Fig. 2).

Figure2: CO J = 7−6 (806 GHz) spectrum around Orion KL. The integration times are 20 s. Ta∗ was scaled under the assumptionof a sideband ratio of 1.

References[1] Sugimoto, M., et al.: 2004, PASJ, 56, L1115.
[2] Sekimoto, Y., et al.: 2003, ALMA memo, 455.
[3] Yokogawa, S., et al.: 2003, PASJ, 55, L519.
[4] Orlowaska et al.: 2002, ALMA project book, Ch. 6.
[5] Sugimoto, M., et al.: 2003, Cryogenics, 43, L435 .

41

Photometric Observations of a Young Family Asteroid (832) Karin
YOSHIDA, Fumi, ITO, Takashi, NAKAMURA, Tsuko

DERMAWAN, Budi

(NAOJ)(BIT)

SAWABE, Yu, HAJI, Masashige, SAITO, Ryoko, HIRAI, Masanori(FUE)

SATO, Yusuke

YANAGISAWA, Toshifumi

MALHOTRA, Renu

(U. Tokyo)(JAXA)(U. Arizona)

The Karin family was born only 5.8 million years ago[1]. Most asteroid families are very old (∼ 2 Gyr), andthey have undergone significant collisional and dynamical
evolution since their formation that likely masks the properties of the original collisions. But the remarkably young
Karin family asteroids possibly preserve some signaturesof the original collisional event that formed the family. The
Karin family would offer us several significant opportunities for asteroid research, such as the potential detection of
tumbling motion of each family member, distributions ofrotation period, and shape of newly-created asteroid fragments. Another important point is about space weathering. Generally, the reflectance spectra of S-type asteroids
become redder with increasing of its surface age. However the time scale of the space weathering has not been
known yet. Since the Karin family is a S-type cluster, it isvery suitable observing target for getting information about
space weathered surface of young asteroid. Based on thesemotivations, we have begun a program to observe the Karinfamily members since November 2002. Here we report
our photometric observations of (832) Karin, which is thelargest member of the Karin family [2].

that the color variation is due to the difference between the
fresh surface, excavated by the family-forming disruption,and the weathered surface, originated from a parent body
exposed to space radiation and particle bombardment overa long period. The existence of the color variations is supported by a near-infrared spectroscopy of this asteroid [3].
They exploited the CISCO at the 8.2-m Subaru Telescopeon Mauna Kea, Hawaii. They found that there are two different spectra on its surface, one is similar to the spectra ofordinary S-type asteroids, another one matches well withthe spectra of ordinary chondrites, possibly coming fromthe fresh inside of parent bodies. This trend is quite similar
to what we have obtained in our observations (Fig. 2(b)).
We will keep observing the Karin family asteroids. They
will give us important and unique information about asteroid disruption event.

Figure1: Lightcurve of (832) Karin. The rotation period is found to be
18.35 ± 0.02 hr.

We observed (832) Karin from 2003 July to September.
We used the 1.8-m telescope at Vatican observatory, Arizona, USA for our multicolor (B, V , R, and I-bands) observation and the 40 cm telescope belonging to the Fukuoka
University of Education for our lightcurve observation.
Fig. 1 shows the lightcurve of (832) Karin. Its rotational
synodic period was determined to be 18.35±0.02 hr. Fromcolor observations, we found an interesting surface color
variation of this asteroid (see Fig. 2(a) and (b)). We infer
42

Figure2: (a) Color variation on (832) Karin’s surface. (b) Relative reflectance spectra for the different hemispheres of Karin. Bothrelative reflectances were normalized at the V-band.
References[1] Nesvorný, D., et al.: 2002, Nature, 417, 720.
[2] Yoshida, F., et al.: 2004, PASJ, 56, 1105.
[3] Sasaki, T., et al.: 2004, ApJ, 615, L161.

Evaluation of ALMA 12-m Prototype Antenna
SAITO, Masao, UKITA, Nobuharu, IKENOUE, Bungo, EZAWA, Hajime, YAMAGUCHI, Nobuyuki(NAOJ)

ATF team
The National Astronomical Observatory of Japan(NAOJ) has conducted the evaluation activities on the 12-m
prototype antenna for Atacama Large Millimeter Submillimeter Arrays (ALMA) in astronomical observations withevaluation equipments in order to check whether the antenna meets the required performance under the operating
conditions. The antenna was designed, manufactured, anddelivered to the VLA site of the National Radio Astronomy Observatory (NRAO) in Socorro, New Mexico, US
in 2002. After the assembly on site and the adjustment,
the performance testing had been repeatedly conducted forabout 6 months under as various operating conditions as
possible in 2003 [1], [2].
Since measurements to confirm its performance are very
challenging, the American, European, and Japanese teams
have collaborated in establishing the evaluation method andthe measurement technology as well as development of theevaluation equipment for several years. They are the computer control system for tracking celestial sources and forevaluation equipment, the radio holography receiver system for the surface accuracy measurement [3], the evaluation receiver system operating at the 1- and 3-mm bands,
the optical telescope for measuring the pointing and tracking accuracy [4], the temperature monitor system for estimating thermal deformation of each part of the antenna andthe accelerometer system which measures minute vibrationof the antenna.
In the evaluation activities, the NAOJ used evaluationequipments such as an optical pointing telescope system
and a submillimeter receiver system newly developed andintegrated. The results of the evaluation have confirmedthat the prototype antenna satisfied the major technicalspecifications including the surface accuracy of 25 µm rms,
the offset pointing and tracking accuracy of 0.6 arcsec rms,
and the fast motion capability with a step of 1.5 degrees on
the sky within 1.5 seconds of time. The path length error(< 20 µm rms) has not been measured. Previous successful
developments of high precision aluminum reflector panels
and a high precision angle encoder greatly contributed tofulfill the required performance. On the other hand, we
have not obtained the target values in some items including
the temperature control in the receiver cabin, which are lessimportant compared with the main technical specifications
mentioned above. They shall be reflected in the design ofthe production antennas in the future.
The evaluation activities of the 12-m prototype antenna
has demonstrated that the large millimeter and submillimeter antenna is technically highly feasible and it has alsoenabled us to establish evaluation methods and measuring

techniques for the high precision antenna. In addition, we
have gained the valuable technical expertise for the future
operation of the antennas in Chile.
References[1] Ukita, N., et al.: 2004, SPIE, 5489, 1085.
[2] Saito, M., et al.: 2004, JAS Fall meeting.
[3] Saito, M., et al.: 2004, JAS Spring meeting.
[4] Ikenoue, B., et al.: 2004, JAS Fall meeting.

Figure1: Optical pointing measurement of absolute pointing accuracy,
blue dots are measurement, red denotes fitting results, The
measured azimuth and elevation pointing error was 0.85 and0.80 arcsec and the total absolute pointing error was 1.17 arcsec rms.

Figure2: Surface Accuracy of the 12-m antenna by Radio Holography,
left:before adjustment 122 µm rms, right:after adjustment 20µm rms.

43

Detection of New Molecules in a Bright Leonid Fireball
ABE, Shinsuke(Ondřejov Observatory, The Czech Republic / Kobe University)

EBIZUKA, Noboru

YANO, Hajime(RIKEN)(ISAS/JAXA)WATANABE, Jun-ichi

BOROVIČKA, Jiřı́(Public Information Center, NAOJ)(Ondřejov Observatory, The Czech Republic)

Figure1: First and second order spectrum of 2001 Leonid fireball. This
image (with a field of view of 23◦ × 13◦ ) is composed of
15 consecutive frames during a total duration of 0.5 s. The
meteor moved from top to bottom and the dispersion direction
is from left to right. A maximum brightness of – 4 visual
magnitude at the standard range of 100 km was derived, whichcorresponded to a photometric meteoroid mass of ∼1.8 g anda diameter of ∼15 mm by assuming a density of 1.0 g cm−3

An ultraviolet-visible spectrum between 300 and 450 nm
of a cometary meteoroid that originated from 55P/TempelTuttle was investigated, and its new molecules, induced byatmospheric interaction, were discovered [1].
Spectroscopic observations of meteors reveal not only
the chemical composition of the cometary meteoroids but
also the emission processes of hypervelocity impacts in theatmosphere(11.2 − 72.8 km s−1 ); these processes are difficult to reproduce in laboratory experiments at present.
Of particular interest is the question as to whether or not
meteoroids could have delivered organics and water to theearly Earth until now. To determine whether large cometary
grains contain mineral water or trapped water in any forms,
it is necessary to confirm the presence of OH A2 Σ+ →X 2 Π emission around a wavelength of 310 nm.
During the 2001 Leonid meteor shower over Japan,
The spectroscopy was carried out using an intensified highdefinition TV camera with a slitless reflection grating andoriginal developed UV lenses ( f =30 mm, F/1.2). In Fig. 1,
we show a clear spectrum of a Leonid meteor fireball,which was obtained at 18:58:20 UT on 2001 November
18. Assuming the local thermal equilibrium (LTE), theatomic synthetic spectrum was computed by adjusting fiveparameters: temperature T and the column densities offour atoms (Fe, Mg, Ca, and Na). After the comparison between observed and synthetic spectra, we found thatthese atomic lines could not help us identify some unknown bands around 350, 330 and 310 nm. The 350 nm
excess was particularly strong. As a result, the best account for two excess bands was found to be the “first negative B–X” band of the molecular nitrogen ion N+
2 (1–).
44

Figure2: Observed spectrum (blackline) compared with synthetic
spectrum considering atoms and molecules of N+
2 (1–) witha temperature of 10,000 K (redline) and 4400 K (blueline).
The dash-dotted lines indicate N+
2 (1–) at the appropriate temperature. The gray area near 310 nm shows OH A–X bands.
The origin of OH band will be needed for future confirmation.

Fig. 2 shows the model spectrum of N+
2 (1–) with fourbands heads (329.3, 353.4, 391.4, and 427.8 nm) causedby different vibrational states of (v’, v”) = (2, 0), (1, 0), (0,0), and (0, 1), respectively. The model spectrum is wonderfully in complete agreement with the observational spectrum in the UV range from 320 to 360 nm.
In general, meteor spectra consist of two components at
different temperatures [2]. A typical temperature of the“main (warm) component,” is T ∼ 4500 K. The “second(hot) component” is excited at T ∼ 10000 K and consistsof a few ionized elements such as Ca II and Mg II. A bestfit calculation mixed with atoms and molecules confirmed
2 +2 +the first discovery of N+
2 B Σu → X Σg bands in the UV
meteor spectrum. The N+
temperature
was estimated to be
2
10000 K with a low number density of 1.55 × 105 cm−3 .
Such unexpectedly strong ultraviolet emission, in particular for N+
2 (1, 0) at 353.4 nm, is supposed to be formed
through the wide dimensions of high-temperature regions
caused by a large meteoroid. Spectroscopic observations ofreentry capsules, such as Stardust (cometary dust sample
return in 2006 January), and Hayabusa (asteroidal material sample return in 2007 June), will provide us with good
opportunities for confirming the discovered N+
2.
References[1] Abe, S., et al.: 2005, ApJ, 618, L141.
[2] Borovička, J.: 1994, Planet. Space. Sci., 42, 145.

Progress and Status of the Development of the Band 4 Cartridge
RecieverASAYAMA, Shin’ichiro, IWASHITA, Hiroyuki, TAKAHASHI, Toshikazu, INATA, Motoko,
SUZUKI, Takakiyo, FUJII, Takuya, HARADA, Naohiko(NAOJ)

OGAWA, Hideo, KIMURA, Kimihiro, HARA, Kazuyoshi(Osaka Prefecture University)

SUZUKI, Kazuji(Technical Center of Nagoya University)

Figure1: Conceptual diagram of Band4 cartridge (left) and Band 4 prototype cartridge (right).

We have been developing the ALMA Band 4 cartridge
receiver. The Atacama Large Millimeter/submillimeter Array (ALMA) is an international collaboration between Europe, North America and Japan to build a synthesis radio
telescope that will operate at millimeter and submillimeter wavelengths. ALMA will be located on the Chajnantor
plain of the Chilean Andes in the District of San Pedro deAtacama, 5,000 meters above sea level. The ALMA receiver system will cover all the available atmospheric frequency windows between 30 GHz and 950 GHz. The range
shall be covered in 10 bands with HFET or SIS devices.
The receiver should be modular so that one easy to install
self-contained receiver should cover that one particular frequency band. These self-contained receivers are known as“cartridges.” The development and production of the Band
4 cartridge receivers is one portion of the Japanese in-kind
contribution to ALMA.
ALMA Band 4 will operate in the 125–163 GHz frequency band, which is 26 % bandwidth to the center frequency of 144 GHz. A conceptual diagram of the cartridge
and a photograph of the Band 4 prototype cartridge areshown in Fig. 1. The beam coming from the telescope isincident on a flat mirror, which reflects the beam out to an
elliptical mirror and then the beam is focused down into
the cryostat onto the horn. It is a dual polarization receiver,which uses an orthomode transducer (OMT) as a polarization splitter. The cartridge consists of three stages (at operating temperatures 4, 15, and 110 K) and the base-plate(which acts as a vacuum seal) at 300 K, with GFRP 10
spacers between them. The 110 K stage has the LO doublers mounted on it and heat sinks for the LO waveguide,
coax cables and wiring. The 15 K stage has only heat sinks
for the LO waveguide, coax cables and wiring attached.

Figure2: SSB noise temperature of ALMA band 4 2SB mixer with averaging over the IF band of 4–8 GHz.

The 4 K stage has the Corrugated horn, OMT, 2SB SIS
mixers, Cryogenic Isolators, Cryogenic HEMT Amplifiers(CLNAs), IF hybrids and heat sinks for the LO waveguide,
coax cable and wiring attached.
To meet the technical specification of the ALMA Band
4 receiver, Band 4 team has developed corrugated horn,
OMT, 2SB SIS mixer, etc.
The corrugated horn was fabricated by NC machining
suited for the series production. The measured beam patterns are consistent with the simulation down to a level of-30 dB relative to the center. The peak of cross polarization is lower than -30 dB relative to the peak of the co-polar
power, which is good.
The OMT has been designed and prototyped for Band 4
based on the double ridged waveguide-based design. Testsof the prototype OMT exhibit a return loss better than 18
dB and an insertion loss of less than - 0.5 dB across thefull 125 – 163 GHz band in both polarizations. This performance is excellent for a critical component in the Band
4 cartridge design.
The overall receiver noise temperatures of the 2SB
mixer with OMT (Horizontal Port) averaged over the IFband of 4–8 GHz are plotted in Fig. 2. Image rejection
ratio (IRR) was measured at IF = 6 GHz. The noise temperatures were corrected for the contribution of the image
sideband at IF center frequency 6 GHz. The noise performance includes the contribution of the vacuum window,
feed horn, OMT, and IF amplifier chain. The measured
single-sideband (SSB) receiver noise temperatures are lessthan 45 K and the image rejection ratios are better than 10
dB in the LO frequency range of 133–155 GHz. This result
is promising that the Band 4 cartridge will meet the noise
temperature specification.
45

The First Build-up of the Solar-B Flight Models
HARA, Hirohisa, ICHIMOTO, Kiyoshi, OTSUBO, Masashi, KATSUKAWA, Yukio, KATO, Yoshihiro
KANO, Ryohei, KUMAGAI, Kazuyoshi, SHIBASAKI, Kiyoto, SHIMIZU, Toshifumi
SHIMOJO, Masumi, SUEMATSU, Yoshinori, TAMURA, Tomonori, TSUNETA, Saku
NOGUCHI, Motokazu, NAKAGIRI, Masao, MIYASHITA, Masakuni, WATANABE, Tetsuya(NAOJ)KOSUGI, Takeo, SAKAO, Taro, MATSUZAKI, Keiichi(JAXA)KITAKOSHI, Yasunori, KUBO, Masahito, SAKAMOTO, Yasushi(Univ. of Tokyo)

Figure1: Telescope apertures of the flight model Solar-B spacecraft.
The Optical Telescope Assembly is at the center and its Focal Plane Package is on the left. X-ray Telescope and EUV
Imaging Spectrometer on the bottom and top are covered withblack baggings for protection from external contamination.

All flight models (FM) of Solar-B, the sun observing
spacecraft, gathered in a clean room of Institute of Spaceand Astronautical Sicnce of Japan Aerospace Exploration
Agency (ISAS/JAXA) in 2004 for the first integration andspacecraft-level testing. The Solar-B Project Office of
the National Astronomical Observatory of Japan (NAOJ)
largely contributes to the system design and spacecraftlevel testing of all telescopes, developments of the Optical
Telescope Assembly in the Solar Optical Telescope (SOT)and X-ray CCD camera of the X-ray Telescope (XRT), andthe spacecraft-level contamination control. From foreign
partners (US NASA and UK PPARC) the Focal Plane Package of SOT, XRT, and EUV Imaging Spectrometer weredelivered there. The primary purpose of the test was tocheck the specification and performance of the Solar-B FM
through the electrical and mechanical interface checks during the course of assembly and after the final assembly. In
addition, the SOT imaging performance was investigatedunder a disturbed environment in which the moving components in the spacecraft are steadily operating. Over a
half-year period of time the interface specification and performance of all telescopes ([1], [2], and [3]) were checkedin detail by the Solar-B Project Office of NAOJ together
with ISAS/JAXA and foreign partners.
The integration and testing of FM started in June and46

Figure2: Micro-vibration test configuration to measure a response of
the Optical Telescope Assembly for moving components inthe spacecraft that act as sources of disturbance.

the integrated spacecraft appeared at the beginning of Oct(Fig. 1). After the performance test of each subsystem was
successfully finished by the end of Nov, a test to evaluate
the effect of external disturbance to the diffraction-limited
imaging performance of SOT was carried out (Fig. 2).
From this test it was confirmed that the degradation of the
SOT imaging performance does not occur under the steady
disturbance from moving components in the spacecraft attitude control system and mechanical components in telescopes. Although sensitive CCD cameras as detectors are
exposed to a severe noise environment from the spacecraft
itself, it was also confirmed that the performace of Solar-B
detectors in telescopes is maintained under various spacecraft operational modes.
All testings were finished successfully, with only minor
problems uncovered, at the beginning of Dec. The spacecraft was de-integrated and each component was returned
to each institute or a contractor in charge. All components
are going to gather again in June 2005 after fixing problems
and finishing the environmental testing such as mechanicaland thermal vacuum tests. The Solar-B spacecraft is going
to be launched in summer 2006 from the Uchinoura Space
Center of JAXA in Kagoshima.
References[1] Shimizu, T.: 2004, ASP Conf. Ser., 325, 3.
[2] Kano, R., et al.: 2004, ASP Conf. Ser., 325, 15.
[3] Hara, H.: 2004, ASP Conf. Ser., 325, 27.

Discovery of evidence of the nucleosynthesis process byphotodisintegration reactions in supernova explosions
HAYAKAWA, Takehito

IWAMOTO, Nobuyuki, SHIZUMA, Toshiyuki(JAERI/NAO)(JAERI)

KAJINO, Toshitaka

UMEDA, Hideyuki, NOMOTO, Kenichi(University of Tokyo/NAO)(University of Tokyo)

Figure1: A partial nuclear chart. X-axis is the proton number and Yaxis is the neutron number. The p-nuclei are located in the
proton-rich side.

At the formation of the Galaxy, only the light elements
such as H, He existed, while heavy elements were dominantly produced by nuclear reaction processes in stars. The
solar system abundance is a record of these nucleosynthesis processes. About 99% of heavy elements are considered
to be synthesized by two neutron-capture reaction chains,r- and s-processes. Two abundance peaks near the neutron
magic number correspond to the r- and s-processes.
There are 35 p-nuclei that cannot be synthesized by theneutron-capture reactions. The p-nuclei are located in the
proton-rich side in the nuclear chart and their isotope ratios are small (typically 0.1 ∼ 1 %) as shown in Fig. 1.
The problem of the origin of the p-nuclei has been pointed
out about 50 years ago and many nucleosynthesis processes have been proposed to explain the origin of the pnuclei. They are nucleosynthesis by Cosmic-rays [1], Xray bursts of Type I in neutron stars [2], photodisintegration reactions in supernova (SN) explosions (p-process)[3],
neutrino-induced reactions in SNe [4], He detonations in
C/O white dwarfs [5]. In order to investigate the origin of
the p-nuclei, we study the solar system abundance.
There are 20 pairs of a p-nucleus and a pure s-nucleusthat is two neutron heavier than the p-nucleus (see Fig. 1).
The pure s-nucleus is dominantly produced by the sprocess and is shielded against the β-decay after the rprocess. 126 Xe has a p-nucleus and 128 Xe has a pure snucleus in Fig. 1. Taking the abundance ratios between thes- and p-nuclei, N(s)/N(p), we find an empirical scaling lawthat the abundance ratios, N(s)/N(p), are almost constantfor a wide range of the atomic number except some deviations (see Fig. 2)[6]. The deviations can be explained by

Figure2: The ratio of the s- and p-nuclei. X-axis is the atomic number.
The ratios are almost constant with the wide range.

the contamination of the s- and r-processes. We would liketo stress that this scaling has not been known.
The scaling indicates that the p-nuclei were synthesizedfrom the s-nuclei by nuclear reactions such as (γ,n) reactions. This is evidence that the most probable origin of
the p-nuclei is the p-process in SN explosions, because thenuclear reactions in the other processes change the proton
number of the seed nuclei as well as the neutron number.
We carry out nucleosynthesis calculations based on a
typical core-collapse SN model. The calculated ratios arealmost constant for a wide range, although the average values is lower than the observed ratios. These resutls are
consistent with the observed scaling in the solar system.
We therefore conclude that the scaling is evidence of the
p-process nucleosynthesis in SNe. This discovery is also
important for the study of the stellar environment where thenuclei are synthesized, and of the galactic chemical evolutions.
References[1] Audouze, J.: 1970, A&A, 8, 436.
[2] Schatz, H., et al.: 2001, PRL, 86, 3471.
[3] Arnould, M.: 1976, A&A, 46, 117.
[4] Woosley, S. E., et al.: 1990, ApJ, 356, 272.
[5] Howard, W. M., et al.: 1991, ApJ, 373, L5.
[6] Hayakawa, T., et al.: 2004, PRL, 93, 161102.

47

Start of regular geodetic VLBI observations within VERA network
JIKE, Takaaki, TAMURA, Yoshiaki, MANABE∗ , Seiji, KAWAGUCHI, Noriyuki,
IWADATE, Kenzaburo, KAMEYA, Osamu, KANYA, Yukitoshi, KUJI, Seisuke,
KOBAYASHI, Hideyuki, SAKAI, Satoshi, SATO, Katsuhisa, SHIBATA, Katsunori,
HIROTA, Tomoya, FUJII, Takahiro, HORIAI, Koji, HONMA, Mareki, MIYAJI, Takeshi,(VERA Observatory, NOAJ), (∗ Mizusawa Astrogeodynamics Observatory, NAOJ)OMODAKA, Toshihiro, IMAI, Hiroshi(Faculty of Science, Kagoshima University)
We succeeded first geodetic VLBI observations within
the VERA network in October 2004 using S/X band receivers and 1Gbps recording system. Also, we started regular geodetic VLBI observations twice a month within the
network from December 2004.
Since December 2001, Mizusawa Station joined domestic VLBI observations named JADE, which were coordinated by the Geographical Survey Institute (GSI), almost
once a month. These observations have been carried out
to tie the VERA network with the International Terrestrial
Reference Frame (ITRF) via Tsukuba Station of GSI. In
these observations, so-called K4 backend system was usedwhich was based on tape recording system of 128Mbps.
From March 2005, we introduced new disk recording system named K5/VSSP.
In the geodetic VLBI observations, we observed total
400 objects in 24 hours. We started the operation of Array Operation Center (AOC) in Mizusawa from October
2004. From the AOC, we can control VERA four stations
and reduce the operation loads at the sites.
As for the analysis software, we can obtain the station
coordinates, clock parameters and so on within one day after the correlation process was done at the Mitaka Correlation Center in NAOJ. In Fig. 1, the tentative analysis resultof the observation on December 17, 2004, is shown. The
baseline solutions might be change about a few mm when
the constraint conditions such as nutation parameters werechanged in the analysis.
The VERA project aims at measuring proper motions
and annual parallax of radio sources in the Galaxy by using relative VLBI observation technique. To realize themain target of the project, the accuracy of the coordinates
in VERA network should be in the order of 10−9 of baseline length, that is 1mm–2mm. The expected accuracy of
the geodetic observation on one time is 2mm in the horizontal position and 8mm in the vertical one (see Fig. 2).
Thus the regular geodetic observations are necessary to obtain required accuracy in the network coordinates.

48

Figure1: Tentative baseline lengths of the VERA network obtained
from the observations on December 17, 2004. The baseline
lengths vary momentarily because of the plate motions which
exceed 60mm per year at the maximum.

Figure2: A sample of error circle at the Iriki Station. The error of vertical position is larger then that of horizontal one, because theresolution among vertical position, clock parameter and atmospheric delay are poor in the parameter estimations.

Hemispheric Sign Rule of Magnetic Helicity on the Sun
HAGINO, Masaoki, SAKURAI, Takashi(Solar Observatory, NAOJ)
The activity cycle of the sun seen, e.g. in the eleven-year
periodicity of sunspot numbers, has been the topic of intensive research for many years. However, its driving mechanism is still not fully understood and is regarded as themost fundamental problem in solar-stellar physics. In thisrespect, attention has been paid recently on the twist of solar magnetic fields, because it provides new information on
how the magnetic fields are generated in the solar interior.
It has long been known that the whirl patterns aroundsunspots show hemispheric preferences, either clockwise
or counter-clockwise. A more recent finding with the soft
X-ray telescope of Yohkoh is that coronal loops also show
hemispheric segregation in twists (either S or inverted S
patterns). These properties can be interpreted as due totwisted magnetic tubes in the sun, which are left-handed in
the northern hemisphere and right-handed in the southernhemisphere (Fig. 1).

taka [1]. The slope is negative, namely the helicity is positive (negative) in the southern (northern) hemisphere. This
property, known as the hemispheric sign property, was discovered by the teams at University of Hawaii and at Beijing Observatory. Our analysis not only confirmed theirresults, but also added more confidence to it by carefully
scrutinizing the accuracy in the data and analysis methods.
The large dispersion in the data points seen in this figure
is not due to observational errors but is a real effect due
to turbulence which the magnetic tubes rising through theconvection zone have experienced.

Figure2: The latitude distribution of magnetic helicity αav derived for
230 active regions. The solid line is the least-square regression line, and two dotted lines show the error bounds in theslope.

Figure1: A schematic picture showing the twist of magnetic fields inthe interior of the sun, at the surface, and in the corona.

The twist of magnetic fields is quantitatively represented by ‘magnetic helicity’; positive helicity means righthanded helical fields. From observations of the magnetic
fields on the solar surface with the instrument called a vector magnetograph, we can derive the magnetic helicity byspatially averaging the quantity B · (∇ × B)/B 2 .
Figure 2 shows the latitude distribution of magnetic helicity derived from 230 active regions observed in the period of 1992–2001, with the Solar Flare Telescope at Mi-

We are investigating the time variability in the magnetic
helicity. It is already known that the hemispheric sign rule
does not change from one eleven-year cycle to the next.
There is, however, some indication of variability as a function of the phase in the activity cycle.

Reference[1] Hagino, M., and Sakurai, T.: 2004, PASJ, 56, 831.

49

Some Coronal Loops have Cooler Loop-Tops
SINGH, Jagdev(Indian Institute of Astrophysics)

SAKURAI, Takashi, ICHIMOTO, Kiyoshi(Solar Observatory, NAOJ)
The mechanism which brings the solar corona into a temperature of 1–2 million degrees is still unknown and is regarded as one of the most fundamental problems in astrophysics.
The temperature distribution along a coronal loop may
indicate important information on whether the heating isconcentrated at some portion of the loop or is more or lessuniformly distributed. Generally the heat conduction along
the length of the loop (namely along the field lines) is efficient and tends to make the temperature gradually decrease
toward the footpoint that is anchored to the cool solar surface. On the other hand if the heating is localized at thefoot portion of the loop, the temperature at the top of theloop may be less hotter, or even cooler, than the footpoint
regions. So far the observations in EUV and X-rays showthat the loops show the highest temperature at their tops.

However, the loops on the right-hand portion of the figure
showed a peculiar behavior (Fig. 2). There the widths ofthe two lines and the intensity ratio (Fe XI/Fe X) of the twolines decreased with height. The decrease in the line widths
alone might be interpreted as the decrease in the turbulent
line broadening (unresolved motions). However, because
the line intensity ratio also decreases with height, the observations are most consistently explained if the temperaturein these loops decreases with height.

Figure2: The height variations of spectral line widths and line intensity
ratio (Fe XI/Fe X). All of the three quantities are seen to decrease with height, which is possible only if the temperature
decreases toward the top of these loops.
Figure1: Coronal loops observed with a 25cm-aperture coronagraph at
Norikura Solar Observatory. The spectral lines used to obtainthese maps are [Fe XI] 7892 Å and [Fe X] 6374 Å. The loops
marked with + in the middle row showed a normal behavior
of increasing temperature with height. The loops marked with+ in the bottom row showed, on the contrary, a temperature
decreasing with height.

We have been conducting systematic studies of the solar corona by using the coronagraph and the spectrographat Norikura Solar Observatory. We found a rare case inwhich the coronal loop showed a temperature distribution
decreasing with height [1]. Figure 1 shows the observed
coronal region. These maps were made by observing the◦[Fe XI] 7892 A line emitted from a 1.3 MK plasma and the◦[Fe X] 6374 A line emitted from a 1.0 MK plasma. Manyloops in the central part of the figure showed a normal
behavior, namely the temperature increasing with height.
50

Our previous studies show that the distribution of temperatures in coronal loops is complicated. Generally a single temperature cannot explain the observations, and one
is forced to introduce multi-temperature components along
the line of sight. In the present example, however, the data
used were from two ions (Fe X and Fe XI) which are closein the ionization equilibrium temperatures. Therefore, we
can assume that we were looking at a plasma with an identical temperature, and the data really show the temperature
which decreases toward the top of the loop.
Reference[1] Singh, J., et al.: 2004, Asian J. Phys., 13, 245.

A CME onset observed with Norikura NOGIS coronagraph
HORI, Kuniko(NICT)ICHIMOTO, Kiyoshi, SAKURAI, Takashi, SANO, Issei, NISHINO, Yohei
and NOGIS team
(NAOJ Solar Observatory)◦

Figure1: Coronal disturbances on 2003 June 2.

We present the first detection of a coronal mass ejection (CME) in the coronal green-line emission (Fe XIV,
2MK) by the two-dimensional Doppler coronagraph NOGIS (Norikura Green-line Imaging System) at the Norikura
Solar Observatory.
CME is a huge expansion of magnetically trapped coronal plasmas that is usually associated with a local explosion
on the solar surface, such as flares and filament eruptions.
Birth places, shapes and expansion process of CMEs reflect global structure of the coronal magnetic fields. Observations of CME onsets can, therefore, provide valuable
information on coronal fields and surrounding plasmas thatare changing as a result of magnetic energy release. While
kinetic features of CMEs have been studied with whightlight coronagraphs [1], spectroscopic observations are essential for diagnosis of CME plasmas [2]. NOGIS is aunique imaging system that can provide both intensity andDoppler velocity images of 2MK plasma from the coronal◦green-line emission λ5303 A of Fe XIV [3]. NOGIS has afield of view of 2000 × 2000 pixels in a full frame mode
and a spatial resolution of 1. 84 in a partial frame mode.
The line-of-sight velocity of up to ±25km/s can be detectedwith an accuracy of 0.6 km/s. Since 1997, NOGIS has observed many flares and coronal waves. Here we introduce a
CME onset on 2003 June 2 that was continuously observedwith NOGIS in relatively good seeing conditions [4].
Figure 1 top panels show the event configuration aroundthe west limb. From left to right, a SOHO/EIT 195A (FeXII; 1.6MK) image, NOGIS intensity image (where the solar disk is occulted), and a sketch that summarizes the evolution of the event. The grid shows 5◦ (dotted line) and
0.1 Rs intervals (solid line). Solar North is up, and west
is to the right. Across the solar equator (thick horizontal line), there were two magnetic flux systems lying along
the limb: a flare-productive active region, NOAA #10365,
and a bundle of face-on coronal loops overarching a quiescent filament. The magnetic polarity of footpoints near
the equator is opposite in each flux system, which suggests a possible magnetic link between the two systems.
An early precursor of the event is a density enhancementof 2 MK plasma in between the two systems. Following
a filament eruption from AR 10365 that was observed by◦
TRACE spacecraft in the 195A passband (1.6 MK), NOGIS
observed a blue-shifted bubble and a red-shifted coronal
wave that almost simultaneously expanded from the boundary of AR 10365 and the overlying dense region. The wave
propagated toward the face-on loop system and triggereda damping oscillation in Doppler shifts among the adjacent loops within the system (Fig. 1 bottom). The blueshifted bubble propagated both inward and upward. The
inward motion triggered an M6.5 flare in AR 10365 while
the upward motion evolved into a partial halo CME that
had an angular extent covering the latitudinal range of thetwo flux systems. Different from typical CME disturbancesthat evolve within a single flux system with a bipolar arcade
on its center, our event proceeded via interaction, which
was presumably magnetic reconnection, between separatrices of the two flux systems.
As a future work, we are planning to combine NOGISwith spaceborn EUV imaging spectrometers, SOHO/CDS
and Solar-B/EIS to have a temperature diagnosis of CME
plasmas and coronal waves.
References[1] Yashiro, S., et al.: 2004, J. Geophys. Res. 109, A07105.
[2] Ciaravella, A., et al.: 2002, ApJ, 575, 1116.
[3] Ichimoto, K., et al.: 1999, PASJ 51, 383.
[4] Hori, K., et al.: 2005, ApJ, 618, 1001.

51

Completion of Solar-B/Optical Telescope Flight Model
SUEMATSU, Yoshinori, ICHIMOTO, Kiyosi, SHIMIZU, Toshifumi, OTSUBO, Masashi
NAKAGIRI, Masao, NOGUCHI, Motokazu, TAMURA, Tomonori, KATSUKAWA, Yukio
KATO, Yoshihiro, HARA, Hirohisa, MIYASHITA, Masakuni, TSUNETA, Saku.
(NAOJ)

KUBO, Masahito, SAKAMOTO, Yasushi(Univ. of Tokyo)
Integration and optical test of Optical Telescope Assembly (OTA) flight model of SOLAR-B Solar Optical Telescope (SOT) is completed in a clean room of NAOJ. The
aim of SOT is to provide data to investigate the physical coupling between the photosphere and the corona toultimately understand the mechanism of coronal dynamics and heating with the coordinated observations with XRay Telescope and EUV Imaging Spectrometer onboard
SOLAR-B. With SOT we will be able to continuously observe solar atmospheric structures, especially solar magnetic structures, with a diffraction-limited spatial resolution of 0.2 to 0.3 arcsec and a polarization accuracy better
than 10−3 ; these performances are difficult to realize withground-based instruments.
The SOT consists of two separate optical structures: theOptical Telescope Assembly (OTA) designed and manufactured in Japan and the Focal Plane Package (FPP) by
NASA, USA. The main structure of OTA is an aplanatic(coma aberration free) Gregorian telescope of a 50 cm effective aperture. The OTA is equipped with newly designed
optical components such as a heat dump and a secondary
field stop aluminum mirror with high reflectivity silver
coating and a temperature low-sensitive apochromatic collimataing lens unit with a UV/IR cut coating on the firstsurface. These components are indispensable to keep OTA
in moderate temperature and optical thermal deformation
small. The SOT has an active image stabilization system
consisting of correlation tracker (in FPP), tip-tilt mirror andits controller against satellite pointing jitter. A bench test
demonstrated the performance of 0.002 arcsec stabilization
with a cross over frequency of 14 Hz.
We had already demonstrated in the summer of 2004 thatthe initially assembled OTA has the diffraction limited performance in all observable wavelengths (388 – 668 nm).
Since then, the OTA experienced system-level mechanical and electrical interface test, final installation of thermal
equipments, and an acoustic test. The OTA also passed theopto-thermal and thermal cycling test in which it was exposed in the lowest temperature on-orbit for 24 hours; thetemperature of telescope envelope, primary and secondary
mirror went down to –45 degC, –15 degC, and –33 degC,
respectively. Then, we confirmed that the the optical performance of OTA has not changed through these activities,
keeping the diffraction-limited performance the same as ayear before. In addition to the optical tests, the top- and52side-door deployment were successfully demonstrated after the acoustic test. These doors protect inside of OTA
from contamination on the ground and during lift-off andtake a role of cold-traps of molecular contaminants on orbit before their deployments.
After completion in the end of June, 2005, the OTA
moved to ISAS/JAXA for system-level final performance
test before launch. The SOLAR-B is sheduled to be put ona solar synchronous polar orbit of altitude about 630 km in
the summer of 2006.

Figure1: SOLAR-B Optical Telescope prior to top- and side-door installation in NAOJ clean room.

Figure2: Top door deployment test of SOLAR-B Optical Telescope in
NAOJ clean room.

References[1] Ichimoto, K., et al.: 2004, SPIE, 5487, 1142-1151.
[2] Shimizu, T., et al.: 2004, SPIE, 5487, 1199-1206.

Generalized Horseshoes in the Standard Mapping
TANIKAWA, Kiyotaka(National Astronomical Observatory of Japan)

YAMAGUCHI, Yoshihiro(Teikyo Heisei University/National Astronomical Observatory of Japan)
The 2-fold horseshoe map introduced by Smale [1]shows the essence of chaos in the sense that the maximal
invariant set contained in the initial square exhibits sensitive dependence on initial conditions and transitivity. If asystem contains this horseshoe map as a subsystem, we canconclude that the system is chaotic and the lower bound for
topological entropy htop is equal to ln 2. Embedded 2-foldhorseshoes are found in many systems such as the Hénonmap [2] and the Duffing systems [3]. In general, if we findan embedded m-fold horseshoe for m ≥ 3 in the system,
we can say that the lower bound for topological entropy
is ln m. Such horseshoes are called the generalized horseshoes. McRobie–Thompson [4] analyzed the structure of
the idealized 3-fold (or ternary) horseshoe expected to exist in a periodically driven damped oscillator system. Gaspard [5] systematically analyzed classical hard-disk scatterers and proved the existence of 2-fold and 3-fold horseshoes, respectively for the three-disk and four-disk scatterers provided that all disks can be seen from each other.
The purpose of this paper [6] is to show how to construct(2n + 1)-fold horseshoes in the standard mapping T for
every n ≥ 1.
yn+1

= yn + a sin xn ,

(1)

xn+1

= xn + yn+1 (mod 2π)(2)Figure1: Three–fold horseshoe at a = 3π.

References[1] Smale, S.: 1967, Bull. Amer. Math. Soc., 73, 747.
[2] Hénon, M.: 1976, Commun. Math. Phys., 50, 69.
[3] Guckenheimer, J., and Holmes, P.: 1983, Nonlinear Oscillations, Dynamical Systems and Bifurcations of Vector Fields (Springer–Verlag).
[4] McRobie, F. A., and Thompson, J. M. T.: 1994, Dynam. Stab. Sys., 9,223.
[5] Gaspard, P.: 1998, Chaos, scattering and statistical mechanics (Cambridge University Press, Cambridge).
[6] Tanikawa, K., and Yamaguchi, Y.: 2005, Prog. Theor. Phys., 113,261-281.

where a > 0. The saddles are represented by P0,0 = (0, 0)
and P1,0 = (2π, 0).
Using the structure of the stable and unstable manifoldsof P0,0 and P1,0 , the existence of the three–fold horseshoe
at a ≥ 3π is proved (see Fig.1). This result can be extended
to the following theorem. The detailed proof is included in[6].
Theorem 1. In the standard mapping, for any n ≥ 1, a(4n−1)-fold horseshoe Ω4n−1 exists for a ≥ (8n−5)π anda (4n + 1)-fold horseshoe Ω4n+1 exists for a ≥ (8n − 1)π.
From Theorem 1, for example, at a = 11π, the coexistence of three different horseshoes Ω3 , Ω5 and Ω7 is derived. Then, the following relation holds.
Ω3 ⊂ Ω5 ⊂ Ω7 .

(3)

53

Metallic abundances of the 2002 Leonid meteor
deduced from visible - ultraviolet spectra
KASUGA, Toshihiro(Graduate University for Advanced Studies/NAOJ)

WATANABE, Juni-chi(Public Relations Center, NAOJ)

YAMAMOTO, Tetsuo(Hokkaido Univ.)(RIKEN)KAWAKITA, Hideyo

YANO, Hajime(Gunma Astron. Obs.)(ISAS/JAXA)

Spectroscopy of a large scale activity of the 2002 Leonid
meteor shower and a small scale activity of the 2004 June
Boötid meteor shower have been reported [1], [2].
Generally, meteor showers are originates from comets’dust and they enter the Earth’s atmosphere with their highvelocity. This results in the meteors reserving the importenergy into the atmosphere; thus the excitation plasma flashfrom the ablated meteoroids, can be appropriate to discuss the origin of solar system and its evolution process.
Composition of Comet dust is revealed to be almost samevalue of solar abundance by past Comet research. We havebeen focusing on spectroscopic observations of the meteor showers in the visible–ultraviolet region, where manylines of metallic atoms are expected, and carried out spectroscopy on the airborne mission (Fig. 1). Metallic abundances of meteors are slightly different from solar abundances and volatility feature of some element is clearlyshown by high-time resolved observation during its ablation process. Large scale meteoroids may show different
composition from that of comet dust with small scale. Thismay caused by the difference of their preserved area incomet. Otherwise, dust particles may be affected by a solar
heating during their orbital revolution as dust trail. It is aconsiderable result for formating non-condritic dust composition. This may cause a possible enhancement of affection on thermal history for pristine objects.
Meteor science will be a new method for exploring primitive objects.

54

EBIZUKA, Noboru

References[1] Kasuga, T., et al.: 2005, A&A 435, 341.
[2] Kasuga, T., et al.: 2004, A&A 424, L35.

Figure1: The 2002 Leonid spectrum. Observed on airborne mission.

II

Publications, Presentations

1. Refereed Publications
Abazajian, K., et al. including Ichikawa, S.: 2004, The
Second Data Release of the Sloan Digital Sky Survey,
Astron. J., 128, 502-512.
Abazajian, K., et al. including Ichikawa, S.: 2004, The Third
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Abbott, B., et al. including Kawamura, S.: 2004, Analysis of
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Abbott, B., et al. including Kawamura, S.: 2004, Analysis ofFirst LIGO Science Data for Stochastic Gravitational
Waves, Phys. Rev., D69, 122004.
Abbott, B., et al. including Kawamura, S.: 2004, First upper
limits from LIGO on gravitational wave bursts, Phys. Rev.,
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Abbott, B., et al. including Kawamura, S.: 2004, Setting
upper limits on the strength of periodic gravitational waves
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Abbott, B., et al. including Kawamura, S.: 2004, Detector
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Abe, S., Ebizuka, N., Yano, H., Watanabe, J., Borovicka,
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Akabane, K., and Kuno, N.: 2005, Dust Content in Compact
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Allen, B., et al. including Kawamura, S.: 2004, Upper limits
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Alonso-Herrero, A., Takagi, T., Baker, A. J., Rieke, G. H.,
Rieke, M. J., Imanishi, M., Scoville, N. Z.: 2004,
Obscured Star Formation in the Central Region of theDwarf Galaxy NGC 5253, Astrophys. J., 612, 222-237.
Alonso-Herrero, A., Pérez-González, P., Rigby, J., Rieke, G.,
Le Floc'h, E., Barmby, P., Page, M., Papovich, C., Dole,
H., Egami, E., Huang, J., Rigopoulou, D.,
Cristóbal-Hornillos, D., Eliche-Moral, C., Balcells, M.,
Prieto, M., Erwin, P., Engelbracht, C. W., Gordon, K. D.,
Werner, M., Willner, S. P., Fazio, G. G., Frayer, D., Hines,
D., Kelly, D., Latter, W., Misselt, K., Miyazaki, S.,
Morrison, J., Rieke, M. J., Wilson, G.: 2004, The Nature of
Luminous X-Ray Sources with Mid-Infrared Counterparts,
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Ambika, S., Parthasarathy, M., Aoki, W., Fujii, T., Nakada,Y., Ita, Y., and Izumiura, H.: 2004, Chemicalcomposition of UV-bright star ZNG 4 in the globularcluster M 13, Astron. Astrophys., 417, 293-300.
Ando, M., Arai, K., Nagano, S., Takahashi, R., Sato, S.,
Tatsumi, D., Tsunesada, Y., Kanda, N., Kawamura, S.,
Beyersdorf, P., Zhu, Zhong-Hong.., Numata, K., Iida, Y.,
Aso, Y., Mio, N., Moriwaki, S., Somiya, K., Miyoki, S.,

Kondo, K., Takahashi, H., Hayama, K., Tagoshi, H.,
Fujimoto, M-K., Tsubono, K., Kuroda K. and the TAMA
Collaboration: 2004, Analysis methods for burst
gravitational waves with TAMA data, Class. Quantum
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Ando, M., Arai, K., Takahashi, R., Tatsumi, D.,
Beyersdorf, P., Kawamura, S., Miyoki, S., Mio, N.,
Moriwaki, S., Numata, K., Kanda, N., Aso, Y., Fujimoto,
M-K., Tsubono, K., Kuroda, K. and the TAMA
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Ando, M., Ohta, K., Iwata, I., Watanabe, C., Tamura, N.,
Akiyama, M., and Aoki, K.: 2004, Lyman Break Galaxies
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Ao, Y., Yang, J., and Sunada, K.: 2004, 13CO, C18O, and CS
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Aoki, K., Kawaguchi, T., Ohta, K.: 2005, The Largest
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Quasars, Astrophys. J., 618, 601-608.
Aoki, W., Inoue, S., Kawanomoto, S., Ryan, S. G., Smith, I.
M., Suzuki, T. K., Takada-Hidai, M.: 2004, A low
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Aoki, W., Norris, J. E., Ryan, S. G., Beers, T. C., Christlieb,N., Tsangarides, S., Ando, H.: 2004, Oxygen
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Ariyoshi, S., Matsuo, H., Otani, C., Sato, H., Shimizu, H. M.,
Kawase, K., Noguchi, T.: 2005, Characterization of an
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Asai, A., Yokoyama, T., Shimojo, M., and Shibata, K.: 2004,
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Motions Associatedwith
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Baba, D., Nagata, T., Nagayama, T., Nagashima, C., Kato, D.,
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55

Direct Observation of Broadband Coating Thermal Noisein a Suspended Interferometer, Phys. Lett., A328, 1-5.
Brevik, I., Ghoroku K., and Yahiro, M.: 2004, Effective
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Broadhurst, T., Takada, M., Umetsu, L. Kong, X., Arimoto,N., Chiba, M., Futamase, T.: 2005, The Surprisingly Steep
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Boer, M., Dezalay, J.-P., Olive, J.-F., Hurley, K., Levine,A., Martel, F., Morgan, E., Woosley, S. E., Cline, T.,
Braga, J., Manchanda, R., Pizzichini, G.: 2005,
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an Off-Axis Gamma-Ray Burst?, Astrophys. J., 621,
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Chaplin, W. J., Sekii, T., Elsworth, Y. P., and Gough, D. O.:
2004, On the detectability of a rotation-rate gradient in thesolar core, MNRAS., 355, 535.
Chiba, T., and Sugiyama, N.: 2004, Does positronium formin the universe?, JCAP, 06, 003.
Cho, S.-H., Kim, H.-G., Park, Y.-S., Choi, C.-H., and Ukita,N.: 2005, First detection of 28Si18O Maser and Thermal
Emission from Orion KL, Astrophys. J., 622, 390-392.
Choi, M., Kamazaki, T., Tatematsu, K., and Panis, J.-F.:
2004, Structure of the Dense Molecular Gas in the NGC
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Deguchi, S., Fujii, T., Glass, I. S., Imai, H., Ita, Y.,
Izumiura, H., Kameya, O., Miyazaki, A., Nakada, Y.,
and Nakashima, J.: 2004, SiO Maser Survey of IRAS
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Deguchi, S., Imai, H., Fujii, T., Glass, I. S., Ita, Y.,
Izumiura, H., Kameya, O., Miyazaki, A., Nakada, Y.,
and Nakashima, J.: 2004, SiO Maser Survey of theLarge-Amplitude Variable in the Galactic Center, PASJ,56, 261-294.
Deguchi, S., Nakashima, J., and Takano, S.: 2004, Study of
the Bipolar Nebula IRAS 19312+1950. II. Circumstellar
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Deng, J., Kawabata, K. S., Ohyama, Y., Nomoto, K.,
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Hydrogen-rich, Asymmetric Circumstellar Medium,
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Dobashi, K., Uehara, H., Kandori, R., Sakurai, T., Kaiden,M., Umemoto, T., and Sato, F.: 2005, Atlas and Catalogof Dark Cluds Based on Digitized Sky Survey I, PASJ, 57,
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Dunlop, J. S., McLure, R. J., Yamada, T., Kajisawa, M.,
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56

counterpart of HDF 850.1, the brightest submillimetre
source in the Hubble Deep Field, MNRAS, 350, 769-784.
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Pérez-Gonzalez, P., Le Floc'h, E., Papovich, C., Barmby,
P., Ivison, R. J., Serjeant, S., Mortier, A., Frayer, D. T.,
Rigopoulou, D., Lagache, G., Rieke, G. H., Willner, S.,
Alonso-Herrero, A., Bai, L., Engelbracht, C., Fazio, G.,
Gordon, K. D., Hines, D., Misselt, K., Morrison, J., Rieke,
M. J., Rigby, J. R., Wilson, G.: 2004, Spitzer Observationsof the SCUBA/VLA Sources in the Lockman Hole: Star
Formation History of Infrared-Luminous Galaxies,
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Enoki, M., Inoue, K. T., Nagashima, M. and Sugiyama, N.:
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Enoki, M., Inoue, K. T., Sugiyama, N., and Nagashima, M.:
2004, Gravitational Background Radiation fromSupermassive Black Hole Coalescence, Stellar-Mass,
Intermediate-Mass, and Supermassive Black Holes, Prog.
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Fujita, Y., and Goto, T.: 2004, The Evolution of Galaxies inand around Clusters at High-Redshift, PASJ, 56, 621-631.
Fujita, Y., and Reiprich, T.-H.: 2004, Can Supermassive
BlackHoles Sufficiently Heat Cool Cores of Galaxy
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Turbulence in the Cool Cores of Galaxy Clusters: Can
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Fujita, Y., Matsumoto, T., Wada, K., and Furusho, T.: 2005,
Simulating Astro-E2 Observations of Galaxy Clusters: The
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J., 619, L139-L142.
Fujita, Y., Sarazin, C.-L., Reiprich, T.-H., Andernach, H.,
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XMM-Newton Observations of A133: A Weak Shock
Passing through the Cool Core, Astrophys. J., 616,
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Fujiyoshi, T., Smith, C., Moore, T., Lumsden, S., Aitken, D.,
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356, 801-809.
Fukagawa, M., Hayashi, M., Tamura, M., Itoh, Y.,
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Fukushima, T.: 2004, Efficient Orbit Integration by Linear
Transformation for Consistency of Kepler Energy, Laplace
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Yamauchi, Y., Moore, R. L., Suess, S. T., Wang, H., andSakurai, T.: 2004, The Magnetic Structure of HαMacrospicules in Solar Coronal Holes, Astrophys. J., 605,
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Yamazaki, D. G., Ichiki, K., and Kajino, T.: 2005,
Constraining Primordial Magnetic Field from CMB
Anisotropies at Higher Multipoles, Astrophys. J. Lett., 625,
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Yanagisawa, T., Nakajima, A., Kadota, K., Kurosaki, H.,
Nakamura, T., Yoshida, F., Dermawan, B., Sato, Y.:
2005, Automatic detection algorithm for small moving
objects, PASJ, 57, 399-408.
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T.,
Nakajima, T., Hanada, H., Kan-ya, Y., Yamada, Y.,
Araki, H., Tazawa, S., Araki, K., Tsuruta, S., Kawano,N.: 2004, CCD Centroiding Experiment for the Japanese
Astrometry Satellite Mission (JASMINE) and In Situ
Lunar Orientation Measurement (ILOM), PASJ, 116,
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Yano, T., Koyama, H., Buchert, T., and Gouda, N.: 2004,
Universality in the Distribution of Caustics in the
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Yoshida, F., Dermawan, B., Ito, T., Sawabe, Y., Haji, M.,
Saito, R., Hirai, M., Nakamura, T., Sato, Y., Yanagisawa,T., Malhotra, R.: 2004, Photometric Observations of a
Very Young Family-Member Asteroids (832) Karin, PASJ,56, 1105-1113.
Yoshida, F., Nakamura, T.: 2004, Basic Nature of Sub-km
Main-Belt Asteroids: Their size and Spatial Distributions,Adv. Space Res., 33, 1543-1547.
Yoshida, H., Nakamura, K., Omote, M.: 2005, The
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Yoshida, M., Ohyama, Y., Iye, M., Aoki, K., Kashikawa,N., Sasaki, T., Shimasaku, K., Yagi, M., Okamura, S., Doi,
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3653-3653.
Yoshida, T., Terasawa, M., Kajino, T., and Sumiyoshi, K.:
2004, Nucleosynthesis of Light Elements and Heavyr-Process Elements through the n-Process in Supernova
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Yoshii, Y., Kobayashi, Y., Minezaki, T.: 2004, The dust
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Astronomische
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Young, K. H., Hunter, T. R., Wilner, D. J., Gurwell, M. A.,
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Matsushita, S., Moran, J. M., Ohashi, N., Papa, D. C.,
Patel, N., Patt, F., Peck, A., Qi, C., Saito, M., Schinckel,
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2. Publications of the National Astronomical
Observatory of Japan
Toda, M., Yamamoto, M.-Y., Higa, Y., Watanabe, J.-I.:
2004, Catalogue of persistent trains I: meteor train images
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3. Report of the National Astronomical Observatory ofJapan
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Yano, T., Takato, N., Kobayashi, Y., and Gouda, N.: 2004,
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Ito, S.: 2004, Scholastic Intercourse between Shogunal
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Wada, S., Maihara, T., Hirata, R. Ohta, K., Iwamuro, f.,
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Koyano, H., Yoshida, M., Okita, K., Okuda, T.,
Izumiura, H., Shimizu, Y., Inata, M., Yanagisawa, K.,
Nagawayama, S., Hattori, T., Tamura, N., and Mikami,
Y.: 2004, Astronomical Evaluation of OAO: Site Researchon Surface Boundary Layer of Air, Rep. Nat. Astron. Obs.
Japan, 7, 29-39.
Yamada, Y., Ueda, S., Kuwabara, T., Yano, T., and Gouda,N.: 2004, JASMINE Simulator -Construction of
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Enoki, M., Taga, M., Ozawa, T., Noda, S., Okumura, S.,

Yoshino, A., Furusho, R., Baba, H., Horaguchi, T.,
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Public Science Archive System of Subaru Telescope 3,
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4. Other Publications
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AE Aquarii emission processes from radio to infrared, The
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Objects, Eds. J.-M. Hameury and J.-P. Lasota. San
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Aoki, W.: 2004, Measurements of Li and Eu isotope
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Asada, K., Inoue, M.: 2004, A follow-up RM observation
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Asai, A., Ichimoto, K., Shibata, K., Kitai, R., and Kurokawa,
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Asai, A., Shibata, K., Yokoyama, T., Shimojo, M.: 2004,
Downflow as a Reconnection Outflow, Eds. T. Sakurai and
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Asai, A., Yokoyama, T., Shimojo, M., and Shibata, K.: 2004,
Downflow as a Reconnection Outflow, Proc. of the 5thSolar-B Science Meeting, "The Solar-B Mission and theForefront of Solar Physics: Dedicated to the Memory of
Yutaka Uchida", ASP Conf. Ser., 325, 361-366.
Asai, A., Yokoyama, T., Shimojo, M., Masuda, S., andShibata, K.: 2004, Flare Ribbon Expansion and Energy
Release Rate, "Multi-Wavelength Investigations of Solar
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Asai, A.: 2004, Flare Associated Oscillations Observed with
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Asayama, S.: 2004, Sideband-Separating SIS Mixer at
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Barkin, Y., Gusev, A., and Petrova, N.: 2004, Modern
investigation of spin-orbital and interior dynamics of theMoon, Proc. Int. conf. "Modern direction of astronomical
evolution in Russia", 263-268.
Carter, M. C., Baryshev, A., Harman, M., Lazareff, B., Lamb,J., Navarro, S., John, D., Fontana, A.-L., Ediss, G., Tham,
C. Y., Withington, S., Tercero, F., Nesti, R., Tan, G-H.,
Sekimoto, Y., Matsunaga, M., Ogawa, H., Claude, S.:
2004, ALMA front-end optics, SPIE, 5489, 1074-1084.
Choudhary, D. P., Balasubramaniam, K. S., Suematsu, Y.:
2004, Asymmetric Stokes-V Profiles at the Penumbral
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Conf. Ser., 325, 137.
Ebizuka, N., Oka, K., Yamada, A., Ishikawa, M., Kashiwagi,
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Ezawa, H., Kawabe, R., Kohno, K., and Yamamoto, S.:
2004, The Atacama Submillimeter Telescope Experiment(ASTE), SPIE, 5489, 763-772.
Fujita, Y., Matsumoto, T., and Wada, K.: 2004, Turbulence
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Gelfreikh, G. B., Shibasaki, K., Nagovitsyna, E. Yu., andNagovitsyn, Yu. A.: 2004, Analysis of Quasi-Periodic
Oscillations of Position and Brightness of Details of theRadio Sources of the Solar Active Regions Based on
Observations Made with the Radio Heliograph Nobeyama,"Multi-Wavelength Investigations of Solar Activity", ed.
A.V. Stepanov, E. E. Benevolenskaya and A. G.
Kosovivhev, Proc. IAU Symp., 223, 245-246.
Gouda, N., Yano, T., Yamada, Y., Kobayashi, Y.,
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Japan Astrometry Satellite Mission for Infrared
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Grechnev, V. V,, Borovik, V. N., Bugaenko, O. I., Bogachev,
S. A., Grigorieva, I. Y., Kuzin, S. V., Lesovoi, S. V.,
Livshits, M. A., Pertsov, A. A., Rudenko, G. V., Slemzin,
V. A., Stepanov, A. I., Shibasaki, K., Uralov, A. M.,
Zandanov, V. G., and Zhitnik, I. A.: 2004, Observations ofa posteruptive Arcade on October 22, 2001 with the
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Gusev, A., and Kitiashvili, I.: 2004, Modeling of pulsar'
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Gusev, A., Kawano, N., and Petrova N.: 2005, Fine
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Gusev, A., Kawano, N., and Petrova, N.: 2004, Modeling of
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Haba, A., Kameno, S., Sawada-Satoh, S., and Sato, N.:
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W3(OH) by VLBI annual parallax measurement, Proc. 7th
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Hachisuka, K., Miyoshi, M.: 2004, Towards anUnderstanding of the Dynamics of the Milky Way, How
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Hagino, M., Sakurai, T., and Miyazawa, A.: 2004, Phase
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Solar Physics, Eds. T. Sakurai and T. Sekii, ASP Conf. Ser.,
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Hanaoka, Y.: 2004, Hα Impact Polarization Observed in a
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325, 347-352.
Hara, H., Nakakubo-Morimoto, K.: 2004, Variation of the
X-ray Bright Point Number over the Solar Activity Cycle,
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Hara, H.: 2004, Solar-B EUV Imaging Spectrometer (EIS),
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Harada, Y. and Kurita, K.: 2004, The Effect of theNon-synchronous Rotation on the Surface Stress ofEuropa: Constraints for the Rotation Period and theSurface Viscosity, Proc. 37th ISAS Lunar and PlanetarySymp., 37, 196-199.
Hayakawa, T., Shimizu, T., Arima, T., Kajino, T., Chiba, S.,
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Takami, H., Takato, N., Colley, S., Eldred, M., Kane, T.,
Guyon, O., Oya, S., Watanabe, M., Hattori, M., Goto,
M., Kobayashi, N., Minowa, Y., Saito, N., Akagawa, K.,
Wada, S.: 2004, Design of laser systems for Subaru LGS
AO, SPIE, 5490, 1088-1095.
Hirabayashi, H., Murata, Y., Edwards, P. G., Asaki, Y.,
Mochizuki, N., Inoue, M., Umemoto, T., Kameno, S.,
and Kono, Y.: 2004, On the Near-Term Space VLBI
Mission VSOP-2, Proc. 7th Symp., European VLBI
Network on New Developments in VLBI Science andTechnology, Eds. R. Bachiller, F. Colomer, J.-F. Desmurs,
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Honda, S., Aoki, W., Kajino, T., Ando, H., Beers, T. C.:
2004, Spectroscopic Studies of r-Process Elements in Very
Metal-Poor Stars with Subaru/HDS, proc. Origin of matterand evolution of galaxies, Eds. Terasawa M., et al., 440.
Honma, M., Bushimata, T., Choi, Y. K., Fujii, T., Hirota,
T., Horiai, K., Imai, H., Inomata, N., Ishitsuka, J. K.,
Iwadate, K., Jike, T., Kameya, O., Kamohara, R.,
Kan-Ya, Y., Kawaguchi, N., Kobayashi, H., Kuji, S.,
Kurayama, T., Manabe, S., Miyaji, T., Nakagawa, A.,
Nakashima, K., Omodaka, T., Oyama, T., Sakai, S., Sato,K., Sasao, T., Shibata, K. M., Shimizu, R., Sora, K., Suda,
H., Tamura, Y., and Yamashita, K.: 2004, Astrometry of
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Hori, K., Ichimoto, K., Sakurai, T., Nishino, Y., andNOGIS Team: 2004, Flare-Induced Coronal Disturbances
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Huang, G., and Nakajima, H.: 2005, Location andParameters of a Microwave Millisecond Spike Event,
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Ichiki, K., and Nakamura, K.: 2004, Stochastic
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and Gravitation in Japan, 462-465.
Ichiki, K., Garnavich, P., Kajino, T., Mathews, G. J., andYahiro, M.: 2004, 6th RESCEU Int. Symp., Frontier in
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Ichimoto, K., Tsuneta, S., Suematsu, Y., Shimizu, T.,
Otsubo, M., Kato, Y., Noguchi, M., Nakagiri, M.,
Tamura, T., Katsukawa, Y., Kubo, M., Sakamoto, Y.,
Hara, H., Minesugi, K., Ohnishi, A., Saito, H., Kawaguchi,N., Matsushita, T., Nakaoji, T., Nagae, K., Sakamoto, J.,
Hasuyama, Y., Mikami, I., Miyawaki, K., Sakurai, Y.,
Kaido, N., Horiuchi, T., Shimada, S., Inoue, T., Mitsutake,M., Yoshida, N., Takahara, O., Takeyama, H., Suzuki, M.,
Abe, S.-I.: 2004, The Solar Optical Telescope onboard theSolar-B, SPIE, 5487, 1142-1151.
Imanishi, M.: 2004, Buried AGNs in LINER Ultraluminous
Infrared Galaxies, The Neutral ISM in Starburst Galaxies,
ASP Conf. Ser., 320, 266-268.
Imanishi, M.: 2004, Compact Nuclear Starbursts in the CfA
and 12 micron Seyfert 2 Galaxies, The Neutral ISM in
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Inoue, M.: 2004, East Asian VLBI Activities, Proc. 7th
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Ishiguro, M., Tholen, D. J., Hasegawa, S., Abe, M.,
Sekiguchi, T., Ostro, S. J. and Kaasalainen, M.: 2005,
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M., Tsuboi, M., Ohishi, M., Fujisawa, K., Kasuga, T.,
Miyazawa, K., and Horiuchi, S.: 2004, A 32 m Parabolic
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European VLBI Network on New Developments in VLBI
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Iye, M., Kashikawa, N., Imanishi, M., Kodama, T., Chiba,
M., Shimasaku, K., Okamura, S., Miyazaki, S., Simpson,C., Kobayashi, N., Terada, H., Goto, M., Iwamuro, F.:
2004, ERO R1 in the field of CL0939+4713 - Evidence for
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Iye, M.: 2004, Concept study of Japan Extremely Large
Telescope, SPIE, 5489, 417-428.
Iye, M.: 2004, ERO R1 in CL0939+4713 - An Evidence for
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Iye, M.: 2004, Japan's Future Planning of Optical/Infrared
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Iye, M.: 2004, Subaru Instrumentation: Today andTomorrow, SPIE, 5492, 23-34.
Jain, R., Katsukawa, Y., Tsuneta, S., Vekstein, G.: 2004,
Heating of the Atmosphere, Nanoflares and Coronal
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Kamata, Y., Miyazaki, S., Muramatsu, M., Suzuki, H.,
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2004, Development of thick back-illuminated CCD to
improve quantum efficiency in optical longer wavelength
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Kameno, S., Inoue M., Shen, Z.-Q., Sawada-Satoh, S.,
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2004, Solar-B X-Ray Telescope (XRT), Eds. T. Sakurai
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Kashiwagi, M., Oka, K., Yamada, A., Ebizuka, N., Iye, M.,
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Katsukawa, Y., Tsuneta, S.: 2004, Multi-Temperature
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Kawabata, K. S., Maeda, K., Deng, J., Nomoto, K., Mazzali,
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Kobayashi, K., Otsubo, M., Suematsu, Y., Kumagai, K.,
Noguchi, M., Tamura, T., Nakagiri, M.: 2004, Imagestabilization system on SOLAR-B Solar Optical Telescope,
SPIE, 5487, 1189-1198.
Shimizu, T.: 2004, Solar-B Solar Optical Telescope (SOT),
Eds. T. Sakurai and T. Sekii, ASP Conf. Ser., 325, 3.
Shimojo, M.: 2004, Derivation of DEM distribution Using
YOHKOH/SXT, Proc. 5th Solar-B Science Meeting, The
Solar-B Mission and the Forefront of Solar Physics:
Dedicated to the Memory of Yutaka Uchida, ASP Conf.
Ser., 325, 313-318.
Shimojo, M.: 2004, NoRH Observations of Prominence
Eruptions, Proc. CD of the Nobeyama Symp. 2004, Solar
Physics with the Nobeyama Radioheliograph, JSPS
international meeting ser.
Shirasaki, Y., Mizumoto, Y., Ohishi, M., Yasuda, N.,
Tanaka, M., Honda, S., Yahagi, H., Nagashima, M.,
Kosugi, G., Kashikawa, N., Matsuzaki, E., Kakimoto, F.,
Ogio, S.: 2004, Searching for a cosmic string through thegraviational lens effect: Japanese Virtual Observatory
science use case, Astron, Data Analysis Software andSystems (ADASS) XIII, ASP Conf. Proc., 314, 46.
Shirasaki, Y., Ohishi, M., Mizumoto, Y., Tanaka, M.,
Honda, S., Oe, M., Yasuda, N., Masunaga, Y.: 2004,
Structured Query Language for Virtual Observatory
Astronomical Data Analysis Software and Systems XIV
P1-1-23, ASP Conf. Ser., XXX, 2005.
Shirley, Y. L., Wootten, A., Johnstone, D., Tatematsu, K.,
and Brogan, C.: 2004, Probing the Physical Conditions ofHigh-Mass Star-forming Cores with Dust Continuum andMolecular Ions, American Astronomical Society Meeting,205, #98.01.
Singh, J., Sakurai, T., Ichimoto, K., and Watanabe, T.:
2004, Spectroscopic Studies of Steady Coronal Structures Line Width Variations with Height of Fe X-XIV Emission
Lines, The Solar-B Mission and the Forefront of Solar
Physics, Eds. T. Sakurai and T. Sekii, ASP Conf. Ser., 325,
235-240.
Sôma, M., Hayamizu, T., Setoguchi, T., Hirose, T.: 2004,
Precise Position of Saturn Obtained from a Stellar
Occultation by Tethys, in Journées 2003, Astrometry,
Geodynamics and Solar System Dynamics: frommilliarcseconds to microarcseconds, Eds. A. Finkelsteinand N. Capitaine, 292-293.
Sôma, M., Tanikawa, K., Kawabata, K.: 2004, Earth's Rateof Rotation between 700 BC and 1000 AD Derived from
Ancient Solar Eclipses, in Journées 2003, Astrometry,
Geodynamics and Solar System Dynamics: frommilliarcseconds to microarcseconds, Eds. A. Finkelsteinand N. Capitaine, 122-127.
Sôma, M.: 2004, V5114 SAGITTARII, IAU Circ., 8316.
Sridharan, T. K., Saito, M., Patel, N., Christensen, R.: 2004,
Holographic surface setting of the Sub-millimeter Arrayantennas, SPIE, 5489, 441-446.
Stepanov, A. V., Kopylova, Yu. G., Tsap, Yu. T., Shibasaki,K., Melnikov, V. F., and Goldvarg, T. B.: 2004,
Diagnostics of Flare Plasma Using Pulsations in73

microwave and X-Ray Emission, Proc. CD of the
Nobeyama Symp. 2004, Solar Physics with the Nobeyama
Radioheliograph, JSPS international meeting ser.
Sugimoto, M., Koda, J., Hasegawa, T., Sawada, T., Handa,
T., Yamamoto, F., and Naito, S.: 2004, High Resolution
Survey of Molecular Clouds in and Between the Galactic
Spiral Arms, Milky Way Surveys: The Structure andEvolution of our Galaxy, Eds. D. Clemens, R. Shah, and T.
Brainerd, ASP Conf. Ser. 317, 88-90.
Suzuki, I., and Uchida, Y.: 2004, Observation of Two
Different Types of Coronal Mass Ejections, The Solar-B
Mission and the Forefront of Solar Physics, Eds. T.
Sakurai and T. Sekii, ASP Conf. Ser., 325, 421-426.
Suzuki, M., Kawai, N., Yoshida, A., Shirasaki, Y.,
Matsuoka, M., Tamagawa, T., Torii, K., Sakamoto, T.,
Graziani, C., Lamb, D. Q., Atteia, J. L., Fenimore, E. E.,
Galassi, M., Donaghy, T., Ricker, G., Doty, J., Vanderspek,
R., Crew, G. B., Villasenor, J., Butler, N., Jernigan, J. G.,
Barraud, C., Boer, M., Dezalay, J.-P., Olive, J.-F., Hurley,
K., Woosley, S. E., Hete-2 Science Team: 2004, Durationsof Gamma-ray Bursts and X-Ray Flashes in X-ray andGamma-Ray Bands Observed with HETE-2 Gamma-Ray
Bursts: 30 Years of Discovery: Gamma-Ray Burst Symp..
AIP Conf. Proc., 727, 217-220.
Tajitsu, A., and Otsuka, M.: 2004, The Multiple Outflows
in the Galactic Halo PN H4-1, Asymmetrical Planetary
Nebulae III: Winds, Structure and the Thunderbird, ASP
Conf. Ser., 313, 202-205.
Takagi, S.-I., Tsuru, T. G., Matsumoto, H., Koyama, K.,
Tsunemi, H., Miyata, E., Miyazaki, S., Kamata, Y.,
Miyaguchi, K., Muramatsu, M., Suzuki, H.: 2004, The
development of back-supportless CCDs and the wideband
hybrid X-ray imager for the NeXT satellite, SPIE, 5501,
101-110.
Takami, H., Watanabe, M., Takato, N., Colley, S., Eldred,M., Kane, T., Guyon, O., Hattori, M., Goto, M., Iye, M.,
Hayano, Y., Kamata, Y., Arimoto, N., Kobayashi, N.,
Minowa, Y.: 2004, Laser guide star AO project at theSubaru Telescope, SPIE, 5490, 837-845.
Takami, M., Bailey, J., Chrysostomou, A., Tamura, M.,
Terada, H.: 2004, Probing AU-scale Structure using
Spectro-Astrometry, Star Formation at High Angular
Resolution, IAU Symp., 221, 417.
Takasaki, H., Kiyohara, J., Asai, A., Yokoyama, T.,
Nakajima, H., Masuda, S., Sato, J., and Kosugi, T.: 2004,
The Spatially Resolved Spectrum Analysis of Gradual
Hardening Flare, Proc. CD of the Nobeyama Symp. 2004,
Solar Physics with the Nobeyama Radioheliograph, JSPS
international meeting ser.
Takato, N., Miyagawa, R., Shigemori, K., Iye, M., Okita,K., Miyashita, A., Sasaki, T., Usuda, T., Sonoda, M.,
Kubota, H.: 2004, An experiment for developing a
microcrack detection system for large thin mirror,
Ground-based Instrumentation for Astronomy. Eds. by A.
F. Moorwood, M. Iye, SPIE, 5495, 652-659.
Tamura, M., Fukagawa, M., Hayashi, M., The
SDPS/CIAO Teams: 2004, Subaru AO Coronagraphic andDirect Imaging of YSOs, Star Formation at High Angular
Resolution, IAU Symp., 221, 313.
Tamura, M., Ojha, D., SIRIUS/ASTRO-F Star Formation
Teams: 2004, Luminosity Functions of YSO Clusters in
74

Star Forming Regions: NIR and MIR Surveys, The
Formation and Evolution of Massive Young Star Clusters,
ASP Conf. Ser., 322. 389.
Tanaka, M., Kodama, T.: 2004, PISCES: Galaxy Properties
as Functioons of Enviroment and time, Baryons in Dark
Matter Halos, Eds. R. Dettmar, U. Klein, P. Salucci, 48.
Tanaka, M., Mizumoto, Y., Ohishi, M., Shirasaki, Y.,
Honda, S., Yasuda, N., Masunaga, Y., Ishihara, Y., Abe,K., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.,
Yoshida, T., and Morita, Y.: 2004, Development of theJapanese
VirtualObservatory(JVO)
prototype
Ground-based Telescopes, SPIE, 5493, 286-293.
Tanaka, M., Mizumoto, Y., Ohishi, M., Shirasaki, Y.,
Honda, S., Yasuda, N., Masunaga, Y., Ishihara, Y., Abe,K., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.,
Yoshida, T., Morita, Y.: 2004, Development of theJapanese Virtual Observatory (JVO) prototype, DBSJ
Letter, 3, 1.
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.: 2004, Japanese Virtual
Observatory (JVO) prototype 2 Astronomical Data
Analysis Software and Systems XIV P1-1-24, ASP Conf.
Ser., XXX, 2005.
Taniguchi, M., Sekiguchi, T., Itoh, Y. and Mukai, T.: 2005,
Photometry and Spectroscopy of TNOs with the Subaru
Telescope, 35th COSPAR Scientific Assembly., 3473.
Terasawa, M., Langanke, K.-H., Kajino, T., and Mathews, G.
J.: 2005, Neutrino effects before during and after thefreezeout of the r-process, Proc. Origin of Matter and
Evolution of Galaxies, 293-303.
Tomisaka, K., Machida, M. N., Matsumoto, T., Saigo, K.:
2004, Numerical Simulations of Collapse andFragmentation of Magnetized Molecular Cloud Cores Formation of Binary Systems, Gravitational Collapse:
From Massive Stars to Planets, Revista Mexicana de
Astronomía y Astrofísìca (Serie de Conferencias), 22,
18-21.
Tsujimoto, T., Shigeyama, T.: 2004, Histories of the Milky
Way Dwarf Spheroidal Galaxies and omega Centauri, The
Carnegie Observatories Centennial Symposia,
Originand
EvolutionoftheElements,
http://www.
ociw.edu/ociw/symposia/series/symposium4/proceedings.html.
Tsujimoto, T., Shigeyama, T.: 2004, Mass Stripping in
Dwarf Spheroidal Galaxies and omega Cen, IAU Sympo.,
217, 384.
Tsujimoto, T., Yamada, Y., Gouda, N.: 2005, Statistical
Methods for Calibrating Trigonometric Parallaxes, Proc.
Symp. The Three-Dimensional Universe with GAIA,
719-722.
Tsuneta, S., Katsukawa, Y.: 2004, Coronal Heating with
Sweet-Parker Picoflares, Eds. T. Sakurai and T. Sekii, ASP
Conf. Ser., 325, 289.
Tsuneta, S., Miyazaki, S., Nakaya, H., Yamada, T., Iye, M.,
Kaifu, N., Taniguchi, Y., Doi, M., Okamura, S., Ikeda, Y.,
Takeyama, N., Kaido, N., Yamaguchi, K., Norman, C.,
Ford, H., Kruk, J., Ouchi, M., Woodruff, R.: 2004, Very
Wide Field Imager(VWFI) for the Hubble Origins
Probe(HOP), AAS Meeting, 205, #100.03.

Ueda, A., Sekimoto, Y., Ishiguro, M., Asayama, S.,
Yamada, M., Noguchi, T.: Evaluation of a commerciallyavailable high efficiency Photomixer, ALMA Memo, 516.
Uehara, M., Nagashima, C., Sugitani, K., Watanabe, M.,
Sato, S., Nagata, T., Tamura, M., Ebizuka, N., Pickles, A.
J., Hodapp, K. W., Itoh, Y., Nakano, M., Ogura, K.: 2004,
Development of the Wide Field Grism Spectrograph 2,
SPIE, 5492, 661-668.
Ukita, N., Saito, M., Ezawa, H., Ikenoue, B., Ishizaki, H.,
Iwashita, H., Yamaguchi, N., Hayakawa, T., and the
ATF-J team: 2004, Design and Performance of the
ALMA-J Prototype Antenna, SPIE, 5489, 1085-1093.
Vanderspek, R., Butler, N., Crew, G. B., Dullighan, A.,
Prigozhin, G., Doty, J. P., Villasenor, J. N., Ricker, G. R.,
Tamagawa, T., Torii, K., Kawai, N., Sakamoto, T., Sato,R., Suzuki, M., Urata, Y., Yamamoto, Y., Yoshida, A.,
Nakagawa, Y. E., Yamazaki, T., Shirasaki, Y., Graziani,
C., Donaghy, T., Lamb, D. Q., Jernigan, J. G., Hurley, K.,
Atteia, J.-L., Fenimore, E. E., Galassi, M.: 2004, Current
Status of HETE-2 Operations, Gamma-Ray Bursts: 30
Years of Discovery: Gamma-Ray Burst Symp.. AIP Conf.
Proc., 727, 630-636.
Vanderspek, R., Dullighan, A., Butler, N., Crew, G. B.,
Villasenor, J. N., Ricker, G. R., Tamagawa, T., Sakamoto,T., Suzuki, M., Shirasaki, Y., Yamazaki, T., Hurley, K.,
Graziani, C., Donaghy, T., Lamb, D. Q., Barraud, C.,
Atteia, J.-L.: 2004, The HETE-2 Burst Catalog,
Gamma-Ray Bursts: 30 Years of Discovery: Gamma-Ray
Burst Symp.. AIP Conf. Proc., 727, 57-60.
Wada, K.: 2004, Evolution of the galactic cores andstructure of the molecular gas tori, The interplay among
black holes, stars, and ISM in galactic nuclei, IAU Symp.,
222, 401-406.
Wada, K.: 2004, Fueling gas to the central region of galaxies,
Coevolution of Black Holes and Galaxies, Carnegie
Observatories Astrophys. Ser., 1, 186-202.
Wada, K.: 2004, The neutral ISM in starburst galaxies, ASP
Conf. Ser., 320, 262-265.
Watanabe, M., Takami, H., Takato, N., Colley, S., Eldred,M., Kane, T., Guyon, O., Hattori, M., Goto, M., Iye, M.,
Hayano, Y., Kamata, Y., Arimoto, N., Kobayashi, N.,
Minowa, Y.: 2004, Design of the Subaru laser guide star
adaptive optics module, SPIE, 5490. 1096-1104.
Watanabe, T., Nakagi, N., Wang, D., Liu, L., Kamata, M.,
and Sakamoto, S.: 2004, Characteristics of lightning
discharges over AOS, ALMA Memo, 486.
Watanabe, T., Namiki, Y., Adachi, H., Marubashi, K.,
Watari, S.: 2005, Interplanetary Flux Ropes and Their
Coronal Counterparts, Eds. T. Sakurai and T. Sekii, ASP
Conf. Ser., 325, 433.
Watanabe, T.: 2004, Electron Densities of HighTemperature Coronal Loops, Eds. T. Sakurai and T. Sekii,
ASP Conf. Ser., 325, 227.
Yagi, M.: 2004, Boxiness estimation method with fourthorder moments, Astronomical Data Analysis Software andSystems (ADASS) XIII, Eds. F. Ochsenbein, M. G. Allenand D. Egret, ASP Conf. Proc., 314, 613.
Yamamoto, T. T., Sakurai, T., Kusano, K., Maeshiro, T.,
and Yokoyama, T.: 2004, Magnetic Helicity Injection andSigmoidal Coronal Loops, The Solar-B Mission and theForefront of Solar Physics, Eds. T. Sakurai and T. Sekii,

ASP Conf. Ser., 325, 145-149.
Yamamoto, T., Kawanishi, S., Ueda, A., and Ishiguro, M.:
Low Phase Noise Laser Synthesizer with Simple
Configuration Adopting Phase Modulator and Fiber Bragg
Gratings, ALMA Memo, 508.
Yamauchi, Y., Moore, R. L., Suess, S. T., Wang, H., andSakurai, T.: 2004, Macrospicules, Coronal Heating, andSolar-B, The Solar-B Mission and the Forefront of Solar
Physics, Eds. T. Sakurai and T. Sekii, ASP Conf. Ser., 325,
301-306.
Yanagisawa, K., Toda, H., Kawai, N.: 2005, GRB 050416:
Mitsume optical observation, GCN Circ., 3287.
Yanagisawa, K., Toda, H., Kawai, N.: 2005, GRB 050525:
MITSuME optical observation in VRI, GCN Circ., 3489.
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T.,
Nakajima, T., Hanada, H., Yamada, Y., Araki. H.,
Tazawa, S., Araki, K., Tsuruta, S., Kawano, N., Takato,
N.: 2005, Optical System for JASMINE and CCD
Centroiding Experiment, Proc. the Gaia Symp., The
Three-Dimensional Universe with Gaia (ESA SP-576), Eds.
Turon, C., O'Flaherty, K. and Perryman, M., 487-490.
Yoshida, A., Nakagawa, Y., Yamazaki, T., Sakamoto, T.,
Suzuki, M., Atteia, J.-L., Kawai, N., Shirasaki, Y.,
Tamagawa, T., Vanderspek, R., Hete-2 Science Team:
2004, X-ray activities of "classical" GRBs seen with
HETE-2, 35th COSPAR Scientific Assembly, 3713.
Yoshida, M., Yagi, M., Okamura, S., Ohyama, Y.,
Kashikawa, N., Sasaki, T., Aoki, K., and Iye, M.: 2004,
Deep Spectroscopy of the Very Extended Ionized Gas of
NGC 4388, IAU Symp., 217, 386.
Yoshida, T., and Kajino, T.: 2005, Light element synthesis
through the, ν-process in supernova explosions, Proc.
Origin of Matter and Evolution of Galaxies, 456-465.
5. Presentations
Abe, S., Borovicka, J., Ebizuka, N., Yano, H., Watanabe, J.:
2004, Discovery of New Molecular Bands in Ultraviolet(300-400 nm) Meteor Spectrum, Meteoroids 2004
Conference in London, (Canada, Aug. 16-20).
Abe, S., Borovicka, J., Maeda, K., Ebizuka, N., Watanabe,J.: 2005, First Results of Quadrantid Meteor Spectrum,
36th Annual Lunar and Planetary Science Conference,(USA, March 14-18).
Abe, S., Nakamura, T., Sato, T., Watanabe, J., Yano, H.,
Yamamoto, M., Oonishi, K., Fujiwara, Y., Hashimoto, T.,
Sagayama, T., Sugimoto, M., Ueda, M., Borovicka, J.,
Koten, P.: 2004, MU Radar Radiant Mapping of
2003-2004 Daytime Arietids, Meteoroids 2004 Conferencein London, (Canada, Aug. 16-20).
Arai, K.: 2004, Noise due to scattered light/Simulation
activities in TAMA, The Interferometer Simulation
Workshop, (Italy, Oct. 13-15).
Arai, K.: 2004, Sensing and Control of an Interferometer
Gravitational Wave Detector TAMA300, Nuclear Science
Symposium, (Italy, Oct. 21).
Asai, A.: 2004, Evolution of Flare Ribbons and Energy
Release Rate, RHESSI/SOHO/TRACE Workshop,(Sonoma, USA, Dec. 8-11).
Asai, A.: 2004, Flare-Associated Oscillations Observed with
NoRH, Nobeyama Symposium 2004, (Kiyosato, Oct.
75

26-29).
Asai, A.: 2004, The Red-Asymmetry Distribution at Hα Flare
Kernels Observed in the 2001 April 10 Solar Flare, AGU
Fall Meeting, (San Francisco, USA, Dec. 13-17).
Asai, A.: 2005, Flare Ribbon Expansion and Energy Release,
Magnetic Reconnection 2005, (Awaji, March 8-10).
Capria, M. T., Cremonese, G., Kawakita, H., Watanabe, J.,
De Sanctis, M. C.: 2004, Analysis of the high resolution
spectrum of comet C/2002 C1 Ikeya-Zhang, 35th
COSPAR SCIENTIFIC ASSEMBLY, (France, July
18-25).
Culhane, J. L., Doschek, D. A., Watanabe, T.: 2004, Solar-B
EIS and its Science Goals, 35th COSPAR Scientific
Assembly, E2.1 Towards the Science of Solar-B and
STEREO, (Paris, July 18-25).
Daisaka, H.: 2004, N-body Simulatins of Planetary Rings,
East Asia Numerical Astrophysics Meeting, (Mitaka, Nov.
30-Dec. 2).
Enoki, M., Inoue, K. T., Nagashima, M. and Sugiyama, N.:
2004, Gravitational Radiation from Coalescing
Supermassive Black Hole Binaries in a HierarchicalGalaxy Formation Model, The XXII Texas Symposium on
Relativistic Astrophysics, (USA, Dec. 13-17).
Enoki, M., Takeuchi, T. T., and Ishii, T. T.: 2004,
Fluctuation of the Infrared and Submillimetre Background
Radiation
fromForming
Galaxies,
Post-Nishinomiya-Yukawa Symposium, (Kyoto, Nov.
4-6).
Fujimoto, M.-K.: 2004, Status of TAMA, 5th International
LISA Symposium, (Noordwijk, Netherland, July 12-15).
Fujita, Y.: 2004, Turbulence Produced by Tsunamis in
Galaxy Clusters, International Conference on Cosmic Rays
and Magnetic Fields in Large Scale Structure, (Busan,
Korea, Aug. 16-20).
Furusho, R., Kawakita, H., Fuse, T., Watanabe, J.: 2004,
Forbidden Oxygen Emission Lines of Comet 116P/Wild 4
at 2.4 AU,
35th COSPAR Scientific Assembly, (France,
July 18-25).
Gouda, N., Yano, T., Kobayashi, Y., Yamada, Y.,
Tsujimoto, T., Nakajima, T. Suganuma, M., Matsuhara,
H., Ueda, S., and JASMINE Working Group: 2005,
JASMINE -Japan Astrometry Satellite Mission forINfrared Exploration-, IAU Colloquium -196 Transit ofVenus, (UK, June 7-11).
Hagino, M., Yamamoto, T., Sakurai, T.: 2004, Loading ofmagnetic helicity and flare activity, 35th COSPAR
Scientific Assembly, E2.3 Energy Release and Particle
Acceleration at the Sun and in the Inner Heliosphere,(Paris, July 18-25).
Hanaoka, Y.: 2004, Imaging polarimetry of H-alpha kernelsof solar flares with a ferroelectric liquid crystal polarimeter,
35th COSPAR Scientific Assembly, E2.3 Energy Release
and Particle Acceleration at the Sun and in the Inner
Heliosphere, (Paris, July 18-25).
Hayama, K.: 2004, Reducing Binary Confusion Noise, 5thInternational LISA Symposium, (Noordwijk, Netherland,
July 12-15).
Hayama, K.: 2004, Wavelet-Based Method to Detect
Gravitational Wave Bursts, The 9th annual Gravitational
Wave Data Analysis Workshop, (Annecy, France, Dec.
15-18).
76

Honda, S., Aoki, W., Kajino, T., Ando, H., Beers, T. C.:
2004, The abundance analysis of r-process elements invery metal-poor stars, 14th International Toki Conferenceon Plasma Physics and Controlled Nuclear Fusion and 4thInternational Conference on Atomic and Molecular Data
and Their Applications, (Toki, Oct.5-8).
Honda, S., Aoki, W., Kajino, T., Ando, H., Beers, T. C.:
2004, The Origin of Light Neutron-Capture Elements in
Very Metal-Poor Stars, Nuclei in the Cosmos VIII,(Vancouver, July 19-23).
Hori, K., Ichimoto, K., Sakurai, T.: 2004, Flare-induced
MHD kink oscillation in coronal multiple loops, 35th
COSPAR Scientific Assembly, E2.1 Towards the Scienceof Solar-B and STEREO, (Paris, July 18-25).
Ichiki, K., and Nakamura, K.: 2004, Stochastic
Gravitational Wave Background in Brane World
Cosmology, 14th Workshop on General Relativity andGravitation, (Kyoto, Nov. 29-Dec. 3).
Ichiki, K., Nakamura, K.: 2004, Causal Structure andGravitational Waves in Brane World Cosmology, 17th
International Conference on General Relativity andGravitation, (Dublin, Ireland, July 18-23).
Ichiki, K.: 2004, WMAP Constraints on Decaying Cold Dark
Matter, International Workshop on Particle Physics and the
Early Universe, (Toront, Canada, Sept. 17-21).
Imanishi, M.: 2004, Buried AGNs in Ultraluminous Infrared
galaxies, The Spitzer Space Telescope New Views of the
Cosmos, (Pasadena, USA, Nov. 9-12).
Imanishi, M.: 2004, Comparison of the luminosities ofnuclear starbursts in dusty tori between Seyfert 1s andSeyfert 2s, Evidence for Tori & Winds in AGN, (Leicester,
UK, Sep. 13-16).
Imanishi, M.: 2004, Spectroscopic evidence of dusty tori inthe close vicinity of AGNs, Evidence for Tori & Winds in
AGN, (Leicester, UK, Sep. 13-16).
Ishitsu, N., and Sekiya, M.: 2004, Origins: Numerical
Simulation of the Shear Instability of the Dust layer in a
Protoplanetary Disk, From First Objects to Extrasolar
Planets, (Kyoto, Nov. 4-6).
Ito, T., and Malhotra, R.: 2004, Dynamical evolution ofasteroid fragments originating near the ν6 resonance, 7th
Lunar & Planetary Laboratory Conference, (Tucson,
Arizona, USA, May 25-26).
Ito, T., and Malhotra, R.: 2004, Near-Earth orbital
distribution of asteroid fragments coming from the ν6resonance zone, 35th COSPAR Scientific Assembly, (Paris,
France, Sept. 19-24).
Ito, T., and Malhotra, R.: 2004, Orbital evolution of asteroid
fragments originating near the ν6 resonance, East-Asia
Numerical Astrophysics Meeting, (Mitaka, Nov. 30-Dec.
2).
Ito, T., and Yoshida, F.: 2004, Surface Color Variation of(832) Karin, International Science Symposium on Sample
Returns from Solar System Minor Bodies, The 1st
HAYABUSA Symposium - Characterization of Asteroid
Itokawa, Its Sample Analyses and Related Topics,(Sagamihara, Oct. 20-22).
Ito, T., Yoshida, F., Derwaman, B.: 2004, Lightcurves of
Karin family asteroids, Yukawa symposium, (Kyoto, Nov.
3-5).
Ito, T., Yoshida, F., and Dermawan, B.: 2004, Photometricobservation of a new-born asteroid, 832 Karin, 2004
Post-Nishinomiya-Yukawa Symposium, (Kyoto, Nov.
4-6).
Ito, T., Yoshida, F., Dermawan, B. and Malhotra, R.: 2004,
Lightcurves of the Karin family asteroids, 7th Lunar &Planetary Laboratory Conference, (Tucson, Arizona, USA,May 25-26).
Iwata, T., Sasaki, T., Izumi, T., Kono, Y., Hanada, H.,
Kawano, N., and Kikuchi, F.: 2004, Results of the criticaldesign of RSAT/VRAD mission instruments on SELENE
sub-satellites Rstar/Vstar for selenodesy，XXIII General
Assembly of IUGG, (Sapporo, June 30-July 12).
Izumiura, H.: 2004, An Eeast Asian Planet Search Network,
6th East Asian Meeting of Astronomy, (Seoul, Korea, Oct.
18-22).
Izumiura, H.: 2004, Recent Developments in Observationsof Carbon Stars, Stars as Probe into the Evolution andOrigin of Astrophysical Objects, (Sapporo, Japan, Sep.
30-Oct. 1).
Kajino, T.: 2004, Supernova Nucleosynthesis: Implications
for Nuclear Physics and Cosmology, 1st Germany-Japan
Joint Astrophysics Workshop, (Germany, Dec. 16-18).
Kajino, T.: 2005, Big-Bang Cosmology and Cosmic
Chemical Evolution, 4th COE Symposium, Hokkaido
University, (Sapporo, Mar. 1-2).
Kajino, T.: 2005, Big-Bang cosmology and explosive
nucleosynthesis, Summer School at TRIUMF, (Vancouver,
Canada, July 5-9).
Kajino, T.: 2005, Big-Bang Cosmology and Nucleosynthesis,
Lecture, Universite Libre de Bruxelles, (Belgium, Dec. 9).
Kajino, T.: 2005, Big-Bang Cosmology and Nucleosynthesis,
Lecturer, Universitde Catholique de Louvain, (Belgium,
Dec. 6).
Kajino, T.: 2005, Big-Bang Nucleosynthesis and Cosmology,
8th Int. Conf. on Nuclei in Cosmos, (Vancouver, Canada,
July 19-23).
Kajino, T.: 2005, Disappearing Lightest SupersymmetricParticle as CDM in Brane World Cosmology, 12th Int.
Conf. on SUSY04, (Tsukuba, June 17-23).
Kajino, T.: 2005, New Waiting-Point Nuclei in R-Process
Nucleosynthesis, 20th Astrophysics Workshop, Universite
Libre de Bruxelles, (Belgium, Dec. 12-13).
Kano, R.: 2004, Evolution of the High Temperature Corona,
35th COSPAR Scientific Assembly, E2.2 Mechanisms of
the Solar Activity Cycle, (Paris, July 18-25).
Kasuga, T., Yamamoto, T., Watanabe, J., Ebizuka, N.,
Kawakita, H., and Yano, H.: 2004, Metallic abundances ofthe 2002 Leonid meteor, Meteoroids 2004 Conference inLondon, (Ontario, Canada, Aug. 16-20).
Kasuga, T., Yamamoto, T., Watanabe, J., Yano, H.: 2004,
Metallic abundances of the 2002 Leonid, 35th COSPAR
Scientific Assembly, (France, July 18-25).
Katsukawa, Y., Solar-B team.: 2004, Solar-B: The Next
Japanese Solar Missions, AOGS 1st Annual Meeting,(Suntec, Singapore, July 6-9).
Katsukawa, Y., Tsuneta, S.: 2004, What determines thecoronal heating rate in the photosphere?, 35th COSPAR
Scientific Assembly, E2.1 Towards the Science of Solar-B
and STEREO, (Paris, July 18-25).
Kawaguchi, T.: 2004, Black Hole growth in Narrow-Line
Seyfert 1 Galaxies, Multiwavelength Obsevations of the

Subaru/XMM Deep Survey Field, (Kyoto, Jun. 3-5).
Kawaguchi, T.: 2004, Physics of Super-Eddington Accretion
Discs, Ringberg Workshop on AGN Physics, (Ringberg,
Nov. 22-25).
Kawakita, H., Watanabe, J., Furusho, R., Fuse, T.: 2004,
Ortho to para ratios of molecules in comets, Joint AOGS
1st Annual meeting & 2nd APHW Conference, (Singapore,
July. 5-9).
Kawakita, H., Ootsubo, T., Furusho, R., Watanabe, J.: 2004,
Icy Grains in the Inner Coma of Comet C/2002 T7(LINEAR), 35th COSPAR Scientific Assembly, (Paris,
France, July 18-25).
Kawano, N., Kono, Y., Ping, J., Matsumoto, K., Kikuchi,F., and Liu, Q.: 2004, Narrow and width and INTERNET
Linked VLBI (Very Long Baseline Interferometry) for
Satellite Tracking, 24th Int. Symp. on 24th Int. Symp. on
Space Technology and Science, (Miyazaki, May 30-June
6).
Kobayashi, H., Maehara, S., Nimonji, T., Sato, T., Ohkawa,M., Maruyama, T., Yoshino, T., Kunimori, H., Hosokowa,
M., Ito, H., Li, Y., Nagano, S., Kawamura, S.: 2005,
Oscillation frequency stabilization of a semiconductor
laser using the Faraday effect of Rb absorption lines andthe double optical feedback, SPIE International
Symposium Photonics West 2005, (San Jose, USA, Jan.
22-27).
Kobayashi, H., Nimonji, T., Sawamura, A., Sato, T., Ohkawa,M., Maruyama, T., Yoshino, T., Kunimori, H., Hosokowa,
M., Ito, H., Li, Y. and Nagano, S., Kawamura, S.: 2004,
Evaluation of oscillation frequency stability of a diodelaser using a fs laser optical comb, The 14th Ultrafast
Phenomena Conference, (Niigata, July 25-30).
Kobayashi, Y., Yano, T., Gouda, N., Yamada, Y., Takato,N., Miyazaki, S., Suganuma, M., Tsujimoto, T., Yamada,Y., Gouda, N.: 2004, Statistical Calibrations ofTrigonometric Parallaxes, IAU Colloquium No.196,
Transit of Venus, (UK, Jun. 7-11).
Kodama, T.: 2004, Panoramic Imaging and Spectroscopy ofCluster Evolution with Subaru (PISCES), The
Environments of Galaxies: from Kiloparsecs to
Megaparsecs, (Crete, Greek, Aug. 9-13).
Kodama, T.: 2004, Galaxy Evolution as Functions ofEnvironment and Mass, Multiwavelength Observations of
the Subaru/XMM-Newton Deep Survey Field, SXDS
Workshop, (Kyoto, June 3-5).
Kokubo, E.: 2004, Dynamics of Planetesimals, IAU
Colloquium 197, Dynamics of Populations of Planetary
Systems, (Belgrade, Aug. 31-Sep. 4).
Kokubo, E.: 2004, Origins of Diversity of Planetary Systems,
Post-Nishinomiya-Yukawa Symposium, Origins: FromFirst Objects to Extrasolar Planets, (Kyoto, Nov. 4-6).
Kokubo, E.: 2004, The Habitat Segregation of Planets,
Bioastronomy 2004, (Reykjavik, July 12-16).
Kokubo, E.: 2005, Protoplanets to Terrestrial Planets, Planet
Formation and Detection, (Aspen, Feb. 6-12).
Kotani, T., Kawai, N., Yanagisawa, K., Watanabe, J.,
Kataoka, J., Suzuki, M., Sato, R., Serino, Y., Yatsu, Y.,
Arimoto, M., Shimizu, Y., Nagayama, S., Inata, M.,
Hattori, T., Okita, K., Koyano, H., Izumiura, H.,
Kuroda, D., Okada, T., Yoshida, M., Fukushima, H.,
Ohta, K., Ushiyama, T., Toda, H., Mori, M., Yoshida, A.:77

2004, NIR/Optical Robotic Telescope for GRBS,
Gamma-Ray Bursts in the Afterglow Era, (Rome, Italy,
Oct. 18-22).
Machida, M. N., Matsumoto, T., Tomisaka, K., Hanawa, T.:
2004, Collapse and Fragmentation of a Magnetized
Molecular Cloud - 3D Nested Grid MHD Simulation, East
Asia Numerical Astrophysics Meeting, (Mitaka, Nov.
30-Dec. 2).
Machida, M., Nakamura, K. E., Matsumoto, R.: 2004,
Globalthree-dimensional
magnetohydrodynamic
simulations of state transitions in black hole accretion
disks, East-Asia Numerical Astrophysics Meeting, (Mitaka,
Nov. 30-Dec. 2).
Machida, M., Nakamura, K. E., Ohsuga, K., Matsumoto, R.:
2004, Global Three-dimensional MHD simulations ofco-existence of hard state and soft state disks in black holeaccretion flows, Growing black holes: Accretion in acosmological context, (Garching, Germany, June 21-25).
Machida, M., Nakamura, K. E., Matsumoto, R.: 2005, MHD
simulations of intermediate state of low-high transition inblack hole accretion disk, International Workshop on
MHD Accretion Flows and Jets, (Kyoto, Jan. 25-28).
Maehara, S., Kobayashi, H., Nimonji, T., Sato, T., Ohkawa,M., Maruyama, T., Yoshino, T., Kunimori, H., Hosokowa,
M., Ito, H., Li, Y., Nagano, S., Kawamura, S.: 2004,
Oscillation frequency stabilization of a diode laser for thelaser interferometer in a satellite-to-satellite tracking
system, International Symposium Photonics Asia 2004,(Beijing, Nov. 8-11).
Maehara, S., Kobayashi, H., Sato, T., Ohkawa, M.,
Maruyama, T., Yoshino, T., Kunimori, H., Hosokowa, M.,
Ito, H., Li, Y., Nagano, S., Kawamura, S.: 2004,
Oscillation frequency stabilization of a diode laser for thelaser interferometer in a satellite-to-satellite tracking
system, Asia-Pacific Optical Communications Conference
and Exhibition, (Beijing, China, Nov. 7-11).
Matsumoto, K., Shum, C.K., Yi, Y. and Wang, Y.: 2004,
Southern
Ocean
Tide
Modeling
Basedon
TOPEX/POSEIDON and ERS, Western PacificGeophysics Meeting, (Hawaii, Aug. 16-20).
Matsumoto, T., Hiyama, E., Ogata, K., Iseri, Y., Kamimura,
M., Chiba, S., and Yahiro, M.: 2005, International
Workshop on Reaction Mechanisms for Rare Isotope
Beams, (Michigan, Mar. 9-12).
Matsumoto, T., Tomisaka, K.: 2004, Alignment of Outflow,
Magnetic Field, Disk, and Rotation in Protostellar Collapse,
East Asia Numerical Astrophysics Meeting, (Mitaka, Nov.
30-Dec. 2).
Matsuo, H., Ariyoshi, S., Nagata, H., Hajime, E.: 2004,
Direct Imaging Detectors Develpopment at NAOJ,
International Conference on Submillimeter Science andTechnology, (India, Oct. 13-15).
Matsuo, H., Obuchi, Y., Nagata, H., Ohta, I., Ariyoshi, S.,
Takahashi, N., Ezawa, H., Sekiguchi, T.: 2004, BolometricObservations with ASTE, 5th Workshop on Submm Wave
Receiver Technologies in Eastern Asia, (Taipei, Dec. 6-7).
Matsuo, H., Ohta, I. S., Hattori, M.: 2004, Aperture
Synthesis Imaging using a Double Input Fourier
Spectrometer, International Conference on Submillimeter
Science and Technology, (India, Oct. 13-15).
Miyoshi, M.: 2004, (astro-ph/0409328) An Approach78

Detecting the Event Horizon of SgrA*, The 7th European
VLBI Network Symposium on New Developments in
VLBI Science and Technology and EVN Users Meeting,(Toledo, Spain, Oct. 12-15).
Miyoshi, M.: 2004, A sub-mm VLBI netwrok, Horizon
Telescope II, 3rd e-VLBI Workshop, (Makuhari, Oct. 6-7)
Miyoshi, M.: 2005, VLBI investigations of SgrA* flares,
International Workshop on Magnetohydrodynamic (MHD)
Accretion Flows and Jets, (Kyoto, Jan. 25-28).
Musha, M., Nakagawa, K., Ueda, K., Ueda, A., Ishiguro,
M.: 2004, Optical generation of a highly stable millimeterwave by heterodyning of two phase-locked diode lasers
with an optical comb generator, (CLEO, May 18).
Nagata, H., Matsuo, H., Kobayashi, J., Fujiwara, M., Akiba,
M.: 2004, Cryogenic Readout Integrated Circuits for STJ
detectors, 5th Workshop on Submm Wave ReceiverTechnologies in Eastern Asia, (Taipei, Dec. 6-7).
Nakajima, T.: 2004, Hyper Digital Sky Survey: In search offaint high proper motion stars, Cool Stars, Stellar Systems
and the Sun 13, (Hamburg, Germany, July 5-9).
Nakajima, Y.: 2004, Deep Infrared Surveys of Star Forming
Regions in the MWG and LMC, The Sixth East Asian
Meeting of Astronomy, (Seoul, Oct. 18-22).
Nakamura, K.: 2004, General framework of higher ordergauge invariant perturbation theory, 17th International
Conference on General Relativity and Gravitation, (Dublin,
Ireland, July 18-23).
Nakamura, K.: 2004, Second Order Gauge Invariant
Perturbation Theory, 14th Workshop on General Relativity
and gravitation, (Kyoto, Nov. 29-Dec. 3).
Noda, H., Hanada, H., Iwata, T., and Kawano, N.: 2004,
The SELENE mission and Japanese lunar exploration
scenario，6th East Asian Meeting of Astronomy(EAMA6),(Seoul, Oct. 18-22).
Nogami, N., Ohtsuka, K., Watanabe, J.: 2004, The shortduration "outburst" phenomena of meteors in Leonids
recorded in Chinese Historical Books, Meteoroids 2004
Conference in London, (Ontario, Canada, Aug. 16-20).
Nordgren, T. E., Ohishi, N., Hutter, D. J.: 2004, AsymmetricSurface Brightness Distribution of Altair Observed with
the Navy Prototype Optical Interferometer, American
Astronomical Society Meeting 204, (Colorado, May
30-June 3).
Ogata, K., Yahiro, M., Iseri, Y., Matsumoto, T., Hashimoto,S., T. Egami, T., and Kamimura, M.: 2004,
Japanese-German Nuclear Structure and Astrophysics
Workshop, (GSI, Dec. 16-18).
O'Mullane, W., Budavari, T., Haridas, V., Li, N., Malik, T.,
Ohishi, M., Szalay, A., Thakar, A., Williamson, R.: 2004
OpenSkyQuery ¥& OpenSkyNode - the VO Framework toFederate Astronomy Archives, Astronomical Data
Analysis Software & Systems XIX, (USA, Oct. 25-27).
Saigo, K., Matsumoto, T., and Umemura, M.: 2004, The
Formation of Population III Binaries, East Asia Numerical
Astrophysics Meeting, (Tokyo, Nov. 30-Dec. 2).
Saigo, K., Matsumoto, T., and Umemura, M.: 2004, The
Formation of Population III Binaries, 7th Post
Nishinomiya-Yukawa Symposium, (Kyoto, Nov. 4-6).
Saitoh, T. R., Koda, J., Okamoto, T., Wada, K., Habe, A.:
2004, East-Asian Numerical Astrophysics Meeting 2004,(Tokyo, Nov. 29-Dec. 1, 2004).

Sasaki, S., Sasaki, T., Watanabe, J., Sekiguchi, T., Yoshida,F., Ito, T., Kawakita, H., Fuse, T., Takato, N. andDermawan, B.: 2004, Mature and Fresh Surfaces on
New-Born Asteroid Karin, American Astronomical
Society, DPS meeting #36, (Singapore, July 5-9).
Sasaki, S., Sasaki, T., Watanabe, J., Sekiguchi, T.,
Yoshida, F., Ito, T., Kawakita, H., Fuse, T., Takato, N.,
Dermawan, B.: 2004, Mature and Fresh Surfaces on
New-Born Asteroid Karin, American Astronomical
Society, DPS meeting, (USA, Nov. 8-12).
Sasaki, S.: 2004, Process of water supply from Martiansubsurface, Japanese-American Frontiers of Science Symp.,(California, USA, Dec. 10-12).
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 the Newborn Asteroid Karin, 36th Annual
Lunar and Planetary Science Conference, (USA, Mar.
14-18).
Sasaki, T., Sasaki, S., Watanabe, J., Sekiguchi, T.,
Kawakita, H., Fuse, T., Takato, N., Yoshida, F.: 2004, A
new-born asteroid 832 Karin with old and new surfaces,
35th COSPAR Scientific Assembly, (Paris, France, July
18-25).
Sato, T., Plag, H.-P., Tamura, Y., Matsumoto, K., Asari,K., and Francis, O.: 2004, Gravity Tides and seasonal
Gravity Variation at NY-ALESUND, Svalbard in Arctic,
The 15th Int. Symp. on Earth Tides, (Ottawa, Canada, Aug.
2-6).
Sato, Y.: 2005, Subaru/Keck Observations of the UKIDSSDXS/SWIRE Fields: Lockman Hole and ELAIS N1,
FMOS Science WS, (Oxford, UK, Jan. 11-12).
Shibasaki, K.: 2004, Quiet Sun and Active Region Studies
by Nobeyama Radioheliograph, Nobeyama Symposium
2004, (Kiyosato, Oct. 26-29).
Shibasaki, K.: 2004, Results from Nobeyama Radio
Heliograph, 6th East Asian Meeting of Astronomy, (Seoul,
Korea, Oct. 18-22).
Shimojo, M.: 2004, The Joint Observations of Prominence
Eruptions using Solar-B, STEREO and NoRH, 35th
COSPAR Scientific Assembly, E2.1 Towards the Scienceof Solar-B and STEREO, (Paris, July 18-25).
Shimojo, M.: 2004, NoRH Observations of Prominence
Eruptions, Nobeyama Symposium 2004, (Kiyosato, Oct.
26-29).
Shimojo, M.: 2004, The Joint Observation of Prominence
Eruptions using Solar-B, STEREO and NoRH, 35th
COSPAR Scientific Assembly 2004, (Paris, France, July
18-25).
Shirasaki, Y., Tanaka, M., Honda, S., Mizumoto, Y.,
Ohishi, M., Yasuda, N., Masunaga, Y., Oe, M.: 2004,
Structured Query Language for Virtual Observatory,
Astronomical Data Analysis Software & Systems XIX,
(USA, Oct. 25-27).
Shirasaki, Y.: 2005, Japanese Virtual Observatory
Implementation Experience, GGF13 Astro-RG, (Korea,
Mar. 15).
Shirasaki. Y.: 2004, ADQL/s Syntax (Proposal) - towards
unification of ADQL, SIAP, SSAP, SXAP...,IVOA
Interoperability Meeting, (USA, May 24-28).
Shirasaki. Y.: 2004, Design and Implementation of JVO

SkyNode, VO Small Projects Meeting, (India, Sep. 30-Oct.
1).
Shirasaki. Y.: 2004, Standard Query Language for VO,
IVOA Interoperability meeting, (India, Sep. 27-29).
Shirasaki. Y.: 2004, SXDS database and Japanese Virtual
Observatory Multiwavelength Observations of the
Subaru/XMM-Newton Deep Survey Field, (Japan, Jun.
3-5).
Shum, C., Yi, Y., Wang, Y., Matsumoto, K., and Andersen,
O.: 2004, Southern Ocean Ocean Tide Modeling,
ENVISAT Symposium, (Salzburg, Sept. 6-10).
Shum, C. K., Matsumoto, K., Yi, Y., Han, S., Niwa, Y., Han,G., and Braun, A.: 2004, Coastal Ocean Tide Modeling,
Ocean Surface Topography Science Team Meeting, (St.
Petersburg, Nov. 4-6).
Sôma, M., Tanikawa, K.: 2004, Variation of Delta T
between AD 800 and 1200 Derived from Ancient Solar
Eclipse Records, Journ¥'ees 2004, Fundamental
Astronomy: New concepts and models for high accuracy
observations, (Paris, France, Sept. 20-22).
Somiya, K.: 2005, Frequency noise and intensity noise of the
RSE interferometer, LIGO Science Collaboration August
2003 Meeting, (Livingston, USA, Mar. 20-24).
Sugano, T., and Heki, K.: 2004, Lunar Interior Studies Using
Lunar Prospector Line of Sight Acceleration Data, Lunarand Planetary Science Conf., (Houston, Mar. 15-19).
Sugimoto, M.: 2004, Cartridge-Type 800 GHz Receiver for
the ASTE, 5th Workshop on Sub-mm Wave ReceiverTechnologies in Eastern Asia, (Taipei, Dec. 6-7).
Sugiyama, N.: 2004, Reionization: State of the Art, 20th IAP
colloquium on Cosmic Microwave Background Physics
and Observation, (IAP, Paris, June 28-July 2).
Sugiyama, N.: 2004, Cosmic Microwave Background:
Reveals Secrets of the Universe, Japanese-American
Frontiers of Science, Seventh Annual Japanese-American
Beckman Frontiers of Science Symposium, (Irvine,
California, USA, Dec. 10-12).
Takahashi, R.: 2004, Scattering of Gravitational Waves by
the Weak Gravitational Fields of Lens Objects, The 14th
Workshop on General Relativity and Gravitation, (Kyoto,
Nov. 29-Dec. 3).
Takahashi, R.: 2004, Status of TAMA300, The 17th
International Conference on General Relativity andGravitation, (Dublin, Ireland, July 18-23).
Takata, T.: 2004, Near Infrared Imaging of SXDS field,
SXDS International Meeting, (Kyoto, June 3-5).
Takeuchi, T. T., Enoki, M., Ishii, T. T.: 2004, Contributionof Forming Galaxies to the Cosmic Infrared BackgruondFluctuation, 35th COSPAR Scientific Assembly, (France,
Jul. 18-25).
Tamura, M., Shibai, H., Nakagawa, T., Yamada, T.,
Matsumoto, T., Nagashima, C., Nishikawa, J., and JTPF
working group: 2004, A Japanese TPF Mission: HighContrast Space Telescope (HCST), Second TPF Workshop,(San Diego, July 26-29).
Tamura, M.: 2004, Subaru Exploration of Exo-planets andDisks, The Sixth East Asian Meeting of Astronomy,(Seoul, Oct. 18-22).
Tamura, M.: 2004, Toward Direct Observations ofExtrasolar Planets, The Post-Yukawa Symposium, (Kyoto,
Nov. 4-6).
79

Tamura, M.: 2005, Planet Fiding Efforst in Japan andPossible Collaboration with TPF, TPF-I Science Working
Group Meeting, (Monrovia, Mar. 9-10).
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.: 2004, Japanese Virtual Observatory (JVO)
prototype 2, Astronomical Data Analysis Software andSystems XIV, (USA, Oct. 25-27).
Tanaka, M.: 2004, Japanese VO prototype system andapplications to Astrophysics - Portal System -, VO Small
Projects Meeting, (India, Sep. 30-Oct. 1).
Tanaka, M.: 2004, Prototype system of the Japanese Virtual
Observatory, Multiwavelength Observations of the
Subaru/XMM-Newton Deep Survey Field, (Japan, Jun.
3-5).
Tatematsu, K.: 2004, N2H+ Observations of Molecular
Cloud Cores in Taurus, Cores, Disks, Jets & Outflows in
Low & High Mass Star Forming Environments, (Canada,Jul. 12-16).
Tatematsu, K.: 2004, N2H+ Observations of Molecular
Cloud Cores in Taurus, The Sixth East Asian Meeting of
Astronomy, (Korea, Oct. 18-22).
Tatsumi, D., and TAMA collaboration: 2004, Status of
TAMA data analysis, The 17th International Conference
on General Relativity and Gravitation, (Dublin. Ireland,
July 18-23).
Tatsumi, D., Tsunesada, Y., and the TAMA Collaboration:
2004, New noise reduction method for ringdown signal
search in TAMA300, The 9th Gravitational Wave Data
Analysis Workshop, (Annecy, France, Dec. 15-18).
Title, A., Tsuneta, S.: 2004, The Focal Plane Package for
Solar B, 35th COSPAR Scientific Assembly, E2.1
Towards the Science of Solar-B and STEREO, (Paris, July
18-25).
Tomisaka, K., Machida, M. N., Matsumoto, T., Hanawa, T.:
2004, Role of Magnetic Field in Star Formation Process,
The Magnetized Plasma in Galaxy Evolution, (Cracow,
Poland, Sept. 27-Oct. 1).
Tomisaka, K.: 2004, How Magnetic Fields Affect the SNR
Evolution, Diffuse Matter in the Galaxy: Observations
Confront Theory, (Arecibo, Puerto Rico, Aug. 29-Sept. 2).
Tsujimoto, T., Yamada, Y., Gouda, N.: 2004, Statistical
Calibrations ofTrigonometric Parallaxes, IAU
Colloquium No.196, Transit of Venus, (UK, Jun. 7-11).
Tsujimoto, T.: 2004, A New Class of Type Ia Supernovae
Inferred from Abundance Patterns of Halo Stars andHigh-z Galaxies, Chemical Abundances and Mixing inStars in the Milky Way and its Satellites, (Italy, Sep.
13-17).
Tsunesada, Y., and the TAMA Collaboration: 2004, Searchfor black hole ringdowns using TAMA300 data, The 9th
Gravitational Wave Data Analysis Workshop, (Annecy,
France, Dec. 15-18).
Tsuneta, S., Title, A.: 2004, Science with Solar-B solar
optical telescope, 35th COSPAR Scientific Assembly,
E2.1 Towards the Science of Solar-B and STEREO, (Paris,
July 18-25).
Ueda, S., Nakasuka, S., and JASMINE Working Group:
2005, Nano-JASMINE:a nanosize astrometry satellite,
IAU Colloquium No.196, Transit of Venus, (UK, Jun.
807-11).
Ueda, S., Yamada, Y., Kuwabara, T., Gouda, N., Tsujimoto,T., Kobayashi, Y., Nakajima, T., Matsuhara, H., Yano,
T., Suganuma, M., and JASMINE Working Group: 2005,
JASMINE Simulator, IAU Colloquium No.196, Transit ofVenus, (UK, Jun. 7-11).
Umemura, M.: 2004, Early Reionization by Pop III Binaries,
Post-Nishinomiya-Yukawa Symposium, Origins: FromFirst Objects to Extrasolar Planets, (Kyoto, Nov. 4-6).
Umemura, M.: 2004, The Origin of Galaxies, The Quest fora Concordance Cosmology and Beyond, (Cambridge, July
5-9).
Umezu, K., Ichiki, K., Kajino, T., Mathews, G. J., Yahiro,
M., Nakamura, R.: 2004, International Workshop on
Particle Physics and the Early Universe, (Toronto, Canada,
Sep. 17-21).
Wada, K.: 2004, Numerical Astrophysics in Japan, East Asia
Numerical Astrophysics Meeting, (Mitaka, Nov. 30-Dec.
2).
Wada, K.: 2004, Formation of galactic cores and primordial
SMBH during galaxy formation, The role of mergers andfeedback in galaxy formation, (Ringberg Castle, Germany,
Oct. 31-Nov. 5).
Wada, K.: 2004, Fueling gas to the central region, The
central parsec of galaxies, (Heidelberg, Germany, Oct.
6-8).
Wada, K.: 2004, Gravity-driven and spiral-shock driven
turbulence in the galactic central region, Diffuse matter in
the Galaxy, (Arecibo, Puerto Rico, Aug. 30-Sept. 3).
Watanabe J.: 2004, Ishigaki Astronomical Observatory
Project, Deep Impact Mission Workshop, (Taiwan, May
28).
Watanabe J.: 2004, New prospects of comets and TNOs, 6th
East Asia Meeting of Astronomy, Asian View of
Cooperation in Astronomy, (Korea, Oct. 18-22).
Watanabe, J., Kasuga, T.: 2004, Possible Extreme Meteor
Storm observed in fall 1933 over Japan, Meteoroids 2004
Conference in London, (Ontario, Canada, Aug. 16-20).
Watanabe, J., Kawakita H.: 2004, Crystalline Sillicate in
Comets: Remnants of Physical Process in Protoplanetary
Disk, Joint AOGS 1st Annual meeting & 2nd APHW
Conference, (Singapore, July 5-9).
Watanabe, J.: 2004, Meteor streams and Comets: Recent
Progress (INVITED REVIEW), Meteoroids 2004
Conference in London, (Ontario, Canada, Aug. 16-20).
Watanabe, T., the Solar-B Team: 2004, Solar-B scientificoperation and its observing modes, 35th COSPAR
Scientific Assembly, E2.1 Towards the Science of Solar-B
and STEREO, (Paris, July 18-25).
Yahagi, H.: 2004, Parallel Adaptive Mesh Refinement
N-body Code and Its Applications, East-Asia Numerical
Astrophysics Meeting, (Mitaka, Nov. 30-Dec. 2).
Yamada, Y., Gouda, N., Tsujimoto, T., Kobayashi, Y.,
Nakajima, T., Matsuhara, H., Yano, T., Ueda, S.,
Suganuma, M., and JASMINE Working Group: 2005,
Overall Design of JASMINE, IAU Colloquium No.196,
Transit of Venus, (UK, Jun. 7-11).
Yamamoto, M., Toda, M., Higa, Y., Maeda, K., Watanabe,J.: 2004, Altitude distribution of persistent meteor trains
derived by METRO campaign archives, Meteoroids 2004
Conference in London, (Ontario, Canada, Aug. 16-20).

Yamamoto, T., Sakurai, T., Kusano, K., Yokoyama, T.,
Maeshiro, T.: 2004, Magnetic helicity injection andsigmoidal coronal loops, 35th COSPAR Scientific
Assembly, E2.2 Mechanisms of the Solar Activity Cycle,(Paris, July 18-25).
Yanagisawa, K.: 2004, Okayama Astrophysical Observatory
Wide-Field Camera, 6th East Asian Meeting on
Astronomy, (Seoul, Korea, Oct. 18-22).
Yano, T., Gouda, N., Kobayashi, Y., Tsujimoto, T.,
Nakajima, T., Hanada, H., Kan-ya, Y., Yamada, Y.,
Araki, H., Tazawa, S., Asari, K., Tsuruta, S., Kawano,N., and Takato, N.: 2005, CCD Centroiding Experiment
for the Japan Astrometry Satellite Mission (JASMINE)
and In Situ Lunar Orientation Measurement (ILOM), IAU
Colloquium No.196, Transit of Venus, (UK, Jun. 7-11).
Yi, Y., Matsumoto, K., Braun, A., Shum, C. K. and Wang,Y.: 2004, Advances in Southern Ocean Tide Modeling,
15th Int. Symp. on Earth Tides, (Ottawa, Aug. 2-6).
Yoshida, F., Cellino, A., Di Martino, M., Nakamura, A. M.,
Ishiguro, M., Saito, J., Derwaman, B., Anderlucci, E.:
2004, Polarimetric observation s of (25143) Itokawa atlarge phase angles, Hayabusa symposium, (ISAS, Oct.
20-22).
Yoshida, F., Nakamura, T.: 2004, Size distribution of small
main-belt asteroids as a source of Near-Earth Asteroids,
COSPAR, (Paris, France, July 19-24).
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