PREFACE 08.2.28 6:43 PM ページ1

Table of Contents

Preface

Shoken MIYAMA
Director General
National Astronomical Observatory of JapanI

Scientific Highlights April 2006 - March 2007 ··························································· 1IIPublications, Presentations ························································································· 46
1. Refereed Publications······························································································ 46
2. Publications of the National Astronomical Observatory of Japan ························· 57
3. Report of the National Astronomical Observatory of Japan ·································· 57
4. Conference Proceedings ························································································· 57
5. Publications in English ··························································································· 65
6. Conference Presentations ······················································································· 65

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PREFACEI am pleased to present the Annual Report of the National
Astronomical Observatory of Japan (NAOJ) for fiscal 2006. This is thefirst annual report that I present as Director General of NAOJ.
Three years have passed since the national universities and inter-university research institutes were incorporated. This year, NAOJ had the second
annual evaluation by the National University Corporation Evaluation
Committee, and I think our activities were highly evaluated. From now on,
we will make the most of the increased freedom given to the independent
corporations and apply it for researches and activities as an inter-university
research institute. For evaluations of each project and center, we organized
the Planning and Reviewing Committee, in which external committee
members are half of the members in number. We have utilized the feedbacks from the committee for the improvement of our activities.
Also, international evaluations were conducted for two “A projects”(projects in the early developmental stage), 4-Dimensional Digital Universe (4D2U) Project and MIRA Project,
to judge the project activity level and discuss the continuance of these projects. The future vision of these projects will be defined next year based on the result of this international evaluation as well as the evaluation result
presented by the Planning and Reviewing Committee.
As for the achievements in research field, the Subaru Telescope at NAOJ Hawaii Observatory has been continuously achieving many results, such as the success of the first measurement of the spatial distribution of dark
matter in the universe, and the establishment of a new world record for the most distant galaxy observation. It isnoteworthy that nine from the ten of most distant galaxies have been discovered by the Subaru Telescope.
However, if we are content to the current achievements of the Subaru Telescope, we will soon lag behind otherresearch institutes in the world. To avoid such situation, it is important to advance research and development(R&D) of new observation instruments. In 2006, as a part of our R&D efforts, a new adaptive optics AO188
was completed. In this new adaptive optics, wavefront compensation has been remarkably improved by increasing the number of segmented mirrors several times, and thereby near-diffraction-limit resolution has beenachieved. Further development is expected by combining this with a newly-completed laser-guide star system
which artificially creates reference objects for AO. Furthermore, we have also been developing HiCIAO, thesuccessor to the current stellar coronagragh CIAO, and HiperSurprimeCam, the successor to the current widefield imager SurprimeCam. We will continuously work hard on the equipment development for the Subaru
Telescope.
In October 2006, we succeeded in launching the SOLAR-B satellite, which had been a long-held wish of
astronomers involved in solar observation. This astronomical observation satellite named “HINODE” is successfully sending us brilliant initial images, and it has been confirmed that the optical telescope integrating theobservation instrument for launch, which was assembled in the NAOJ Advanced Technology Center, is producing results as expected. The moving images of the Sun’s surface captured with unprecedentedly high angularresolution show us the activities on the Sun’s surface in great detail. By analyzing these images, a new pictureof solar physics will be unveiled.
In addition to what has been mentioned above, many other results have been achieved such as: a creation of aradio map catalog of near-by galaxies using the multi-beam receiver at Nobeyama Radio Observatory; a discovery of a planet around a giant star by Okayama Astrophysical Observatory; and a success of distance measurement of a Galactic maser object by Mizusawa VERA Observatory. Further detailed observation, measurementof distance and proper motion of many maser sources are expected in future.
ALMA (Atacama Large Millimeter/submillimeter Array) Project, which is under construction in international
cooperation, has entered the 3rd year in the 8-year plan. The construction of the antenna and development of thereceiver and the correlator are about to enter the most important phase. The antennas are scheduled to bePREFACE 08.2.28 6:43 PM ページ4

shipped to Chile in 2007, and their tentative assembly is now going on in Japan. As for the ALMA Board, thetop decision-making body of ALMA, it was authorized that the number of delegates from NAOJ shall be
increased from 1 to 3, after discussions from various viewpoints. As a result, the board will be operated in amanner which is approximately consistent with the contribution ratio to ALMA: with 4 members from North
America, 3 from Europe, 3 from East Asia, and 1 from Chile.
In October 2006, there was an earthquake in the sea around the Island of Hawaii, and the Subaru Telescopeand other observation facilities were damaged. Fortunately, we could escape from fatal damages to the facilities
by conducting prompt investigations and making emergency action plans, and could restore them to the normal
operation status after nearly one-month operation halt. Although there were some remaining actions in the following year, most of them have already been completed. In addition to this, there were some powerful typhoons
in this year. Ishigakijima Astronomical Observatory, VERA Ishigaki Station, and VERA Chichijima Station
were damaged by typhoon. In particular, Ishigakijima Astronomical Observatory were suffered strong gusts ofwind of the powerful typhoon, which blew off both of the two dome slits, and the inside of the dome was
exposed to heavy wind and rain and severely damaged. As the wind speed was higher than expected, we conducted a detailed investigation of the damages. Restoration of the facilities had almost been completed by theend of the year after operation halt of more than 6 months. The costs for restoring the facilities affected by theearthquake and typhoon were covered by the natural disaster relief expenditure from the government, nonlife
insurance, and NAOJ contingency fund. These events taught us that it is necessary to take various measures inthe event of natural disasters.
Also in this year, we made a lot of effort for graduate education. Once in several months, we held an informal gathering for discussion between students at the Graduate University for Advanced Studies and the facultyincluding the Academic Dean (NAOJ Director General) and Associate Dean to have a lively exchange of opinions. By using the teleconference system, students at remote campuses could also participate in the discussion.
We will continuously facilitate close interactions with students.
Public outreach activities have also been intensely promoted to introduce the latest astronomical researchdevelopment to the public. One of the outstanding accomplishments in this year is the completion of the fourdimensional dome theater (4D2U Dome Theater) at the end of the year, which was developed by the 4D2U
project mentioned above. This dome theater can project the image of outer space seamlessly on the screen of the
10-meter planetarium dome with 13 projectors, unlike the old theater with just 3 flat screens. And the method ofstereoscopic viewing has also been changed from the conventional polarization-based method to the wavelength
multiplex imaging method using interference filters, which allows freedom of choice in the selection of screenmaterials and reduces eye’s fatigue of the viewers. The dome theater will enable us to provide a wider range ofcontents produced by NAOJ for the public.
Another event to be mentioned is the decision on the main building of the former international latitude
observatory in Mizusawa campus. We canceled the demolition of the building according to the request fromlocal residents, and decided to assign it to Oshu city where the observatory was located, as a result of a selection. The renovation will be completed in 2007 at the expense of Oshu city, and the renovated building will beshared by the citizens as a historical property in tribute to Dr. Hisashi Kimura and “Kaze no Matasaburo”(Matasaburo of the Wind - one of the major works of Kenji Miyazawa), and will be used as a building to provide opportunity for the citizens to become familiarized with Astronomy.

Shoken Miyama
Director General of NAOJ

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I Scientific Highlights(April 2006 - March 2007)

1. Discovery of the most distant galaxy at a redshift 6.96 : Probing the epoch of cosmic reionization ····································· IYE et al.

3

2. CCD Centroiding Experiment for Correcting the Distorted Image on the Focal Plane ···················································· YANO et al.

4

3. An Interpretation of Flat Density Cores of Clusters of Galaxies by Degeneracy Pressure of Fermionic Dark Matter:
A Case Study of A1689 ········································································································································ NAKAJIMA et al.

5

4. Zenith-Distance Dependence of Chromatic Shear Effect: A Limiting Factor for
an Extreme Adaptive Optics System ···················································································································· NAKAJIMA et al.

6

5. A Nobeyama Millimeter Interferometric Search for Buried Supermassive Blackholes
in Luminous Infrared Galaxies ······························································································································· IMANISHI et al.

7

6. Effects of Phase Characteristics in Main Beam of Telescopes on Same-Beam VLBI ··························································· LIU et al.

8

7. A Search for CO (J = 3 – 2) Emission from the Host Galaxy of GRB980425
with the Atacama Submillimeter Telescope Experiment ················································································· HATSUKADE et al.

9

8. Origins of Carbon-Enhanced Metal-Poor Stars ··························································································································· AOKI 10
9. Where did starburst occur and from where did it terminate in E+A galaxies? ··································································· YAGI et al. 11
10. First light of the Laser Guide Star Adaptive Optics System: 10 times clearer vision for Subaru Telescope ··············· TAKAMI et al. 12
11. High-Dispersion and High-S/N Spectrum Atlas of Vega ····························································································· TAKEDA et al. 13
12. ASTE Observations of Warm Gas in Low-mass Protostellar Envelopes: Different Kinematics
between Submillimeter and Millimeter Lines ··································································································· TAKAKUWA et al. 14
13. Atomic Carbon in the AFGL 333 Cloud ··························································································································· SAKAI et al. 15
14. Nobeyama CO Atlas of Nearby Spiral Galaxies: Distribution of Molecular Gas
in Barred and Nonbarred Spiral Galaxies ······················································································································ KUNO et al. 16
15. Luminosity Dependent Evolution of Lyman Break Galaxies : UV Luminosity Functions from redshift 5 to 3 ············· IWATA et al. 17
16. First Infrared Imaging Polarimetry of b Pictoris ········································································································· TAMURA et al. 18
17. Infrared Imaging Polarimetry of the Orion Nebula ····································································································· TAMURA et al. 19
18. Development of a multi-Fourier-transform interferometer: fundamentals ········································································ OHTA et al. 20
19. Neutrino-Nucleus Reactions based on New Shell Model Hamiltonians ········································································ SUZUKI et al. 21
20. Nonlinear Hydromagnetic Wave Support of a Stratified Molecular Cloud. II. a Parameter Study ······························· KUDOH et al. 22
21. ASTE CO(3-2) Observations of the Barred Spiral Galaxy M 83 ············································································· MURAOKA et al. 23
22. ASTE Observations of Nearby Galaxies : A Tight Correlation between CO(J = 3–2) Emission and Ha ··················· KOMUGI et al. 24
23. Neutrino Oscillation Effects on Supernova Light-Element Synthesis ········································································ YOSHIDA et al. 25
24. The Distance to the Galactic Center ······················································································································· NISHIYAMA et al. 26
25. Search for Herbig Ae/Be Stars in the Magellanic Bridge ······················································································ NISHIYAMA et al. 27
26. Distribution of dust clouds around the central engine of NGC 1068 ·········································································· TOMONO et al. 28
27. Abundances of metal-poor star HD 122563 ··················································································································· HONDA et al. 29
28. Project “Origin of Milkyway” ······································································································································· SAITOH et al. 30
29. Periodic Vortex Shedding from a 12-m Antenna ············································································································· UKITA et al. 31
30. Discovery of Ha Absorption in the Broad Absoprtion Line Quasar SDSS J0839+3805 ··················································· AOKI et al. 32
31. Polarization Differential Objective Spectroscopy with a Nulling Coronagraph ···················································· MURAKAMI et al. 33
32. High-Resolution Studies of the Dense Molecular Cores toward Massive Star-Forming Regions ···································· SAITO et al. 34
33. Improvement of Gravitational Wave Detector TAMA300 by the Seismic Attenuation System (SAS) ··················· FUJIMOTO et al. 35

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34. Giant Molecular Association in Spiral Arms of M 31: Evidence for Dense Gas Formation via Spiral Shock
Associated with Density Wave ? ································································································································ TOSAKI et al. 36
35. MOIRCS Deep Survey : DRG Number Counts ······································································································· KAJISAWA et al. 37
36. Protocluster Search around Radio Galaxies at z ~ 2.5 with Subaru/CISCO ····························································· KAJISAWA et al. 38
37. 12CO(J =3–2) Line Observation of Elliptical Galaxies ··························································································· NAKANISHI et al. 39
38. Torsionally Excited Methyl Formate in Orion KL ································································································ KOBAYASHI et al. 40
39. Universality of the c-process in core-collapse supernovae ··················································································· HAYAKAWA et al. 41
40. Removal of Central Obscuration and Spider Arm Effects with Beam-Shaping Coronagraphy ··········································· ABE et al. 42
41. Imaging Spectroscopy of a Gradual Hardening Flare on 2000 November 25 ·························································· TAKASAKI et al. 43
42. Solar Heating Effect on Meteoroids in Meteor Showers ······························································································ KASUGA et al. 44
43. Li Production by the Radiative Decay of Long-Lived Particles ············································································· KUSAKABE et al. 45

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Discovery of the most distant galaxy at a redshift 6.96 :Probing the epoch of cosmic reionization
IYE, Masanori, KASHIKAWA, Nobunari(NAOJ)

OTA, Kazuaki and 7 authors(Univ.Tokyo)
The Universe began with a fireball 13.7 Gyr ago. Quick
expansion and cooling made it filled with neutral hydrogenby 0.38 Myr after the big bang. The first generation ofgalaxies were born a few 100 Myr later and UV radiationof newly formed massive stars ionized the interstellar gas
producing characteristic Lymana line emission. The current group made Suprime-Cam survey with a special filter
developed for isolating galaxies with Lyman a emission
line at redshift 7.0 in the Subaru Deep Field. FOCAS spectroscopy of two targets selected by their color out of 41,533
objects studied, led to the finding of the most distant galaxy
at a redshift 6.96 (Figs. 1, 2, and 3; Table 1), IOK-1, at
12.88 billion light years away [1]. We are looking at thisgalaxy at 780 Myr after the big bang. The number of galaxies at redshift 7.0 appears to be significantly smaller thanthat at redshift 6.6, about 60 Myr later. This decrease could
be interpreted that we are stepping into the era of cosmic
re-ionization.

Figure 3: Lyman a emission line at rest wavelength of 121.5nm wasseen at 968nm, corresponding to a redshift 6.96.
Table 1: Top 10 most distant galaxies as of Sep. 2006.

No

ID

z

distance#

date

1＆

IOK-1

6.964

128.8

2006.92

SDF 1004

6.597

128.2

2005.2

3

SDF 1018

6.596

128.2

2006.4

4

SDF 1030

6.589

128.2

2006.4

5

SDF 1007

6.580

128.2

2005.2

6

SDF 1008

6.578

128.2

2005.2

6

SDF 1001

6.578

128.2

2003.4＊

Figure 1: The most distant galaxy IOK-1 found.

8

HCM-6A

6.560

128.2

2002.49

SDF 1059

6.557

128.2

2006.410

SDF 1003

6.554

128.2

2005.2#For a standard cosmology model with age 13.66 Gyr.
* Discovered by Hu et al. with Keck telescope.
&
The most distant galaxy found by the present study.
Note that a few other gravitationally lensed galaxies are claimed to be atredshift around 7 from their colors but lacking spectroscopic confirmation.
Figure 2: Two candidates visible only in NBF973.

References[1] Iye, M., Ota, K., Kashikawa, N., et al.: 2006, Nature, 443, 186-188.

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CCD Centroiding Experiment for Correcting the Distorted
Image on the Focal PlaneYANO, Taihei, ARAKI, Hiroshi, GOUDA, Naoteru, KOBAYASHI, Yukiyasu,
TSUJIMOTO, Takuji, NAKAJIMA, Tadashi, KAWANO, Nobuyuki, TAZAWA, Seiichi(NAOJ)YAMADA, Yoshiyuki

HANADA, Hideo, ASARI, Kazuyoshi, TSURUTA, Seiitsu(Kyoto University)(NAOJ)INTRODUCTIONJASMINE will measure trigonometric parallaxes, positions and proper motions of stars with the precision of 10
microarcsec. ILOM will also measure the positions of stars
in order to obtain the lunar physical libration and the freelibrations directly from the lunar surface.
Both projects use a common astrometric technique toobtain precise positions of stars. In order to accomplish thisgoal, we must determine the accurate centroid of star
images on the detector.
We have demonstrated the measurements of the positions of artificial star images on the CCD plane with 1/300
pixel precision in a laboratory experiment [1]. In the experiment, we have just measured the positions of stars on the
CCD focal plane, in other words, we do not care about thepossible distortion of the image due to optical aberration.
Here we also consider the correction for the distortion fromthe strongly distorted optical image.
ALGORITHM
In order to estimate the distance between two point
sources from distorted image frames, the following algorithm is proposed. First of all, we pick up two stars tomeasure the distance. Next we seek the pixel in which a
number of photons is maximum in each star. Then we pickup a square subset of 5#5 pixels around the peak pixel ofeach star image. Accordingly, the number of photons is the
maximum values at the center of pixels in both two stars.
Only the pixel values of the two subsets are used to measure the distance of the two stars. The photon weighted
means (xc, yc) are different from the centers of the stars.
Here, we assume that the difference between the photon
weighted mean and the center of the star is proportional tothe deviation of the photon weighted mean from the centerof the pixel.
xa − xc = kxc ,ya − yc = kyc(1)

where (xa , ya) is the center of a star from the center of the
pixel,
We assume that the value of distortion at a certain pointon the focal plane is proportional to the cube of distancefrom the position of the optical axis on the focal plane,d r = e r 3 r̂ ,4(2)

where r = (x - xcenter) 2 + (y - ycenter) 2 is the distance of astar from the position of the optical axis on the focal plane,e is a constant, and r̂ is the unit vector of r. Then we utilizea least square method to obtain the distance of two stars.
RESULTS
Because of the distortion of an image on the focal planein addition to the deviation of the photon weighted meansfrom the center of stars, distances of two stars are spread toabout 0.5 pixels. By correcting the distortion of images andthe deviation of the photon weighted means from the centers of stars, the dispersion of the errors becomes smaller
than 1/100 pixels.
This result indicates that the distortion of the image on
the CCD array is well fitted by the third order correction.
Furthermore, uncontrolled random deviation from theoptics or the CCD array is very small. The other unexpected deviation from the other origin is also small. Therefore
there is high potential for measuring the positions of stars
with high precision by using a CCD array and the algorithm proposed in this paper for our projects.
References[1] Yano, T., et al: 2004, PASP, 116, 667.
[2] Yano, T., et al: 2006, PASP, 118, 1448.

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An Interpretation of Flat Density Cores of Clusters of
Galaxies by Degeneracy Pressure of Fermionic Dark Matter:
A Case Study of A1689
NAKAJIMA, Tadashi

MORIKAWA, Masahiro(Division of Optical and Infrared Astronomy, NAOJ)(Ochanomizu University)

Flat density cores have been obtained for a limited
number of clusters of galaxies by strong gravitational lensing. Using a phenomenological equation of state (EOS)
describing the full-to-partial degeneracy, we integrate theequation of hydrostatic equilibrium [1]. The EOS is basedon an assumption that the local kinetic energy of a classicalparticle induced by the gravity dissolves the quantum statistical degeneracy. The density profile is uniquely determined by four parameters, the central density, t(0), theproperties of a fermion, namely, the mass, m, and statisticalweight, g, and the ratio of the total matter density andfermion density, d. As a case study, we model the column
density and 2D encircled mass profiles of A1689, whose
column density profile has been observationally obtainedby Broadhurst et al., using gravitational lensing. The column density and 2D encircled profiles at the core, are reasonably reproduced for models with a limited range of particle properties. In the case that previously unknown fermions with spin 1/2 dominate the dark matter, the acceptableparticle mass range is between 2 and 4 eV. In the case thatthe dark matter consists of the mixture of degenerate relicneutrinos and classical collisionless cold dark matter particles, the mass range of neutrinos is between 1 and 2 eV, if
the ratio of the two kinds of dark matter particles is fixed toits cosmic value. Both the pure fermionic dark matter models and neutrino-CDM-mixture models reproduce theobservations equally well (Table 1, Figures 1, 2).

Figure 1: Volume density profiles. Profile A corresponds to the highest
density model and profile B is the lowest density model andother model profiles lie between the two extremes. RC and RE
denote the radius of the radial critical curve and that of thetangential critical curve (or the Einstein radius), respectively.

Table 1: Solutions for the Mixture of Neutrinos and Nondegenerate
Cold Dark Matter.
t(B)/t(DM)

0.2
0.5

Particle Type g

o+o
o+o

6
6

(m, rt)eV, kpc(1.6,106) ~ (2.1,73)(1.1,106) ~ (2.4,73)

References

Figure 2: 2D encircled mass profiles for general fermionic dark matter.
The observed profiles and model profiles A and B are indistinguishable.

[1] Nakajima, T., Morikawa, M.: 2007, ApJ, 655, 135.

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Zenith-Distance Dependence of Chromatic Shear Effect:
A Limiting Factor for an Extreme Adaptive Optics System
NAKAJIMA, Tadashi(Division of Optical and Infrared Astronomy, NAOJ)
Consider a perfect AO system with a very fine wavefront sampling interval and a very small actuator interval. If
this AO system senses wavefront at a wavelength, mWFS ,and does science imaging at another wavelength, mSCI , thelight paths through the turbulent atmosphere at these two
wavelengths are slightly different for a finite zenith distance, z. The error in wavefront reconstruction of the science channel associated with this non-common path effect,
or so-called chromatic shear, is uncorrectable and sets anupper bound of the system performance. We evaluate thewavefront variance, v2(mWFS , mSCI , z) for a typical seeing
condition at Mauna Kea and find that this effect is not negligible at a large z [1]. If we require that the Strehl ratio begreater than 99 or 95%, z must be less than about 50 or 60º
respectively, for the combination of visible wavefront sensing and infrared science imaging (Fig. 1).
It is well known that a high-performance adaptive
optics system with a Strehl ratio well over 90% is required
for the direct detection of an exoplanet from the groundespecially in reflected light. Such an adaptive optics system
is often called an extreme AO system (ExAO), because of
its high level of sophistication in instrumentation. The
ExAO has strict requirements on guide stars and wavefront
sensors. Fine wavefront sampling is achieved by many pixels in the wavefront sensor, each of which corresponds tothe length scale less than cm. Fine temporal sampling is
also required along with the fine spatial sampling.
Therefore, a large number of photons are required for a tinyarea on the wavefront for a short period of time. So an AO
guide star must be very bright. Another requirement on theguide star is that it must be regarded as a point source, evenafter the AO correction, and a presently available laser
guide star, located at a finite altitude with a finite angularextent, is not fitted for this purpose, even if the problem ofbrightness or laser power is overcome. If the Strehl reduction due to the finite extent of the laser guide star isinevitable, there is no point of sampling the wavefront so
finely, in other words, there is no use of an ExAO. For thesame reason, a stringent requirement on isoplanicity will
result in a small field of view. For these reasons, the major
application of an ExAO requires a very bright natural guidestar and the high Strehl ratio is achieved only for a small
field of view. All things considered, an exoplanet searcharound bright nearby stars, will remain the primary scientific goal for an ExAO project.
There are many sources of errors that can cause the reduction of the Strehl ratio, but most of them are in principle con-6

trollable by sophisticated instrumentation. However, there arealso some errors which are in principle uncorrectable. Here
we focus on one of the major uncorrectable errors: atmospheric chromatic non-commonpath error, or “chromatic shear(CS)”, associated with the different paths through the turbulent atmosphere of the light beams incident on the visible
wavefront sensor and the infrared science imager, when thetarget star is at a finite zenith distance.
In actual astronomical observations, total observing
time for an object is finite and the object never stays at thezenith. Moreover, it often happens that an object needs tobe observed at a large zenith distance, due a large difference between the declination of the object and the latitudeof the observatory. In order to secure a significant amountof observing time for an exoplanet search, it is inevitable toobserve a target star with a finite zenith distance.
Most of the current AO systems sense wavefront at visible wavelengths and image the target at near-infrared
wavelengths. This is partly due to the higher availability ofa visible detector such as a CCD for a wavefront sensing
camera. However, if the CS effect is a significant limiting
factor for the next-generation extreme AO systems whose
scientific justification is direct exoplanet detection, thechoice of the combination of mWFS and mSCI , may need tobe reconsidered.
In this paper, we quantify the magnitude of this CS
effect, in terms of wavefront variance associated with it.

Figure 1: Wavefront variance due to atmospheric noncommon patheffect. mSCI = 1.65 µm. Assumed seeing condition is r0 = 0.2m
at m = 0.5 µm. The variance for an arbitrary r 0 can beobtained by shifting each curve vertically by (5/3)
log10(0.2/r0).
References[1] Nakajima, T.: 2006, ApJ, 652, 1782.

00eng 08.2.28 6:40 PM ページ7

A Nobeyama Millimeter Interferometric Search for Buried
Supermassive Blackholes in Luminous Infrared Galaxies
IMANISHI, Masatoshi(Division of Optical and Infrared Astronomy, NAOJ),

NAKANISHI, Kouichiro

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

Luminous infrared galaxies (LIRGs) radiate large luminosities (L > 1011L9 ) as infrared dust emission. The large
infrared luminosities mean that: (1) powerful energy
sources are present hidden behind dust; (2) energetic radiation from the energy sources is absorbed by the surrounding dust; and (3) the heated dust grains re-emit this energy
as infrared thermal radiation. To understand the nature of
LIRGs, it is essential to distinguish whether the hiddenenergy sources are starbursts and/or active galactic nuclei(AGNs; mass accreting supermassive blackholes). If luminous AGNs are present and obscured by dust in a torus
geometry, such obscured AGNs are easily detectablethrough optical spectroscopy, because AGN’s ionizing
radiation can escape along the torus axis direction.
However, since the nuclear regions of LIRGs are very
dusty, most of putative AGNs in LIRGs are likely to be
obscured by dust along all sightlines. It is fundamental toevaluate the energetic contribution from such buried AGNs
to LIRGs.
In an AGN, much stronger X-ray emission than a starburst is produced in the close vicinity of an accretion disk
around a central supermassive blackhole. Hence, detectionof a strong X-ray emitting source can be strong evidence
for the presence of a luminous AGN. Unfortunately, thebulk of buried AGNs in LIRGs are likely to suffer from
Compton thick (NH > 1024 cm–2) absorption, so that detection of directly transmitted X-ray emission is difficult withthe existing X-ray satellites, except a few nearby, bright
LIRGs. However, a luminous X-ray emitting buried AGN
can make chemical and physical effects to the surrounding
gas and dust, and can produce the X-ray dissociation
regions (XDRs). If XDRs show different flux ratios ofemission lines from photo-dissociation regions (PDRs) usually found in a starburst, they are distinguishable. We haveobserved several bright LIRGs at the HCN (J=1–0) andHCO + (J=1–0) lines at ~3.4 mm (89 GHz), using theNobeyama Millimeter Array (Figure 1), and found that
LIRGs which are diagnosed to be AGN (starburst)-poweredfrom our previous infrared spectroscopy tend to show
HCN/HCO+ brightness temperature ratios found in AGNs
(starbursts) (Figure 2). Since dust extinction is negligible inthe millimeter wavelength range, this millimeter method
can potentially be a powerful tool to unveil luminousburied AGNs in LIRGs in the ALMA era [1], [2].

Figure 1: HCN and HCO + spectra of LIRGs obtained with theNobeyama Millimeter Array.

Figure 2: Millimeter interferometric energy diagnostic method [3]. The
abscissa is HCN/CO ratio and the ordinate is HCN/HCO+
ratio in brightness temperature (?flux # m2). LIRGs diagnosed to be AGN (starburst)-powered through infrared spectroscopy tend to distribute in the AGN (starburst) range in thismillimeter-based diagram.
Reference[1] Imanishi, M. et al.: 2006, AJ, 131, 2888.
[2] Imanishi, M., and Nakanishi, K.: 2006, PASJ, 58, 813.
[3] Kohno, K.: 2005, astro-ph/0508420.

700eng 08.2.28 6:40 PM ページ8

Effects of Phase Characteristicsin Main Beam of Telescopes on Same-Beam VLBI
LIU, Qinghui, KIKUCHI, Fuyuhiko, TSURUTA, Seiitsu, MATSUMOTO, Koji, HANADA, Hideo
KAMEYA, Osamu, TAMURA, Yoshiaki, ASARI, Kazuyoshi, KAWANO, Nobuyuki(NAOJ)The Japanese SELENE project to be launched in 2007
consists of a main satellite, a relay sub-satellite (Rstar), anda VLBI sub-satellite (Vstar). The differential phase delay
between Rstar and Vstar will be obtained for the first timewith a very high accuracy of several pico seconds. Rstar
and Vstar only transmit three carriers at frequencies of
2.212, 2.218, and 2.287 GHz and one carrier at a frequencyof 8.456 GHz. The absolute difference in the correlation
phase at each frequency has to be estimated without 2π
ambiguity when obtaining the differential phase delay. Thisrequires the rms error of the differential correlation phase at
S-band to be lower than 0.075 radians.
To resolve the 2π-ambiguity problem, we will use
same-beam differential VLBI, in which Rstar and Vstar are
observed simultaneously using the main beam of each telescope [1]. Because the propagation paths of the radio
waves from Rstar and Vstar are nearly the same, the influence of the instrument, the atmosphere and the ionosphere
can nearly be canceled out. However, phase characteristics
across the main beam of the telescopes must not be neglected. Accurate measurement and correction for phase characteristics of the telescopes are thus key techniques forachieving same-beam differential VLBI.
We measured the phase characteristics at S-band of theMizusawa 20-m and 10-m telescopes by using geostationary satellites [2]. In the measurement, one telescope tracks
the satellite with a zero-offset angle, and the other scans for
12 paths as shown in Fig. 1(b). The phase characteristics ofthe telescope under test was obtained using the phase difference between the signals received by the two telescopes.
The phase characteristics were measured stepped radiallywith 29 points along each path. The measurements weremade in 1 minute for every point. The zero-offset point of
the telescope under test was observed repeatedly every 8
minutes to correct the time variation of the phase in thesystem itself.
Figure 1 shows the measured phase characteristics ofthe 20-m telescope for paths 1–12 measured at a freqencyof 2.2807 GHz and an EL of 44.8 degrees. They are nearly
constant up to an offset angle of about 0.4 degrees, where
they jump by about π. Figure 2(a) shows the phase characteristics in the main beam of the 20-m telescope. To correct
the phase characteristics across the main beam, we fitted
the measured results over all 12 paths to a single quadratic
in both AZ and EL. The results after correction are shownin Fig. 2(b). Within !0.3 degrees in both axes there is a significant improvement. Before correction, the phase characteristics lie between !0.1 radians with an overall rms of
0.06 radians. After correction, the phase characteristics lie
between !0.05 radians with an overall rms of 0.03 radians.

8

Figure 2(c) and (d) show the two-dimensional phasecharacteristics in the main beam of the 20-m telescope. The
phase characteristics shown in the upper left part of Fig.
2(c) is negative, whereas the phase characteristics in thelower light part are positive. After correction, the residual
phase characteristics are random. We also measured thephase characteristics at an EL of 30 degrees, the results are
similar for an EL of 44.8 and 30 degrees.
The phase characteristics were measured to an error of
about 0.04 radians rms. The phase characteristics in themain beam after correction is less than 0.03 radians rms forthe 20-m and 0.04 for the 10-m telescopes. This satisfies
the 0.075 radians rms required to resolve the 2π ambiguity
problem, and confirms the effectiveness of the same-beamdifferential VLBI technique for the VLBI observations of
SELENE.

Figure 1: Phase characteristics of 20-m telescope.

Figure 2: Phase characteristics in main beam of 20-m telescope (a)(c)before correction and (b)(d) after correction by quadratic formula.
References[1] Liu, Q., et al.: 2006, IEICE Trans. Commun., 89B, 602-617.
[2] Liu, Q., et al.: 2007, IEEE Trans., Antenna and Propa., 55, 5.

00eng 08.2.28 6:40 PM ページ9

A Search for CO (J = 3 – 2) Emission from the Host Galaxy of
GRB980425 with the Atacama Submillimeter Telescope Experiment
HATSUKADE, Bunyo, KOHNO, Kotaro, ENDO, Akira
OKUDA, Takeshi, MURAOKA, Kazuyuki, KAMEGAI, Kazuhisa(Univ. of Tokyo)

OHTA, Kouji

SAKAMOTO, Seiichi

KAWAI, Nobuyuki(Kyoto Univ.)(JAXA)(Tokyo Institute of Technology)

TOSAKI, Tomoka, NAKANISHI, Kouichiro, SAKAI, Takeshi(NRO, NAOJ)

CORTES, Juan R.

VREESWIJK, Paul M.

(Univ. of Chile)(ESO)

EZAWA, Hajime, YAMAGUCHI, Nobuyuki, KAWABE, Ryohei(Division of Radio Astronomy, NAOJ)
We report on a deep search for CO(3–2) line emission
from the host galaxy of GRB980425 with the Atacama
Submillimeter Telescope Experiment (ASTE) [1].
Long-duration gamma-ray bursts (GRBs) are considered to be due to the death of massive stars. Therefore,
GRBs are closely associated with the star formation of hostgalaxies. Since GRBs can be detected at cosmological distances, they are expected to be probes of the star formation
history of the Universe. In order to determine the use ofGRBs, it is essential to understand the star formation of
their hosts. Multi-wavelength observations have shown thatthe star formation rates (SFRs) of GRB hosts derived from
submillimeter/radio observations are generally higher thanthose from optical/UV observations [2], [3]. This implies
that GRB hosts have a large amount of molecular gas andmassive star formation obscured by dust. In order to solve
this problem, it is necessary to derive the SFRs in a method
which is independent of existing methods and not affectedby dust extinction.
We searched for CO(3–2) toward the host galaxy of
GRB980425 with the ASTE. This galaxy is the nearest
GRB host known to date (z = 0.0085), and the proximity
makes it the best target to detect CO emission. We
observed five points of the galaxy covering the entire
region. After combining all of the spectra, we obtained a
global spectrum with the rms noise level of 3.3 mK in Tmb
scale at a velocity resolution of 10 km s–1 (Fig. 1). No significant emission was detected, though we find a marginalemission feature in the velocity range corresponding to theredshift of the galaxy. We derive 3 v upper limits on the
global properties: the velocity-integrated CO(3–2) intensity
of ICO(3–2) < 0.26 K km s–1 by adopting a velocity widthof 67 km s –1 ; the H 2 column density of N(H 2 ) < 3 #1020cm–2; the molecular gas mass of M(H2) < 3 # 108 M9 ,by assuming a CO line luminosity to H2 molecular gas
mass conversion factor of XCO = 5.0 # 1020 cm–2 (K kms–1)–1; and the star formation rate of SFR < 0.1 M9 yr–1,
based on the Schmidt law. The SFR is consistent with theprevious results of Ha and mid-IR observations, thereby
suggesting that there is no significant obscured star formation in this galaxy.
Figure 2 shows the SFRs of GRB hosts derived by several methods (see [4] and references therein). The ordinate

Figure 1: Global spectrum at a velocity resolution of 10 km s–1. This
exhibits the global property of the host galaxy of
GRB980425. The rms noise level is 3.3 mK in Tmb scale.
Figure 2: Comparison of the
SFRs of GRB hosts determined by various observational methods. The ordinate is
the SFR derived by extinction-free methods, and theabscissa is the SFR from optical and UV. The open symbols are the SFRs that are corrected for extinction in thehost galaxies, and the solid
symbols are those that are notcorrected.

is the SFR determined from extinction-free wavelengths,
such as the CO line, radio/submillimeter continuum, IR,
and X-rays. The abscissa is the SFR determined from optical and UV. The majority of the GRB hosts are locatedabove the diagonal, implying that they have a large amountof molecular gas and massive star formation obscured bydust. This tendency is observed in LIRGs, ULIRGs, andsubmillimeter galaxies but not in normal spiral galaxies.
On the other hand, our study shows that the host galaxy of
GRB980425 shows a different trend. This suggests thatvarious GRB hosts exist in terms of the presence ofobscured star formation.
References[1] Hatsukade, B., et al.: 2007, PASJ, 59, 67.
[2] Le Floc’h, E., et al.: 2003, A&A, 400, 499.
[3] Berger, E., et al.: 2003, ApJ, 588, 99.
[4] Endo, A., et al.: 2007, ApJ, 659, 1431.

9

00eng 08.2.28 6:40 PM ページ10

Origins of Carbon-Enhanced Metal-Poor Stars
AOKI, Wako
(Division of Optical and Infrared Astronomy, NAOJ)
An important fact found by the surveys of metal-poorstars is that the fraction of Carbon-Enhanced Metal-Poor(CEMP) stars is significantly high in the low metallicity
range. At the solar metallicity, carbon-enhanced
Asymptotic Giant Branch (AGB) stars, which are evolved
low- and intermediate-mass stars, are known but their fraction is at most 1%. On the other hand, the fraction of
CEMP among metal-poor stars (e.g. [Fe/H]< –2) is estimated to be 10–20%. This class of stars includes the two
objects having the lowest abundances of heavy elements
known to date ([Fe/H]< –5), indicating the importance of
CEMP stars for understanding of the star formation andnucleosynthesis in the very early Universe. In order toinvestigate the origins of CEMP stars, we have been conducting measurements of chemical abundances for a large
sample of these objects since 2000 using Subaru TelescopeHigh Dispersion Spectrograph. A summary of our work is
given by Aoki et al. (2007)[1], in which following observational facts are reported:(1) About 80% of the sample (64 CEMP stars) show large
excesses of Barium (Ba), indicating the source of highabundances of carbon as well as heavy elements is thenucleosynthesis in AGB stars. Hence, the most importantorigin of carbon-excesses in CEMP stars is AGB stars.
However, since the objects we are now observing are not at
the AGB stage, we should be observing the companion
object that has received significant mass from the primary
AGB star that has already evolved to faint white dwarfs.
(2)The fraction of Ba-enhanced objects among CEMP stars
is dependent on metallicity: the fraction of Ba-normal
objects increases in the metallicity of [Fe/H]< –2.6 (Figure1). The two objects with [Fe/H]< –5 should be the extreme
examples of this class. The existence of such objects atlower metallicity is the second reason for the high fractionof CEMP stars, though their origins are still very unclear(see below).
(3) A majority of Ba-enhanced stars have carbon abundances similar to, or slightly lower than, the solar value(–1 <[C/H]K 0), and a clear cutoff exists at [C/H]~ 0. Thissuggests that AGB stars yield carbon abundances similar tothe solar value ([C/H]~ 0), which is mostly independent of
the metallicity, and the yields are now observed at the surface of the secondary star without significant dilution.
Such recent work revealed the classification of CEMP
stars, while the detailed understanding for each group is theongoing and future work. The detailed abundance patternsof heavy elements in Ba-enhanced stars, whose carbon isbelieved to be provided by AGB stars, give strong constraints on the models for the s-process in AGB stars. Some10

CEMP stars are already known to show abundance patterns
that cannot be explained by the current s-process models [2].
Such objects are important target to study the origins ofheavy elements in the universe. The Ba-rich CEMP stars
are believed to belong to binary systems, but that should be
confirmed by a long term monitoring of radial velocities.
Several CEMP stars having normal Ba-abundances
show excesses of a-elements compared to other metal-poorstars, suggesting these stars are produced from the material
polluted by unusual supernovae that yields high C/Fe
ratios. These are important objects to investigate the nucleosynthesis in the first generations of stars. Other Ba-normal
CEMP stars show no abundance anomaly except for carbon
and nitrogen. Understanding of such objects remains as a
future work.

Figure 1: Ba abundance ratios ([Ba/Fe]) as a function of iron abundances ([Fe/H]) for CEMP stars (filled circles). The symbols
with error bars indicate the results reported by Aoki et al. [1].
The open circles show the upper limit of Ba abundances for
CEMP with [Fe/H]# – 4. Normal stars (with no excess of carbon) are shown by crosses for comparison purposes. All but
one CEMP stars with [Fe/H]> –2.6 show excesses of Ba([Ba/Fe]> +0.5), while Ba-normal CEMP stars appear in thelower metallicity range.

References[1] Aoki, W., et al.: 2007, ApJ, 655, 492.
[2] Aoki, W., et al.: 2006, ApJ, 650, L127.

00eng 08.2.28 6:40 PM ページ11

Where did starburst occur and from where did it terminate
in E+A galaxies?
YAGI, Masafumi, HATTORI, Takashi

GOTO, Tomotsugu, YAMAUCHI, Chisato(NAOJ)(ISAS/JAXA)

We investigated stellar population in E+A galaxies byslit spectrometry.
E+A galaxy is a galaxy with strong Balmer absorption
and no emission lines. They are thought to be a poststarburst galaxy; experienced a strong starburst in 1 Gyr andterminated it abruptly. How the starburst started, and how it
stopped is not understood so far.
To answer the questions, we observed 3 E+A galaxies
from unbiased E+A sample [1] selected from SDSS catalog
with the Apache Point 3.5m telescope, and investigated the
distribution of young stellar population [2]. Spatiallyresolved spectra were obtained by taking several apertures
along the slit. Assuming that the light distribution of thegalaxies follow Sersic function, we deconvolved the PSF,
and showed that the extension of poststarburst region is notconfined in the core but rather extended in whole galaxy.
We also showed that required mass of starburst is only
~5% of old population to reproduce the observed spectra.
Our second study[3] is based on slit spectroscopy using
faint object camera and spectrograph (FOCAS) at theSubaru telescope. A nearby E+A galaxy (SDSS
J161330.18+510335.5; Fig 1) shows a tidal feature(plume),
and is apparently interactiong with its neighbour(Fig1,
Red). We confirmed that the two galaxies have almost thesame redshift, and they are a phisically interacting pair. We
also discovered that poststarburst signature, strong Balmer
absorption without any sign of starformation, exist not onlyin its core but also at 4 kpc from the core (Fig 2). It meansthat there had been a strong starburst in the plume and theburst suddenly stopped. Then, we made model spectrausing a stellar synthesis model (BC2003), assuming thatthe progenitor of the E+A is mildly starforming galaxy.
Investigating the models and the observed spectra in Hd vs
4000Å break (D4000) plane, we found that the age ofyoung population can be decoupled from the metal and theburst-strength (mass ratio of young population to old one)when the luminosity of young population is much stronger
than that of old population. It enable us to estimate the age
since the end of the burst approximately. Applying thismethod to the observed data, we found the sign that the endof the starburst is relatively later at the center than the outerpart (in the plume) in this galaxy. This result is consistent

with the fact that CaH-K ratio is larger at the center(x=0).
We concluded that the end of starburst propagated inward
in this galaxy.
More detailed study on this E+A, kinematics study andmetallicity distribution, is ongoing.

Figure1: Image taken from SDSS archive around SDSS
J161330.18+510335.5 (“Blue E+A”). Slit position is overplotted [3]. Tidal plume is extended to the bottom right.

Figure 2: Spatioally resolved spectra of E+A in Fig.1 [3]. Hd at ~4100Å
(rest) and Hc at ~4350Å (rest) are obvious. The unit of x is
[pixel], and x=+30 corresponds to ~ 4kpc, since the scale is0.13 kpc/pixel at this galaxy.
References[1] Goto, T.: 2003, Doctral thesis, University of Tokyo.
[2] Yagi, M. Goto, T.: 2006, AJ, 131, 2050.
[3] Yagi, M., Goto, T., Hattori, T.: 2006, ApJ, 642, 152.

11

00eng 08.2.28 6:40 PM ページ12

First light of the Laser Guide Star Adaptive Optics System:
10 times clearer vision for Subaru Telescope
TAKAMI, Hideki, HAYANO, Yutaka, WATANABE, Makoto, HATTORI, Masayuki
SAITO, Yoshihiko, OYA, Shin, TAKAMI, Michihiro, GUYON, Olivier, MINOWA, Yousuke
COLLEY, Stephen, ELDRED, Michael, DINKINS, Mathew, GOLOTA, Taras
CLERGEON, Christophe(Subaru Telescope, NAOJ)

and IYE, Masanori(ELT Project, NAOJ)
Even though the theoretical diffraction limit of an 8mclass telescope is 0.06 arcsec in the near infrared K-band,practical average seeing at Mauna Kea is about 0.6 arcsec,
10 times poorer than the ideal limit. Adaptive Optics is aninnovative technology to measure the wavefront errors dueto the turbulent atmosphere and correct them in real time toretrieve the diffraction limited imaging capability. The current group developed (1) an advanced adaptive optics system with 188 control elements based on their experiencesin constructing the 36-element AO system and (2) a laser
guide star generating facility for the Subaru Telescope. The
project was supported by the grant in aid for specially promoted research on “High resolution near infrared observations of distant universe by a laser guide star adaptive
optics system” led by M.Iye during the fiscal years 20022006. The left panel in Figure 1 shows the first light imageof Trapezium region in the Orion nebula taken by the 188element AO system on October 9, 2006. The breathtaking
resolution is evident when the image is compared with theimage on the right panel of Figure 1 obtained in 1999 using
a classical infrared camera during the first light epoch of
Subaru Telescope.
Figure 2: The first launching of the laser beam from Subaru Telescope.

about 100km above the site on October 12, 2006. These
successful results ensure that diffraction limited imaging
observations will become reality with Subaru Telescope
even for target fields where no bright natural guide star isavailable for the driving the AO system. A series of papers
reporting these achievements are published in [1]- [9].

Figure 1: 188 AO image(left) and non-AO image(right) of the trapezium region in the Orion nebula.

Figure 2 shows another impressive picture when the
powerful laser beam was launched for the first time from
Subaru Telescope to generate an artificial guide star at

12

References[1] Iye, M.: 2006, Proc. SPIE, 6269, 626905.
[2] Takami, H., et al.: 2006, Proc. SPIE, 6272.
[3] Hayano, Y., et al.: 2006, Proc. SPIE, 6272, 133.
[4] Hattori, M., et al.: 2006, Proc. SPIE, 6272, 62725G.
[5] Oya, S., et al.: 2006, Proc. SPIE, 6272, 62724S.
[6] Saito, Y., et al.: 2006, Proc. SPIE, 6272, 627246.
[7] Ito, M., et al.: 2006, Proc. SPIE, 6272, 627245.
[8] Guyon, O.: 2006, Proc. SPIE, 6272, 62723C.
[9] Hodapp, K. W., et al.: 2006, Proc. SPIE, 6269, 62693V.

00eng 08.2.28 6:40 PM ページ13

High-Dispersion and High-S/N Spectrum Atlas of Vega
TAKEDA, Yoichi, KAWANOMOTO, Satoshi, OHISHI, Naoko(NAOJ)
Vega has long been known for its low projected rotational
velocity (ve sin i of ~ 20 km s–1), which is rather unusual forsuch early-type stars (A0 V). However, the discovery ofanamolous “flat-bottomed” shape of weak lines, which was
revealed for the first time by the ultrahigh S/N (> 2000)
Reticon spectrum obtained at Dominion AstrophysicalObservatory [1], presented a new picture that the apparently
sharp-lined Vega is actually a rapid rotator seen nearly poleon and the peculiar line profile may be interpreted as due tothe rotation-induced latitude-dependent variation of stellar
surface properties [2, 3]. In fact, this view has got support at
least qualitatively from a recent interferometric observation of
Vega’s surface brightness distribution [4].
This does not mean, however, that we already have afully satisfactory understanding of this star. As a matter offact, from a quantitative point of view, any consensus has
not yet been accomplished regarding the nature of Vega’s
rotation, as the best solutions of (ve, i) suggested from thesestudies appreciably differ from each other: (245 km s–1,
5º.1; [2]), (160 km s–1, 7º.9; [3]), and (274 km s–1, 4º.5; [4]).
It is evident that much more work remains to be done inthis field.
Unfortunately, the ultra-high-S/N spectrum obtained at
Dominion Astrophysical Observatory [1], which has been
exclusively invoked so far [2, 3], is not placed in the publicdomain. We therefore decided to collect such similar highquality spectral data of Vega based on our own observations at Okayama Astrophysical Observatory, and to publish them as a digital spectrum atlas.
The spectroscopic observations were carried out on
2006 May 1–4 by using the HIDES Spectrograph attachedto the 188 cm reflector at Okayama AstrophysicalObservatory (OAO), which enabled us to obtain the data atfour wavelegth regions (region “b” of ~3900–5100 Å,region “g” of ~5000–6200 Å, region “r” of ~6000–7200 Å,and region “i” of ~7600–8800 Å). The data reduction was
performed with IRAF in the standard manner. The resolving power of the finally resulting spectra is R ~100000(corresponding to the slit width of 100 µm), and their typical S/N ratios are ~1000–2000 on the average as shown in
Figure 1.
We have made these very high-quality digital spectra ofVega freely available via on-line, the details of which aredescribed in [5]. The actual data are given in the form of

Figure 1: Estimated S/N ratios vs. wavelwength.

electronic tables to this paper, though also downloadablefrom the FTP site of the Astronomical Data Center of NAOJ:
ftp://dbc.nao.ac.jp/DBC/ADACnew/J/other/PASJ/59.245/
In addition, the theoretically simulated spectra based on the
spectrum synthesis, the list of lines predicted to have appreciable strengths, and the spectra of a rapid rotator (a Leo)for the removal of telluric lines, are also appended toincrease the usability of the atlas.
An example of comparison between our spectra andtwo other published spectra [6, 7] is presented in Fig. 2,
where we can recognize that our data are of so high quality
as to reveal the peculiar/characteristic profile shape seen invery weak lines.

Figure 2: Comparison with other published spectra.

References[1] Gulliver, A. F., et al.: 1991, ApJ, 380, 223.
[2] Gulliver, A. F., et al.: 1994, ApJ, 429, L81.
[3] Hill, G., et al.: 2004, in The A-Star Puzzle, Proc. IAU Symp. 224, 35.
[4] Peterson, D. M., et al.: 2006, Nature, 440, 896.
[5] Takeda, Y., et al.: 2007, PASJ, 59, 245.
[6] Allende Prieto, C., et al.: 2004, A&A, 420, 183.
[7] Moultaka, J., et al.: 2004, PASP, 116, 693.

1300eng 08.2.28 6:40 PM ページ14

ASTE Observations of Warm Gas in Low-mass Protostellar Envelopes:
Different Kinematics between Submillimeter and Millimeter Lines
TAKAKUWA, Shigehisa, KAMAZAKI, Takeshi, SAITO, Masao(ALMA Project Office, NAOJ)YAMAGUCHI, Nobuyuki

KOHNO, Kotaro(Nobeyama Radio Observatory, NAOJ)(Institute of Astronomy, University of Tokyo)

We report the first results of mapping observations of
low-mass protostellar envelopes in submillimeter CS(J=7–6; 342.9 GHz) and HCN (J=4–3; 354.5 GHz) lines
with ASTE [1]. ASTE is the first Japanese large (= 10 m)
submillimeter single-dish telescope at the Atacama Dessert,
northern Chile, where ALMA will be constructed [2].
Observational studies with ASTE should provide us withinvaluable insight for future studies with ALMA.
In Figure 1, we show total integrated intensity maps in
the HCN (J=4–3) and CS (J=7–6) lines toward one of thelow-mass protostars, L483, observed with ASTE. Thereappears a western extension both in the HCN and CS emissions, and the structures traced by these submillimeteremissions are resolved with ASTE. The deconvolved sizeof the HCN emission measured from a 2- dimensional
Gaussian fitting to the image is 5500 # 3700 (AU) (P.A. =78º), while in the CS emission only the major axis is
resolved (~ 2300 AU). This result suggest that these submillimeter emissions, which should trace gas temperatures
above ~ 40 (K) and densities above ~ 107 cm–3, can be
more extended than ~ 2000 AU in the low-mass protostellar envelope.

as N2H+ (1–0) [3]. The same results are also seen in anotherlow-mass protostellar envelope around B335 (Figure 3).
These results suggest that the submillimeter emissions havedifferent origin from that of the millimeter lines.
In summary, submillimeter molecular lines can be more
extended than expected, and trace different gas components
from those by millimeter lines in lowmass protostellar
envelopes. Detailed observations with ALMA should
unveil the origin of these submillimeter emissions in lowmass protostellar envelopes.

Figure 2: ASTE results of the velocity structure traced by the submillimeterCS (7–6) line in L483. (upper left) Total integrated intensity mapof the CS (7–6) emission in L483, shown in Figure 1. (lower left)
Position-Velocity diagram of the CS (7–6) line along the axis of
the associated molecular outflow in L483. Contour levels arefrom 2 v in steps of 2 v (1 v = 0.133 K). A dashed line delineates the detected velocity gradient. (right) CS (7–6) line profile
map at a grid spacing of 10" along the outflow axis in L483. A
star mark indicates the position of the protostar.

Figure 1: Total integrated intensity maps (integrated velocity range 4.2- 6.9 km s–1) of the HCN (4–3) (left) and CS (7–6) (right)
emission in L483, taken with ASTE. Contour levels are 2, 4,
6 v, and then 10 v in steps of 4 v (1 v = 0.0733 K km s–1).
The highest contour in the HCN map is 18 v and that in the
CS map 34 v. Crosses indicate observed positions, and open
circles at the bottom right corner beam sizes. Red and blue
arrows show the direction of the redshifted and blueshifted
molecular outflow, respectively, and he roots of the arrows
indicate the protostellar position.

Figure 2 presents the velocity structure traced by thesubmillimeter CS line in L483. Along the axis of the associated molecular outflow, the CS (7–6) line is redshifted at
the west of the protostar and blueshifted at the east. The
same velocity gradient is also found in the HCN (4–3) line.
Interestingly, this trend of the velocity gradient is opposite
to that of the molecular outflow, and that in the 3-mm
counterpart of the CS (2–1) line and other 3-mm lines such

14

Figure 3: Same as Figure 2 but for another protostar of B335.
References[1] Takakuwa, S., et al.: 2007, PASJ, 59, 1.
[2] Ezawa, H., et al.: 2004, Proc. SPIE, 5489, 763.
[3] Tafalla, M., et al.: 2000, A&A, 359, 967.

00eng 08.2.28 6:40 PM ページ15

Atomic Carbon in the AFGL 333 Cloud
SAKAI, Takeshi(Nobeyama Radio Observatory, NAOJ)

OKA, Tomoharu, YAMAMOTO, Satoshi(Department of Physics, University of Tokyo)

Figure 1: Integrated intensity maps of the C0 3P1 – 3P0 emission (a) andthe 12CO J=3–2 emission (b) observed toward the W 3 giant
molecular cloud.

The W 3 giant molecular cloud (W 3 GMC) is an active
star-forming site lied on the Perseus arm. It involves threestar forming clouds; W 3 Main, W 3(OH), and AFGL 333.
The three clouds exhibit different starforming activities inspite of their similarity in size and mass. The ratio of theinfrared luminosities inW3 Main, W 3(OH) and AFGL 333
is 1.0:0.25:0.07 [1], suggesting that AFGL 333 is lessactive than W 3 Main and W 3(OH). The W 3 Main and W
3(OH) regions have been studied extensively with observations at various wavelengths. In contrast, little attention has
been paid on the AFGL 333 region, probably because of its
weaker star-formation activity.
We have mapped the W 3 GMC in the C0 3P1–3P0 ([CI]492 GHz) and 12CO J=3–2 emission lines with the Mount
Fuji Submillimeter-wave Telescope. We found that the [CI]intensity is notably strong in the AFGL 333 cloud (Fig. 1a),whereas the 12CO J=3–2 intensity, which traces warm gas,
is relatively weak (Fig. 1b). In order to investigate an originof the bright [CI] emission toward the AFGL 333 cloud, we
have mapped the cloud in the CO J=1–0 isotopomer lines
by using the Nobeyama Radio Observatory (NRO) 45 m
telescope.
Figure 2 shows the integrated intensity maps of the [CI]and CO isotopomer lines and the peak temperature map of
12
CO J=1–0 toward the AFGL 333 cloud. We found thatthe [CI] emission mainly arises from the molecular cloud
traced by the 13CO and C18O lines. The C0 column density

Figure 2: Integrated intensity maps of the C0 3P1 – 3P0 emission (a), the13
CO J=1–0 emission (b), and the C18O J=1–0 emission (c) in
the AFGL 333 cloud, and a peak temperature map of the12
CO J=1–0 emission in the same region (d).

is found to be linearly correlated with the C0 column density. In addition, the [C0]/[CO] ratio tends to be higher in the
AFGL 333 cloud than in the W3(OH) cloud. These results
suggest the chemical youth of the AFGL 333 cloud relative
to the W3(OH) cloud.
If the chemical youth of the AFGL 333 cloud is responsible for the high N(C0)/N(CO) trend, it should also bereflected in the chemical composition of dense cores. From
this motivation, we observed the CCS and N2H+ lines with
the NRO 45 m telescope (CCS is abundant in the earlystage of chemical evolution, while N2H+ is abundant in thelate stage). The CCS line was detected only in the AFGL
333 cloud, and we found that the [CCS]/[N2H+] ratio ishigher in the AFGL 333 cloud than in the W3(OH) cloud.
This result along with the higher [C0]/[CO] ratio in the
AFGL 333 cloud indicates the chemical youth of the AFGL
333 cloud relative to the W3(OH) cloud. Since there is no
IRAS and cm sources toward the two clumps in the AFGL
333 cloud (see Fig. 2c), the clumps are chemically andphysically young. These clumps would be important targets
to study the early stage of massive star formation. Detailsof this study are described in [2].
References[1] Thronson, H. A., Jr., et al.: 1980, ApJ, 239, 533.
[2] Sakai, T., et al.: 2006, ApJ, 649, 268.

1500eng 08.2.28 6:40 PM ページ16

Nobeyama CO Atlas of Nearby Spiral Galaxies: Distributionof Molecular Gas in Barred and Nonbarred Spiral Galaxies
KUNO, Nario(Graduate University for Advanced Studies/Nobeyama Radio Observatory, NAOJ)

SATO, Naoko(Wakayama University)

NAKANISHI, Hiroyuki, TOSAKI, Tomoka(Nobeyama Radio Observatory, NAOJ)

HIROTA, Akihiko

SHIOYA, Yasuhiro

SORAI, Kazuo(University of Tokyo)(Ehime University)(Hokkaido University)

NAKAI, Naomasa

NISHIYAMA, Kota

VILA-VILARÓ, Baltsar(Tsukuba University)(Bisei Spaceguard Center)(NAOJ)

16

tion toward the center many times in the Hubble time.

Figure1: Histgrams of fin for SA and SAB+SB galaxies.
8SA
Number

6

4

2

0

SAB +SB
6

Number

We made a CO(1 – 0) mapping survey of 40 nearby
spiral galaxies with the Nobeyama 45-m telescope. The criteria of the sample selection were (1) RC3 morphologicaltype in the range Sa to Scd, (2) distance less than 25 Mpc,
(3) inclination angle less than 79º (RC3), (4) flux at 100 µm
higher than ~ 10 Jy, (5) spiral structure is not destroyed byinteraction. The maps of CO cover most of the optical diskof the galaxies. Using these data we have compared the distribution of molecular gas in barred and non-barred spirals
and investigated the influence of the bar. We confirmedthat the degree of the central concentration of moleculargas within the radius of the order of a bar length ( fin ) inbarred spirals is significantly higher than that in non-barredspirals (Figure 1). This is contrast with the degree of theconcentration of the total molecular gas mass within theradial distances of the order of the bar ( fout ), which is similar for both barred and non-barred spirals (Figure 2). Thisimplies that the bars appear to be efficient in driving gasthat lies within their radial scales toward the center of thehost galaxies, but that they play quite a smaller role at larger spatial scales on the disks. Thus the characteristic featureof the radial distribution of molecular gas seen in barredspirals, i.e. the strong intensity peaks at their centers, theshallow gradients within the bar regions or/and the secondary peaks at the radius of the bar-ends, can be explained by
the accumulation of molecular gas within the bar regions.
The accumulated gas by bars accounts for about half ofmolecular gas within the central region. We also found acorrelation between the degree of central concentration ofmolecular gas, fin , and the bar strength. Galaxies withstronger bars tend to have higher central concentrations. A
correlation between the degree of central concentrations ofmolecular gas and the abundance gradient of heavy elements was also found. Galaxies with higher fin have shallower abundance gradient. These results indicate thatstronger bar accumulate molecular gas toward the center
more efficiently. The correlation between the degree ofcentral concentration of molecular gas and the strength
seem to be consistent with long-lived bars rather thanshort-lived ones which are destroyed by the gas accumula-

4

2

0
0.1

0.3

0.5

0.7

0.9

1.1

fout
Figure2: Histgrams of fout for SA and SAB+SB galaxies.
References[1] Kuno, N., et al.: 2007, PASJ, 59, 117.

00eng 08.2.28 6:40 PM ページ17

Luminosity Dependent Evolution of Lyman Break Galaxies :UV Luminosity Functions from redshift 5 to 3
IWATA, Ikuru1, OHTA, Kouji2, TAMURA, Naoyuki3, AKIYAMA, Masayuki3, AOKI, Kentaro3
ANDO, Masataka2, KIUCHI, Gaku2, SAWICKI, Marcin2,4(1: Okayama Astrophysical Observatory, NAOJ, 2: Dept. Astronomy, Kyoto Univ.,
3: Subaru Telescope, NAOJ, 4: St. Mary’s Univ.)
The development of large ground-based telescopes andsensitive large format detectors, as well as the develepmentof various techniques for the selection of high-z galaxies
enabled us to construct large samples of galaxies in theearly universe. The next major step for the comprehensive
understanding of galaxy evolution would be to explore therelationship of galaxies selected with different criteria at
different epochs and find links between them. Here wefocus on the evolution of Lyman break galaxies, which arethought to be actively star-forming galaxies with relatively
small amount of dust attenuation. The properties of Lyman
break galaxies (LBGs) at z~5 obtained by deep and wide
blank field surveys are presented, and through the comparison with samples at lower redshift ranges (z=4 and z=3) we
discuss the evolution of star-forming galaxies in the early
universe.
Our z~5 LBG sample is based on surveys for the two
independent blank fields (the region including the Hubble
Deep Field - North and the J0053+1234) obtained with theSuprime-Cam attached to the 8.2m Subaru Telescope. The
total effective area after masking bright objects is 1,300
arcmin2, and deep V , Ic and z'-band imaging enabled us tosecurely select V - dropout objects down to z'AB=26.5 mag(for the HDFN region) or 25.5 mag (for the J0053+1234
region). The number of z~5 LBG candidates in our sample
is 850. It should be emphasized that the area coverage of
our survey is more than 100 times wider than the ACS fieldof the Hubble Ultra Deep Field and more than 4 times
wider than the total area covered by the GOODS, and thiswide field coverage has a crucial importance for reliable
determination of the abundance of luminous objects. Thus
our survey is able to explore both bright and faint parts of
the LF reliably. The redshifts of a number of our LBG candidates have been spectroscopically determined, and thevalidity of our color selection criteria have been confirmed.
In figure 1 we show the UV luminosity function (LF) of
LBGs at z ~ 5 derived from our sample with filled circles
and a solid line [1]. In this figure we also show the UVLF
of LBGs at z ~ 4 and 3 based on the very deep survey(Keck Deep Fields; [2]). We found that in the luminous endof the UV LF there is no significant evolution from z ~ 5 to
3 (c1 Gyr), while in the fainter part, the gradual increase of
number density is observed. This clear contrast in the UV
LF suggests that the evolution of the LBGs is differential,
depending on UV luminosity.
In spectroscopic follow-up observations we also foundFigure 1: LBG UV luminosity function from z=5 to 3. Data for z=3 and
4 are taken from [2] and [4].

that equivalent widths of Ly-a emission for star-forming
galaxies at z = 5–6 show a strong dependence on UV luminosity [3]: UV luminous objects have weak or no Ly-aemission, suggesting that they are either in relatively dusty
environment or are enshrouded by massive HI gas haloes.
We suggest that the evolution of star-forming galaxies in
the first 2 Gyr of the universe could be well described withthe biased evolution scenario: a galaxy population hosted
by massive dark haloes start active star formation preferentially at early time of the universe, while less massive
galaxies increase their number density later. To understandthe origin of this differential evolution would be an important clue to clarify the star formation process in the early
universe.
The details of this work can be found in [1] and [3].
References[1] Iwata, I., et al.: 2007, MNRAS, 376, 1557.
[2] Sawicki, M., Thompson, D.: 2006, ApJ, 642, 653.
[3] Ando, M., et al.: 2006, ApJ, 645, L9.
[4] Steidel, C. C., et al.: 1999, ApJ, 519, 1.

17

00eng 08.2.28 6:40 PM ページ18

First Infrared Imaging Polarimetry of b Pictoris
TAMURA, Motohide, SUTO, Hiroshi, ABE, Lyu(NAOJ)

FUKAGAWA, Misato(Nagoya University)

KIMURA, Hiroshi, YAMAMOTO, Tetsuo(Hokkaido University)
One of the most exciting news from IRAS launched in1983 was that some main-sequence stars were associatedwith large infrared excesses (IRE). This was interpreted as
the presence of circumstellar dust which is considered to be
debris of planetary formation. As a consequence of followup observations from the ground, Smith and Terrile discovered the dust disk around b Pic [1]. This result is regarded
as one of the most important discoveries in witnessing aphase of planetary formation.
A number of main-sequence stars with similar IRE havebeen discovered, and they are known as Vega type stars. At
present, those disks are not regarded as the “debris” of protoplanetary disk but are rather secondary; they are due tocollisions of smaller bodies. (Thus, they are indeed a kindof “debris”).
However, the progress of direct observations of suchdebris disks has been slow since the b Pic, especially at
optical and near-infrared wavelengths. Although there aresome observations with the Hubble Space Telescope andthe adaptive optics on the 4-m class telescopes, no nearinfrared polarimetry or no observations with 8-m class telescopes have been conducted yet. This is because the central
stars of Vega-like stars are too bright to directly observe
their circumstellar structures (b Pic is a 4th magnitude starat a distance of 19 pc).
In order to resolve this contrast problem and to observe
structures near bright stars, we have observed b Pic with
the Subaru 8-m telescope, adaptive optics, coronagraph,and a polarimeter (Figure 1) [2]. This is the first case thatcombined adaptive optics, coronagraph, and polarimetry,simultaeously.
Our main results are summarized as follows [3]:• Polarization of ~10% is detected out to r~120 AU with acentrosymmetric vector pattern around the central star,confirming that the disk is seen as an infrared reflection
nebula.
• We have modeled our near-infrared and previous opticalpolarization results in terms of dust scattering in the disk
and argue that the observed characteristics of the disk
dust are consistent with the presence of ice-filled fluffy
aggregates consisting of submicron grains in the b Pic
system.

18

Figure 1: Polarization vector map in K band, overlaid with intensity
contours. The intensity contours are created from the Stokes I
parameter.

• Our results are indicative of the presence of multiple
planetesimal belts.
References[1] Smith, B. A., Terrile, R. J.: 1984, Science, 226, 1421.
[2] Tamura, M., Fukagawa, M., Murakawa, K., et al.: 2003, SPIE, 4843, 190.
[3] Tamura, M., Fukagawa, M., Kimura, H., et al.: 2006, ApJ, 641, 1172.

00eng 08.2.28 6:40 PM ページ19

Infrared Imaging Polarimetry of the Orion Nebula
TAMURA, Motohide, KANDORI, Ryo, NAKAJIMA, Yasushi(NAOJ)KUSAKABE, Nobuhiko

HASHIMOTO, Jun(GUAS)(Tokyo University of Science)

NAGASHIMA, Chie

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

KIMURA, Hiroshi, YAMAMOTO, Tetsuo

HOUGH, J. H., LUCAS, P., CHRYSOSTOMOU, A.

(Hokkaido University)(University of Hertfordshire)

BAILEY, J.
(Macquarie University)
SIRPOL is the polarization mode of the three-band
simultaneous camera SIRIUS [1] on the 1.4-m telescope,
IRSF, situated in SAAO, South Africa. The development of
the polarimeter started in FY2005 and the linear polarization mode had its first light in 2005 December [2] and thecircular polarization mode in 2006 December.
Near infrared imaging polarimetry is important to study
dusty star forming regions and late-type stars as well as the
Galactic center and star forming galaxies by revealing thedust scattering and absorption. In particular, it provides
crucial information on illuminating YSOs which form
infrared reflection nebulae, thus enabling us to understandthe “geometry” of the regions. We can also obtain information of magnetic fields by observing background stars.
However, in spite of its usefulness, the “wide-field”
infrared polarimetry has been scarcely conducted becauseof the lack of the appropriate polarimeter. Even toward themost famous Orion star forming cloud, the regions studied
with polarimetry was very limited.
Figure 1 (left) shows JHKs color composite images ofM42. It was reproduced from the Stokes I parameterobtained with SIRPOL. Figure 1 (right) shows the same but
in polarized intensities (intensity I # P). One could easily
notice the prominent difference between the two. Even thisone-field data is the widest infrared polarization image.
Our main results from the polarization data are summarized as follows [3]:• We detected various circumstellar structures as infrared
reflection nebulae (IRNe) around young stellar objects(YSOs), both massive and low mass. We found the IRN
around both IRc2 and BN to be very extensive, suggesting that there might be two extended bipolar/monopolar
IRNe in these sources.

Figure 1: Near-infrared three-color composite images of the Orion
Nebula (M42) in intensity (left) and in polarized intensity(right). North is up, and east is to the left. The images are in
logarithmic scale.

• We discovered at least 13 smaller scale (~0.01 to 0.1 pc)
IRNe around less massive YSOs, including the famous
source i2 Ori C.
• We also suggest the presence of many unresolved (<690
AU) systems around low-mass YSOs and young browndwarfs showing possible intrinsic polarizations.
Wide-field infrared polarimetry is thus demonstrated to
be a powerful technique in revealing IRNe and hence
potential disk/outflow systems among high-mass to substellar YSOs. The information of the magnetic fields will be
discussed elsewhere.
References[1] Nagayama, T., Nagashima, C., Nakajima, Y., et al.: 2003, SPIE,
4841, 459.
[2] Kandori, R., Kusakabe, N., Tamura, M., et al.: 2006, SPIE, 6269,
626951.
[3] Tamura, M., Kandori, R., Kusakabe, N., et al.: 2006, ApJ, 649, L29.

19

00eng 08.2.28 6:40 PM ページ20

Development of a multi-Fourier-transform interferometer:
fundamentals
OHTA, Izumi S., HATTORI, Makoto

MATSUO, Hiroshi(Institute of Astronomy, Tohoku University)(NAOJ)We report the fundamentals of Multi-Fourier Transform
interferometer(MuFT). MuFT is an aperture synthesis interferometer using direct detector in millimeter and sub-millimeter bands. We report Fundamentals of observation by
MuFT in this article[1].
MuFT is a kind of bolometric interferometer applying
Fourier transform spectroscopy in aperture synthesis technique. This idea was researched for Double-Fourier system
in near-infrared from the end of 1980s[2][3]. In this addition, MuFT is also able to measure polarimetry, as follow.
This is a reason of call this system ‘Multi- Fourier’. Figure
1 is simplified schematic diagram of a MuFT. Light from

Figure 2: Two basic configurations of wire grid 1 and 2. Left figure is
Option.1 (WGs are parallel) and right figure is Option.2. Graylines are light path (WGs are perpendicular).

penetrates in the direction of the wire, and a parallel electric field element reflects. In these reason, MuFT has two
advantages. First, MuFT performs wideband imaging andspectroscopy. Second, by combining WGs adequately,
source intensity distributions of four Stokes parameters canbe acquired in a wide band as equation (1),I (i, o) ! Q (i, o)
I Op1 = 1 # d 2 i # doA o (i)4 X
2v<1 + cos 2r c _ b $ i - 2x i F ,Figure 1: Simplified schematic diagram of a MuFT. Wavefront divisionof the source light is performed by the LiC. The divided
waves are combined by the FI through optical systems. Theinterferogram is measured by the DeS. Bol is Bolometer.

the object is been wavefront division. These beams arerecombined after modulation of one of the light path
lengths to make an internal time lag. Modulation signal isdetected by a direct detector system. This signal isexpressed as a mutual coherence function of the apertures
position (baseline vector) and an internal time lag.
However this function is real function, Fourier transformed
function to the time lag is expressed as a baseline vector
and frequency. This function has phase information except
at spectra. A physical explanation of the observability ofcomplex visibility by the MuFT is given.
A wire grid polarizer (WG) is used as a beam splitter inthis system. So the wavelength dependence of the reflectivity and transmissivity of a WG is small and is suitable for awide-band measurement system. The wire grid makes
polarization light that an orthogonal electric field element20

I Op2 = 1 # d 2 i # doA o (i) 1 8 I _ i, v i
2 X2+ e u _ i, v i cos < 2r vc _ b $ i - 2x i FV! v _ i, v i sin < 2r vc _ b $ i - 2x i F o WW ,X

（1）equations (1) are interference signal in each optical option,
I, Q, u, o is Stokes parameter, i is 2D position, and x is
distance of moving mirror.
We already in acquiring the mutual coherence signal foran extended source in broadband at laboratory experiment.
2D source images for each frequency from 5 cm–1 (150GHz) to 35 cm–1 (1.05 THz) with a wavenumber interval of
0.4 cm–1 (12 GHz) were successfully extracted[4]. The test
astronomical observation using MuFT is in progress at
Nobeyama Astronomical observatory.
References[1] Ohta, I., et al.: 2006, Appl. Opt., 45, 2576.
[2] Itoh, K., Ohtsuka, Y.: 1986, J. Opt. Soc. Am. A, 3, 94.
[3] Mariotti, J.-M., Ridgway, S. T.: 1988, A&A, 195, 350.
[4] Ohta, I., et al.: 2007, Appl. Opt., 46, 2881.

00eng 08.2.28 6:40 PM ページ21

Neutrino-Nucleus Reactions based on New Shell Model
Hamiltonians
SUZUKI, Toshio

CHIBA, Satoshi

YOSHIDA, Takashi(Nihon University/NAOJ)(JAEA)(NAOJ)

KAJINO, Toshitaka

OTSUKA, Takaharu(NAOJ/University of Tokyo)(University of Tokyo)

Figure 1: Calculated cross sections for neutrino 12C reactions inducedby supernova neutrinos with temperature T obtained by using
the SFO and PSDMK2 Hamiltonians. Both (a) the chargeexchange reactions and (b) the neutral current reactions aretreated. Previous calculations of Ref. [9] are also given.

A new shell model Hamiltonian for p-shell nuclei [1]which properly takes into account important roles of spinisospin interactions is used to obtain cross sections of neutrino-12C reactions induced by decay-at-rest (DAR) neutrinos as well as supernova neutrinos [1].
Our new shell model Hamiltonian (SFO) can describe
well the exclusive Gamow-Teller transitions in 12C as wellas magnetic moments of p-shell nuclei [2]. It is shown tohave proper tensor components, which have attractive(repulsive) nature for the monopole matrix elements with
j1 = j > and j2 = j < ( j1 = j2 = j > or j1 = j2 = j<).
This is consistent with the general robust nature of the tensor interaction [3]Charge-exchange and neutral current neutrino nucleus
reaction cross sections for 12C induced by the DAR neutrinos [4-6] are shown to be well reproduced by our new shellmodel Hamiltonian. The exclusive reaction is induced by
the Gamow-Teller transition, which is well described by
the SFO Hamiltonian. For the inclusive reaction, a large
quenching is needed in the spin-dipole transitions with J=2–
to explain the data, which is consistent with the observations in electron scaterings [7].
Reactions induced by supernova neutrinos are also
investigated (see Fig. 1). Branching ratios to various decay
channels, including neutron and proton knock-out processes, are calculated by the Hauser-Feshbach theory. Neutrino-4He reactions are also investigated by using recent shellmodel Hamiltonians such as WBP [8]. The reaction crosssections are found to be enhanced for both 12C and 4Hecompared with previous calculations [9](see Figs. 1 and 2).
As an interesting consequence of this enhancement in
the cross sections, a possible enhancement of the production yields of light elements, 7Li and 11B, during supernova
explosions is pointed out. The neutral current reactions,Figure 2: Calculated (a) charge-exchange and (b) neutral current reaction cross sections for o-4He reactions obtained by using the
WBP and SPSDMK Hamiltonians. Previous calculations ofRef. [9] are also shown.

Figure 3: Nucleosynthesis path of light elements 7Li and 11B during supernova explosion [10].
12C (o, o´p) 11B and 12C (o, o´n) 11C, are important for the
production of 11B. The enhancement of these cross sections
lead to those of the abundance of 11B. The reactions, 4He(o, o´p) 3H and 4He (o, o´n) 3He are important for the production of 7Li through 3H (a, c) 7Li and 3He (a, c) 7Be (e–,oe) 7Li processes. When the o- 4He reaction cross sections
are enhanced, the abundances of both 7Li and 11B are
increased as the abundance of 11B is affected by that of 7Li
through 7Li (a, c) 11B etc. Compared to the case by previous cross sections (HW92), the abundances of 7Li and 11B
are found to be enhanced by a factor of 1.30 and 1.19,
respectively, for WBP+SFO.

References[1] Suzuki, T., et al.: 2006, PRC, 74, 034307.
[2] Suzuki, T., et al.: 2003, PRC, 67, 044302 .
[3] Otsuka, T., et al.: 2005, PRL, 95, 232502.
[4] Auerbach, L. B., et al.: 2001, PRC, 64, 065501.
[5] Bodmann, B. E., et al.: 1994, PL, B332, 251.
[6] Armbruster, B., et al.: 1998, PL, B423, 15.
[7] Gaarde, C., et al.: 1984, NP, A422, 189.
[8] Warburton, E. K., et al.: 1992, PRC, 46, 923.
[9] Woosley, S. E., et al.: 1990, ApJ, 356, 272.
[10] Yoshida, T., et al.: 2006, ApJ, 649, 319.

2100eng 08.2.28 6:41 PM ページ22

Nonlinear Hydromagnetic Wave Support
of a Stratified Molecular Cloud. II.
a Parameter StudyKUDOH, Takahiro

BASU, Shantanu(NAOJ)(UWO)

We have performed 1.5-dimensional numerical simulations of nonlinear MHD waves in a gravitationally stratified molecular cloud that is bounded by a hot and tenuous
external medium [1].
Using the same basic model as presented in Paper I [2],we have carried out a parameter survey by varying the frequency of the driving force and the magnetic field strengthof the cloud. Under the influence of a driving source of
Alfvénic disturbances, a cloud shows significant upwardand downward motions, with an oscillation time scale thatis comparable to the cloud crossing time. We found that the
key parameter for the evolution of the cloud is the Alfvén
wavelength of the driving force. If the wavelength is larger
than the size of the cloud, the cloud is affected less by thewaves. The wavelength that is the same order of the cloudsize is the most effective in expanding the cloud (Fig.1).

This means that turbulent expansion is different than theusual notion of expansion due to a “turbulent pressure” inwhich the wavelengths need to be much smaller than thecloud size.
The line-width–size relation [3],
1/2

0.5

G v 2 Ht ? G z Ht,

(1)

is obtained by an ensemble of clouds with different physical parameters which are individually in a time-averaged
self-gravitational equilibrium state (Fig.2). The largest
amplitude random motions occur in the outer low density
regions of a stratified cloud.

Figure 2: Time averaged velocity dispersions (Gv2H1/2t ) of different
Lagrangian fluid elements for different parameters as a function of time averaged positions (GzHt). The open circles correspond to Lagrangian fluid elements whose initial positions arelocated at z = 2.51H0, which is close to the edge of the cold
cloud. The filled circles correspond to Lagrangian fluid elements whose initial positions are located at z = 0.61H0, which
is approximately the half-mass position of the cold cloud. The
0.5
dotted line shows Gv2H1/2
t ? GzHt .

Figure 1: The time evolution for different frequencies ( ṽ0 = 0.5, ṽ0 = 1,ṽ0 = 2) with the same parameters of ãd = 30 and b0 = 1. The
upper panels show the time evolution of density. The density
profile at various times are stacked with time increasing
upward in uniform increments of 0.2t0. The lower panels
show the time evolution of v´y at z = 0.

22

References[1] Kudoh, T., Basu, S.: 2006, ApJ, 642, 270.
[2] Kudoh, T., Basu, S.: 2003, ApJ, 595, 842.
[3] Solomon, P. M., et al.: 1987, ApJ, 319, 730.

00eng 08.2.28 6:41 PM ページ23

ASTE CO(3-2) Observations of the Barred Spiral Galaxy M 83
MURAOKA, Kazuyuki, KOHNO, Kotaro, OKUDA, Takeshi, ENDO, Akira
KAMEGAI, Kazuhisa, TANAKA, Kunihiko(Institute of Astronomy, University of Tokyo)

TOSAKI, Tomoka, KUNO, Nario, NAKANISHI, Kouichiro, SSAKAI, Takeshi

SORAI, Kazuo(Nobeyama Radio Observatory, NAOJ)(Hokkaido University)

SAKAMOTO, Seiichi, JUAN, Cortes, EZAWA, Hajime, YAMAGUCHI, Nobuyuki, KAWABE, Ryohei(NAOJ)

Figure 1: A contour map of the CO(J = 3–2) peak brightness temperature. Countours are at 0.2, 0.3, 0.4, 0.5, 0.7, 0.9, 1.1, 1.3, 1.5
K, and the peak is 1.53 K. Major structures, i.e., the nucleus,bar, and inner spiral arms are clearly resolved.

Figure 2: (top) Azimuthally averaged Star formation rate as a functionof the galactocentric radius of M 83. (bottom) Azimuthally
averaged Star formation efficiency and R3–2/1–0 as a functionof the galactocentric radius of M 83.

We report wide-area observations of CO(J = 3–2) line
emission using the Atacama Submillimeter Telescope
Experiment (ASTE) towards the whole inner disk of M 83
(NGC 5236) [1].
The CO(J = 3–2) emission can trace the dense component of molecular clouds (nH2 ~ 1 # 104cm–3), which is
directly linked to star formation.
M 83 is a nearby, face-on, barred spiral galaxy hosting
an intense starburst at its center. The distance to M 83 isestimated to be 4.5 Mpc; so 1" corresponds to 22 pc. The
inclination of M 83 is 24º. Its proximity and face-on view
enable us to resolve its major structures such as the nuclear
starburst region, bar, and inner spiral arms even by singledish observations at millimeter or submillimeter wavelength. Therefore, M 83 is the best target to investigate thespatial variations of star formation effi- ciency (defined asstar formatino rate per unit gas mass; hereafter SFE) andthe physical state of the molecular gas between the nuclear
region and the disk region.
Figure 1 shows a peak temperature map of the CO(J =3 – 2) emission of M 83. Significant emission was detected
at the nucleus, bar, and inner spiral arms. We successfully
resolved these structures at a resolution of 22". This is thefirst map that clearly depictsthe distribution of CO(J = 3 –2) emission in the disk region of M 83 including spiralarms However, no significant emission lines were detectedin the inter-arm region.
Figure 2 shows azimuthally averaged star formation

rate, SFE, and CO(J = 3 – 2)/CO(J = 1 – 0) ratio (R3–2/1–0)
as a function of the galactocentric radius of M 83. The
average R3–2/1–0, at the 22" resolution was ~ 1 at the centerof M 83 (r < 0.5 kpc). The ratio drops to a constant value,
0.6–0.7, through the disk region (0.5 < r < 3.5 kpc). Thisimplies that molecular gas is denser at the nucleus than disk
region. The radial pro- file of the SFE, determined from 6
cm radio continuum and the CO(J = 1 – 0) emission, shows
the same trend as R3–2/1–0 ; i.e., the SFE shows a strong
peak at the nucleus (r < 0.25 kpc), whereas it drops to a
constant value in the disk region (0.5 < r < 3.5 kpc).
At the bar-end of M 83 (r ~ 2.4 kpc), the amounts ofmolecular gas and the massive stars are enhanced, whereas
there is no excess of R3–2/1–0 and SFE in that region unlike
its center. This means that the presence of nuclear starburst
is not only due to the enhancement in the gas mass but also
due to the enhancement in the ef- ficiency of star formation. In other words, a simple summation of the star forming regions at the bar-end (and the disk region) cannot
reproduce the nuclear starburst of M 83. These results
could suggest that the spatial variation of the dense gas
fraction traced by R3–2/1–0 governs the spatial variation of
SFE in M 83.
References[1] Muraoka, K., et al.: 2007, PASJ, 59, 43.

23

00eng 08.2.28 6:41 PM ページ24

ASTE Observations of Nearby Galaxies : A Tight
Correlation between CO(J = 3–2) Emission and Ha
KOMUGI, Shinya1,3, KOHNO, Kotaro1, TOSAKI, Tomoka2, NAKANISHI, Hiroyuki2
ONODERA, Sachiko1, EGUSA, Fumi1, SOFUE, Yoshiaki1(1Institute of Astronomy, University of Tokyo, 2Nobeyama Radio Observatory, NAOJ, 3ALMA Project Office, NAOJ)
Star formation rates (SFRs) obtained via extinction corrected Ha are compared to dense gas as traced by 12CO(J =3–2) emission at the centers of nearby galaxies, observedwith the ASTE telescope.
The present knowledge of star formation on galactic
scales in relation with its precursor gas is generally
expressed by the Schmidt law, SFR ? tN where SFR is thestar formation rate, t the gas density, and N the Schmidt
law index, expressing the efficiency of star formation fromgas. Often written also in terms of surface averaged quantities (e.g., [1]), the equation above relates two physical values SFR and t which are generally spatially decoupledwhen observed locally, and connected in a spatially averaged sense. The connection between the two values also
have a time averaged nature, namely the formation
timescale of massive stars. Therefore, in order to obtainvalid physical suggestions from the Schmidt law, we mustderive these two values based on measurements which
express conditions that are spatially and temporally connected as much as observations allow.
The main objective and result of this paper is to examine the correlation between 12CO(J = 3–2) tracing warm
dense gas (typically ~ 30K), and extinction corrected Haluminosity tracing accurately the SFR, both in surface averaged densities.

Figure 1: 12CO(J = 3–2) spectra of NGC 1022 observed at ASTE.

Observation of the 12CO(J = 3–2) at 345GHz was conducted using the Atacama Submillimeter Telescope
Experiment (ASTE), a 10m single dish located in the
Atacama desert of altitude 4800m in Pampa La Bola, Chile.
Figure 1 shows a spectra from one of galaxies observed at

24

Figure 2: The obtained Schmidt law for the sample galaxies, using combinations of gas (12CO(J = 1–0) and 12CO(J = 3–2), and SFR withand without internal extinction correction. The lower right handpanel is best correlated, with N = 1.0 shown as the best fit line.

ASTE. A total of 9 galaxies were observed towards 14
pointings.
Figure 2 shows the obtained Schmidt law between
extinction corrected Ha and 12CO(J = 3–2). For comparison, we also show the relation between 12CO(J = 1–0)
and Ha. 12CO(J = 1–0) data are taken from similar resolution (16" or 22") surveys ([2] and references therein).
Apparently, a combination of extinction corrected SFR anddense gas gives a better correlation.
Interpreting this result in a qualitative manner is easy.
Assuming that star formation occurs where gas density
exceeds a certain value, we can expect that 12CO(J = 3–2)
is more spatially and temporally connected to star formation compared to 12CO(J = 1–0). By using Ha as a SFR
tracer, the spatial connection (resolution) and temporal connection (traces SF over 106 years) are even more improved.
This improvement should show up in terms of the Schmidt
law. The best fit slope of N = 1.0 suggests that dense gas
observed here traces and counts the individual units of starformation sites., as implied by [3].
References[1] Komugi, S., et al.: 2005, PASJ, 57, 733.
[2] Komugi, S., et al.: 2006, IAU Symposium, 237.
[3] Wu, J., et al.: 2005, ApJL, 635, L173.

00eng 08.2.28 6:41 PM ページ25

Neutrino Oscillation Effects on Supernova Light-Element Synthesis
YOSHIDA, Takashi, KAJINO, Toshitaka

YOKOMAKURA, Hidekazu, KIMURA, Keiichi(Division of Theoretical Astronomy, NAOJ)(Nagoya University)

TAKAMURA, Akira

HARTMANN, Dieter, H.

(Toyota National College of Technology)(Clemson University)

Figure 1: Mass fraction distribution of 7Li in the normal mass hierarchy
as a function of the mass coordinate in units of M9. Thicklines and thin lines correspond to the mass fractions of 7Li
and its isobar 7Be, respectively. Solid lines and dashed lines
correspond to the cases of sin2 2i13 = 1 # 10–2 and 1 # 10–6.
The mass fractions calculated without neutrino oscillations
are indicated by dotted lines.

Figure 2: Dependence of the 7Li/11B abundance ratio on sin2 2i13. The
dark- and medium-shaded regions indicate the ranges of the7
Li/11B in the normal and inverted mass hierarchies. The abundance ratio without oscillations is indicated by the light-shaded region. These regions are obtained including uncertainties
of neutrino temperatures (see [1] for details).

We study the supernova light-element nucleosynthesis
considering neutrino oscillations and investigate thedependence on neutrino oscillation parameters such as
mass hierarchies and a mixing angle i13 [1].
We adopt the supernova model of a 16.2 M9 star corresponding to SN 1987A, as the same in the previous study[2]. We use a Large Mixing Angle (LMA) solution for neutrino oscillation parameters. Since mass hierarchies havenot been clarified from neutrino experiments and only an
upper limit of the mixing angle i13 has been obtained, weparameterize these quantities.
The mass fraction distribution of 7Li is shown in Fig. 1.
Most of 7Li is produced as 7Li and its isobar 7Be in theouter He layer. Neutrino oscillations raise the mass fractions of 7Li and 7Be. Especially, the 7Be mass fraction
increases in the case of the normal mass hierarchy andsin2 2i13 = 1 # 10–2.
The main production process of 7Li and 7Be in the Helayer is 4He(o, o´p)3H(a, c)7Li and 4He(o,o´ n)3He(a,c)7Be. When neutrino oscillations are considered, the contribution from 4 He(o e , e – p) 3 He and 4 He( ō e , e + n) 3 H
becomes also important. As a result, 3He and 3H are produced more effectively, and therefore, the abundances of
7
Be and 7Li increase. The temperatures of oe and ōe aresmaller than those of oµ,x and ōµ,x just above the neutrino
sphere. Then, the temperatures of oe and ōe increase in the
O/C layer due to the transitions of oe )oµ,x and ōe ) ōµ,x.
The transition of oe and oµ,x becomes most effectively inthe normal mass hierarchy and large sin2 2i13 value.
We propose a possibility for constraining neutrino
oscillation parameters from the supernova light-element
synthesis. The dependence of the 7Li/11B abundance ratioon sin2 2i13 is shown in Fig. 2. Each shaded region is
obtained including the uncertainties in the supernova neutrino temperatures (see [1] for details). The 7Li/11B is about
0.6 without neutrino oscillations. On the other hand, it islarger than 0.83 in the case of the normal mass hierarchyand sin2 2i13 > 0.002. Future observations of 7Li/11B ratio
in stars having a trace of supernovae or supernova originating presolar grains combined with the evaluation of supernova nucleosynthesis models may constrain neutrino oscillation parameters.
New neutrino-nucleus reaction cross sections of 4He
and 12C have been calculated recently as a function of theneutrino energy [4]. The abundances of 7Li and 11B as wellas the dependence on oscillation parameters will be evaluated more precisely with the new cross sections.
References[1] Yoshida, T., et al.: 2006, ApJ, 649, 319.
[2] Yoshida, T., et al.: 2006, PRL, 96, 091101.
[3] Shigeyama, T., et al.: 1990, ApJ, 360, 242.
[4] Suzuki, T., et al.: 2006, PRC, 74, 034307.

25

00eng 08.2.28 6:41 PM ページ26

The Distance to the Galactic Center
NISHIYAMA, Shogo, TAMURA, Motohide

NAGATA, Tetsuya(Division of Optical and Infrared Astronomy, NAOJ)(Department of Astronomy, Kyoto University)

NAGAYAMA, Takahiro, KATO, Daisuke, SATO, Shuji

KUSAKABE, Nobuhiko(Department of Astrophysics, Nagoya University)(Graduate University for Advanced Studies/NAOJ)

MATSUNAGA, Noriyuki

NAOI, Takahiro(Institute of Astronomy, University of Tokyo)(Department of Infrared Astrophysics, JAXA)SUGITANI, Koji
(Graduate School of Natural Sciences, Nagoya City University)

KH - K / KS-

AKS# $^ H - K S h - ^ H - K S h0 .
E ^H - K Sh

where we use the reddening law AKS / E(H – KS) = 1.44 [2],and the intrinsic H – KS color of RC stars (H – KS)0 = 0.07.
KH–K is thus defined so that if AKS / E(H – KS) is independent of location, then KH–K is independent of extinction forany particular star. We then construct KS vs. H – KS CMD
and extract the stars in the region of the CMD dominatedby RC stars. The extracted stars are used in turn to make a
K H–K histogram (luminosity function, Fig. 1). The histogram has a clear peak and is fitted with the sum of exponential and Gaussian functions (thick curve in Fig. 1).
By fitting the luminosity function of the extracted stars
at | l |< 1º.0 and 0º.7 <| b |< 1º.0, we obtained the center of the
RC peak as KH–K = 12.855 ± 0.005. The distance modulus
to the Galactic center is given by (m – M)0 = KH–K –MKS +∆MK , where MKS is the absolute KS magnitude of local RC

26

25000

20000

Num. of Stars

We report the determination of the distance to the center of our Galaxy using the Bulge red clump giants [1].
Derived distance modulus is (m – M)0 = 14.38 ± 0.03 (stat)± 0.10 (sys), which corresponds to the distance
R0 = 7.52 ± 0.10 ± 0.35 (sys) kpc.
Red clump (RC) giants have been recently claimed to
be a very accurate distance indicator. They are the equivalent of horizontal-branch stars for a metal-rich population,and have narrow distributions in luminosity and color, andconsequently occupy a distinct region in the color magnitude diagram (CMD). The Hipparcos catalog allows us anexact calibration of RC absolute magnitudes, and therefore
RC stars can be used as a reliable standard candle.
About 100 # 3 (J, H, KS) images were obtained over| l |< 1º.0 and | b |< 1º.0 using the near-infrared camera SIRIUS on the IRSF telescope. The averages of the 10v limiting magnitudes were H = 16.6, and KS = 15.6.
To analyze the magnitude distribution of RC stars, wedefine the extinction-free magnitude

15000

10000

5000

10.5

11

11.5

12

12.5

13

13.5

14

K H-K [mag]Figure 1: Histogram of the dereddened KH–K magnitude for all the stars
in the RC dominated region at | l |< 1º.0 and 0º.7 <| b |< 1º.0.
Exponential and Gaussian functions are used to fit the histograms (thick curve).

stars, and ∆MK is population correction calculated fromtheoretical stellar evolution models. Here we adopt ∆MK =–0.07 and M K S = –1.59. Hence we obtain (m–M) 0 =14.38±0.03 (stat), which corresponds to R0 = 7.52±0.10(stat) kpc. Systematic errors are summarized in Table 1,
and estimated to be ±0.35 kpc.
Table 1: Systematic Error Budget

Error
fitting the RC peakextinction law
zero-point uncertainty
population correction
system transformation

Estimation (mag)
0.03
0.05
0.04
0.07
<0.01

Our result, R0 = 7.52±0.10 (stat) ±0.32 (sys) kpc, is inexcellent agreement with 7.62 ± 0.32 kpc [3] which is determined geometrically with the star S2 orbiting the super massive black hole in the Galactic center. When the population
effect of RC stars is taken into account, the distances obtainedin previous RC studies are consistent with this result.
References[1] Nishiyama, S., et al.: 2006, ApJ, 1093, 1098.
[2] Nishiyama, S., et al.: 2006, ApJ, 638, 839.
[3] Eisenhauer, F., et al.: 2005, ApJ, 628, 246.

00eng 08.2.28 6:41 PM ページ27

Search for Herbig Ae/Be Stars in the Magellanic Bridge
NISHIYAMA, Shogo, TAMURA, Motohide, NAKAJIMA, Yasushi(Division of Optical and Infrared Astronomy, NAOJ)

HABA, Yasuaki, KATO, Daisuke, BABA, Daisuke, SATO, Shuji(Department of Astrophysics, Nagoya University)

ISHIHARA, Akika

NAGATA, Tetsuya(Department of Earth and Planetary Science, University of Tokyo)(Department of Astronomy, Kyoto University)

SUGITANI, Koji

MATSUNAGA, Noriyuki, FUKUSHI, Hinako(Graduate School of Natural Sciences, Nagoya City University)(Institute of Astronomy, University of Tokyo)

KUSAKABE, Nobuhiko(Graduate University for Advanced Studies/NAOJ)(see [1] for more details), and the frequency is still controversial. Therefore a more precise determination of the CBefrequency or observations to differentiate between the
Herbig Ae/Be stars and CBe stars are required.
The luminosity of the candidates implies that the formation process of the Herbig Ae/Be stars in the MB is different from those in our Galaxy. Assuming that our candidates
are the group III Herbig Ae/Be stars defined by Hillenbrand
et al.[2], the J band magnitudes show that the candidates
have masses in the range of ~10 to more than 30 M9. Ifthey are members of the group I/II, the mass range is ~ 3 tomore than 20M9. Higher mass PMS stars are not expected
to be visible before they reach the zero-age main sequence
due to obscuration by circumstellar dust envelope/disk, but
the visibility may depend on the environmental condition
such as metallicity. Hence our result may suggest that theenvironmental effect of low metallicity can be seen for the
Herbig Ae/Be stars in the MB.
J-H

1.2
3

10

1.0

0.6

2

10

0.4

0.2
10

-2

0.8

stars [0.1mag]

We have found Herbig Ae/Be star candidates in thewestern region of the Magellanic Bridge [1].
A number of HI surveys have revealed a continuous
bridge of gas between the SMC and LMC, now known as the
Magellanic Bridge (MB). The MB is the closest bridge(~60kpc) among a number of known intergalactic bridges
situated in groups of galaxies, and the mechanism responsible for the formation of the MB is widely considered to be
gravitational influence of the LMC. The MB can thus provide us with insights into the role of external dynamicalinteractions in stimulating star formation. In addition, thevery low metallicity of the MB was found to be ~1.1 dex
lower than our Galaxy. Because of their metallicity andvicinity, the pre-main sequence (PMS) stars in the MB offera good opportunity to study in detail the formation and evolution of individual young stars in different environments.
We surveyed about 3º.0 # 1º.3 (24º < a < 36º, –75º.0 < d< –73º. 7) in the near-infrared J,H, and K S bands with
IRSF/SIRIUS, and have detected ~ 20,000 stars in the threebands with photometric errors of 0.1 mag. Herbig Ae/Bestars show strong excess radiation at infrared wavelengths,
and thus one can find them in a color-color diagram, suchas J – H versus H – K S diagram (Fig. 1). We selected
Herbig Ae/Be candidates with the following criteria: (1) J –H ≤ 0.2, (2) J ≥ 13.4, (3) more than 0.1 mag apart from the
OB locus, and (4) located under the line J – H = 4.2#
(H–K S ) –0.23 (see Fig. 1). As a result, we found 203
Herbig Ae/Be star candidates. A concentration of the candidates associated with a star cluster NGC796 is found, but
we cannot find any other concentrations.
There could be three populations in the region where
our Herbig Ae/Be candidates are distributed: Herbig Ae/Bestars, classical Be (CBe) stars, and dwarfs of O to F5 spectral type. To confirm whether Herbig Ae/Be stars exist in
the MB or not, the number of contamination by them wasestimated. The estimates suggest that about 60% of the 203
candidates could be contaminated by the dwarfs and CBestars. We therefore conclude that 81 of them are Herbig
Ae/Be stars after eliminating the possible contaminating
sources. However, the contamination of the CBe stars
depends on the frequency of the CBe stars among B-stars

0

-0.2
-0.2

0

0.2

0.4

0.6

0.8

1

1.2

1

H-Ks

Figure 1: J – H versus H – KS color-color diagram for the point sources
detected in all bands with photometric error less than 0.1 mag(grayscale). Crosses represent Herbig Ae/Be candidates. The thinand thick curves are the loci of dwarfs and giants, respectively.

References[1] Nishiyama, S., et al.: 2007, ApJ, 658, 358.
[2] Hillenbrand, L. A., et al.: 1992, ApJ, 397, 613.

27

00eng 08.2.28 6:41 PM ページ28

Distribution of dust clouds around the central engine of
NGC 1068
TOMONO, Daigo, TERADA, Hiroshi

KOBAYASHI, Naoto(Subaru Telescope, NAOJ)(Institute of Astronomy, University of Tokyo)

Figure 1: MIR image and grey body parameters in eq. 1. Locations of the 5
GHz sources [open circles][2] and the [O III] clouds [filled circles][3]are indicated. (a) 11.7 µm image. The straight lines show positions andwidths of the three L-band slits. (b) x9.7 map. Solid contours and darker grey scale show x9.7 > 0 (absorption) up to 1.5 while dashed contours and lighter grey scale shows negative x9.7. (c) Tcont(MIR)
between 160 K (dark) and 280 K (light). (d) fcont shown with ve contours in each dex between 10–1.4 (dark) and 10–3.8 (light). The fit forthe outer region is performed on images convolved with a Gaussian of
FWHM same as the original PSF (the circle in panel a).

We studied the distribution of dust clouds around thecentral engine of NGC 1068 based on shifted-and-added
8.8 – 12.3 µm (MIR) multi-filter images and 3.0 – 3.9 µm(L-band) spectra obtained with the Subaru Telescope [1].
From the MIR multi-filter images and the L-band spectra, we successfully constructed maps of color temperatures, emissivities, and optical depths of silicate and carbonaceous dust in absorption and emission in a region of
100 pc (1".4) around the central peak (Fig. 1). The MIR
parameters are derived with fitting the observed data to agrey body model:mF (m) = f cont e 10nomdifierent distances.
Second, the peak of the 9.7 µm silicate absorption feature is shifted to a longer wavelength at some locations.
Third, the ratio of the optical depths of the silicate
absorption feature and the absorption feature by carbonaceous dust is difierent from the Galactic values and showcomplicated spatial distribution.
Fourth, there is a pie-shaped warm dust cloud as anenhancement in the emissivity of the MIR continuum
extending about 50 pc to the north from the central engine(Fig. 1d). We speculate that material falls into the central
engine through this cloud.

- 1.6

B (Tcont , m) # e - x9.7 # k (m) ,（1）where k(m) is the optical depth of the silicate feature
obtained from the IR excess [4] and normalized at 9.7 µm.
The L-band parameters area derived with assuming straightcontinuum at each position. The reconstructed parameters
show the following characteristics.
First, color temperature of the MIR continuum scattersaround the thermal equilibrium temperature with the central
engine as the heat source while that of the L-band continuum is higher and independent upon distance from the central engine. Figure 2 shows the continuum temperatures at

28

Figure 2: Color temperatures of continua measured in MIR (filled circles) and in the L-band (empty circles). Horizontal axis shows
projected distance on the sky from the central engine. The solidline shows thermal equilibrium temperature of dust with emissivity proportional to m–1.6 and heated by a UV source of L = 2.2# 1011 L9 [5]. The spatial resolutions of the data and contamination of light from the peak limit the color temperatures to beaccurate only to the right of the vertical dotted lines.

References[1] Tomono, D., et al.: 2006, ApJ, 646, 774–782.
[2] Gallimore, J. F.: 1996, ApJ, 464, 198–211.
[3] Evans, I. N., et al.: 1991, ApJ, 369, L27–L30.
[4] Roche, P. F., Aitken, D. K.: 1984, MNAS, 208, 481–492.
[5] Telesco, C. M., Harper, D. A.: 1980, ApJ, 235, 392–404.

00eng 08.2.28 6:41 PM ページ29

Abundances of metal-poor star HD 122563
HONDA, Satoshi, AOKI, Wako
(NAOJ)ISHIMARU, Yuhri

WANAJO, Shinya

Sean G. Ryan

(Kogakuin University)(University of Tokyo)(University of Hertfordshire)

The chemical composition of metal-poor stars is expected to reflect the yields from a quite small number of nucleosynthesis events (or possibly a single event). Many observational studies for metal-poor stars have shed light on theunderstanding individual processes in the universe.
However, mechanism and astrophysical sites of the rprocess, which synthesizes elements heavier than the iron, is
still not well known. Previous observations have shown thatthe abundance patterns of the heavy neutron-capture elements (Z≥56) agree well with the solar-system r-process
pattern [1], but this is not the case for lighter ones; that is, alarge abundance scatter exists in such elements [2].
Our recent observations revealed that a correlation
exists in light neutron-capture element Sr (Z=38) and heavy
neutron-capture element Ba (Z=56) [3]: There is no Ba-richstar having very low Sr abundance, while a large scatter of
Sr abundances is only found in Ba deficient stars. This
result suggests the existence of a process mainly yielding
Sr (we here call this “weak-r process” [4]), which is separated from the “main r-process” that yields Sr and Ba insimilar proportions.
In order to clarify the weak r-process observationally,
we observed a star having high Sr/Ba ratio with the
Subaru/HDS, which presumably reflects the weak r-processstrongly, to investigate neutron-capture elements in detail[5]. We selected the bright metal-poor star HD 122563([Fe/H]=–2.8) to obtain the near-UV spectrum(3070–4780Å) where many lines of neutron-capture elements exist. Though observing this range with groundbased telescopes is difficult, the S/N ratios of our spectra
are 480 at 3500Å and 1300 at 4500Å with resolving powerof about 90,000.
We have determined abundances of 19 neutron-capture
elements, and upper limits for five other elements. Nb, Mo,
Ru, Pd, Ag, Pr, and Sm are detected for the first time forthis object by this observation. A comparison of the derived
abundance pattern with the r-process pattern of solar-system (Figure 1) reveals that the light neutron-capture elements (Sr- Zr) show very large excesses compared to heavy
ones like Ba, La, and Eu. The abundances of elements withintermediate mass (Z = 41 ~ 47), which are determined byour study for the first time, show a continuous decrease
with increasing atomic number. This trend is not expectedfrom usual r-process models in which a rapid drop of abundances from Zr to heavier elements reflecting the nature ofneutron magic number. Further theoretical work is required
to reproduce the observed abundance pattern.
Such a decreasing trend of the abundances with in-creasing atomic number is also seen in the heavier elements
than Ba. This differs from the abundance pattern found in rprocess rich metal-poor stars so far, possibly reflecting theprocess that produced light neutron-capture elements abundance in the early Galaxy.

Figure 1: Abundances of HD 122563 compared to the scaled solar system r-process pattern (normalized at Eu).

Figure 2: Logarithmic differences from the solar system r-process pattern. The open triangles mean the abundances of r-rich star CS
22892-052, while the open and filled circles mean those of HD
122563 and HD 88609, respectively. The difference of theabundance patterns of HD 122563 and HD 88609 from thesolar r-pattern become larger with increasing atomic number.

A similar abundance pattern is recently found in another metal-poor star [6], indicating that HD 122563 is not aunique object, and that the observed abundance patterns
give strong constraints on the future modeling.
References[1]Honda, S., et al.: 2004, ApJ, 607, 474.
[2]Sneden, C., et al.: 2000, ApJ, 533, L139.
[3]Aoki, W., et al.: 2005, ApJ, 632, 611.
[4]Wanajo, S., Ishimaru, Y.: 2006, Nucl. Phys. A, 777, 676.
[5]Honda, S., et al.: 2006, ApJ, 643, 1180.
[6]Honda, S., et al.: 2007, ApJ, 666, 1189.

29

00eng 08.2.28 6:41 PM ページ30

Project “Origin of Milkyway”
SAITOH, Takayuki, IDETA, Makoto, OKAMOTO, Takashi, KOKUBO, Eiichiro
WADA, Keiichi, TOMISAKA, Kohji, MAKINO, Junichiro(NAOJ)DAISAKA, Hiroshi

YOSHIDA, Naoki(Hitotsubashi University)(Nagoya University)

Figure 1: Photo of our clusters. Left side two 19-inch racks hold 16
nodes, where each node consists of an Opteron 250 CPU and a
GRAPE-7. The aluminum rack in the right side holds other 16
nodes, where each node consists of two Opteron 244 CPUs
without any GRAPEs. Gateway, file server, network switches
are installed between the two clusters.

The scientific goals of the project “Origin ofMilkyway” are to reveal (1)the formation processes of thestereostructure of Milkyway, (2)the origin of variety in themorphology of galaxies, and (3)the origin of the correlation
between super massive BHs and their host galaxies, using
ultra high resolution simulations of galaxy formation
including small scale physics. In order to archive the stateof-the-art simulations, we adopt special purpose computers,
namely GRAPEs, and we develop a special simulation
code which brings out the performance of GRAPEs. See[1] for more details.
In previous numerical simulations on galaxy formation,
special resolution is ~kpc and mass resolution is ~105–6M9. Number of mass elements in a galaxy is only ~104. As a result, it is difficult to reproduce exact massassembly histories with the bottom up nature in currently
favored cosmology and fine structures appeared in interstellar matter. The only way to reveal complex formation
processes on galaxy formation is to increase number ofmass elements in a galaxy.
Until now, we have developed two PC-clusters:
Amanogawa Zerogo-ki (Intel Xeon 3.6 GHz dual # 4) and30

Figure 2: Gas density map. Advanced numerical resolutions and more
realistic and acceptable star formation conditions allow us toobserve complex structures in our interstellar matter. Previous
simulations on galaxy formation can not resolve such a finestructures in their models.

Amanogawa Syogo-ki (AMD Opteron 250 single 2.4GHz#16 + Opteron 244 dual # 16 + GRAPE-7 # 24). We aredeveloping and testing our parallel simulation code onthese clusters.
We investigate a new set of star formation conditions
suitable for high-resolution simulations to resolve molecular clouds. The results of simulations are summarized asfollows:
1. A thin gas disk with inhomogeneous, multiphasestructures is successfully formed.
2. Our models reproduce observational relation, that is
Kennicutt-Schmidt relation. The choice of the starformation efficiency has a minor effect on the starformation in our models.
3. The time scale of the mean mass transfer from diffuse region to dense region is very slow, and it determines global star formation rate.
We are now preparing new simulations of galaxy formation with our new star formation recipe.
References[1] Wada, K., et al.: 2004, IPSJ Magazine, 45, 12.

00eng 08.2.28 6:41 PM ページ31

Periodic Vortex Shedding from a 12-m Antenna
UKITA, Nobuharu, SAITO, Masao, IKENOUE, Bungo(NAOJ)

Jeffrey G. MANGUM, Nicholas J. EMERSONAngel C. OTAROLA(NRAO)(NRAO/ESO)

Figure 1: Three ALMA prototype 12-m antennas (front) at the NRAO VLA
site. The NAOJ antenna (left) was used for the measurements. Two
25-m antennas (back) are element antennas of the VLA.

Figure 2: (a) A time history of yaw motion of the elevation axis for two
minutes in the wind of 9 m s –1. (b) A mean PSD of yaw
motion of the elevation axis for three hours shows anenhanced component near 0.15 Hz.

The von Karman vortex sheet is a famous flow patternwhich forms in the wake of a rough body for a given range
of Reynolds numbers. In nature, this pattern shows up wonderfully on oceanic stratocumulus cloud decks in the wakeof an isolated island as shown in pictures taken from satellites. A similar turbulent flow has been found to take placearound the NAOJ 12-m parabola antenna for the ALMA
project during performance tests carried out at the NRAO
VLA site (Fig. 1).
Figure 2a shows a time history of yaw motion of theelevation axis derived from the displacement of the bearing
housings measured with linear gauges mounted on a reference frame structure built in each side of the yoke. The
measurements were made in the wind of 9 m s–1, and the
Reynolds number was 6 # 106. Figure 2b displays a power
density spectrum (PSD) of the yaw motion in which anenhanced component is discernible at 0.15 Hz. The same
periodicities have also been observed in both the winddirection and wind velocity measured with a 3D ultrasonicanemometer in the wake downstream of the antenna (Fig.
3). Such periodicities have been seen in neither rotation of
the elevation axis nor vertical wind velocity. These obser-

vations suggest that there is a large scale, periodic flow pattern in the wake, possibly a large eddy, and that the oscillatory lateral force by shedding vortices exerts on the antenna
to make the yaw motion.
Our field measurements have determined some basic
wind engineering parameters for a parabola antenna. Frommeasured periodicity, the Strouhal number has been determined to be 0.19, which is comparable to those of cylinder,
inverse triangle, and other similar geometric shapes. Froman observed amplitude of yaw motion and torsional rigidityof the yoke structure, an amplitude of torque variation has
been estimated to be 2,100 Nm. We have found that oscillatory lateral force per unit area on the antenna is equal to
the stagnation pressure of the upstream wind, namely theshape coefficient, Ck , is 1. It is interesting to note that the
Ck for a cylinder is also 1 for a wide range of the Raynolds
number, 102 – 10–7.

Figure 3: Wind velocity vector distributions, mean PSDs of wind speed,
and wind direction in the wake downstream of the antenna (a),(c), (e), and in the undisturbed wind, (b), (d), and (f). Star
marks (*) indicate mean wind velocities, broken lines the winddirections, thin lines the directions of the antenna from theanemometer. Solid lines in (c) and (d) indicate a PSD of Simiu
wind model of 9 m s–1 for an open terrain, dashed line for
3*Simiu, and broken lines for 10*Simiu.

References[1] Ukita, N., et al.: 2006a, Proc. of SPIE, 6267, 122.
[2] Ukita, N., et al.: 2006b, Proc. of National Symposium on Wind
Engineering, 19, 389.

3100eng 08.2.28 6:41 PM ページ32

Discovery of Ha Absorption in the Broad Absoprtion Line
Quasar SDSS J0839+3805
AOKI, Kentaro, AKIYAMA, Masayuki, TAMURA, Naoyuki(Subaru Telescope, NAOJ)

IWATA, Ikuru

OHTA, Kouji, ANDO, Masataka(Okayama Astrophysical Observatory, NAOJ)(Department of Astronomy, Kyoto University)

During our search for low ionization broad absorption
line quasars and iron low ionization broad absorption line
quasars by visual inspection of ~ 4800 spectra between redshifts of 2.1 and 2.8 in the Sloan Degital Sky Survey(SDSS), we found an unusual BAL quasar, SDSS
J0839+3805. Figure 1 shows its rest UV spectrum fromSDSS data. It shows many absorption lines from Fe II, Zn
II, Cr II, and Si II. Since the Lya emission line is narrow
and there are no broad emission lines in the rest UV spectrum of SDSS J0839+3805, we carried out nearinfrared
spectroscopy in order to examine properties of the Hb andHa emission lines.
We discovered Ha absorption in the broad Ha emission line (Fig. 2) through near-infrared spectroscopy with
the Cooled Infrared Spectrograph and Camera for OHS(CISCO) on the Subaru telescope [1]. The presence of nonstellar Ha absorption is known only in the Seyfert galaxy
NGC 4151 at that time [2]; thus, our discovery is the firstcase for quasars. The Ha absorption line is blueshifted by
520 km s–1 relative to the Ha emission line, and its redshift
almost coincides with those of UV low-ionization metal
absorption lines. The width of the Ha absorption (~ 340
km s–1) is similar to those of the UV low-ionization absorption lines. These facts suggest that the Ha and low-ionization metal absorption lines are produced by the same lowionization gas, which has a substantial amount of neutral
gas. The column density of the neutral hydrogen is estimated to be ~ 1018 cm–2 by assuming a gas temperature of
10,000 K from the analysis of the curve of growth.
Furthermore, the UV spectrum of SDSS J0839+3805
shows a remarkable similarity to that of NGC 4151 in its
low state, suggesting that the physical condition of theabsorber in SDSS J0839+3805 is similar to that of NGC
4151 in the low state. As proposed for NGC 4151, SDSS
J0839+3805 may also be seen through the edge of the
obscuring torus.
References[1] Aoki, W., et al.: 2006, ApJ, 651, 84.
[2] Hutchings, J. B., et al.: 2002, AJ, 124, 2543.

32

Figure 1: Observed spectrum of SDSS J0839+3805 in the SDSS.
Ordinate is a flux density, and abscissa is the observed wavelength. The rest wavelength is given along the top axis. Dottedlines show the wavelengths of the absorption lines.

Figure 2: Top: K-band spectrum of SDSS J0839+3805. Ordinate is arelative flux density, and abscissa is the observed wavelength.
The rest wavelength is given along the top axis. The Ha emission is fitted with three Gaussians. The best fit is shown as a
red solid line. Bottom: The sky emission spectrum (solid line)
and the atmospheric transmission curve (dotted line).

00eng 08.2.28 6:41 PM ページ33

Polarization Differential Objective Spectroscopy with a
Nulling Coronagraph
MURAKAMI, Naoshi

BABA, Naoshi, TATE, Yoko, SATO, Yoichiro(NAOJ)(Hokkaido University)

TAMURA, Motohide(NAOJ)
mainly caused by the slight displacement of the image(estimated to be about 0.01 m/D) when modulating thepolarized light using the LCVR.
The obtained differential spectrum ideally corresponds
to the Stokes Q(m) parameter. We expect that observationsof accurate Q(m) [and U(m)] parameters of exoplanets will
enable us to obtain a clearer knowledge of planetary atmospheres.

Figure 1: Optical setup for polarization differential spectroscopy with
FQPoM coronagraph.
10000

(a)
(a)

(b)

(b)

inte nsity [a rb. unit]

Direct detection of exoplanets is very challenging inthat it simultaneously requires extremely high dynamic
range, high spatial resolution, and high sensitivity. For
high-contrast imaging, the light from a parent star must be
suppressed so that a planetary signal can be distinguishedfrom the undesirable stellar noise. A nulling stellar coronagraph with a four-quadrant phase mask (FQPM) is one of
the most promising concepts [1]. To achieve achromatic
deep nulling, we proposed a polarization interferometricstellar coronagraph using a four-quadrant polarization mask
(FQPoM), and have successfully demonstrated over abroad wavelength range [2]. In principle, the FQPoM coronagraph has the ability to realize perfect elimination of thestellar light. However, various factors (manufacturing
errors in the FQPoM, finite angular size of a star, surface
roughness of optical elements etc.) generate residual stellar
noise. For further suppressing the residual noise, we also
proposed a polarization differential imaging (PDI), which
extracts a partially polarized planetary signal from unpolarized residual stellar noise [3].
We report the laboratory demonstrations of spectroscopic observations using the FQPoM coronagraph and the
PDI testbed. Figure 1 shows an optical setup. The lightfrom a halogen lamp (planet model) is made to produce anartificial absorption line by using the reflection from aninterference filter. Three tilted glass plates are used to simulate a partially polarized planetary signal. The light beamsof the stellar and planetary models are led to the polarization modulator (liquid-crystal variable retarder, LCVR) for
the PDI, FQPoM coronagraph, and objective spectrometer.
Figure 2 shows the experimental results. The planet/starintensity ratio is 8 # 10–5, and their angular separation is
3.2 m/D. A degree of polarization of the planet model isabout 50%. The images on the left are the FQPoM coronagraphic images (a,b) before and (c) after the differentiation.
The graph on the right shows their objective spectra recorded at the position of the planet model. In this graph, the dip
caused by the artificial absorption can be seen aroundm = 630 nm. Plot (d) is the differential spectrum created byusing only the planet model (ideal differential spectrum of
the planet model). The deviation from the ideal spectrum
can be observed in particular in the short-wavelength(m < 560 nm) and long-wavelength (m > 650 nm) regions.
This is because the residual stellar noise contaminates these
spectral regions. We suppose that the residual noise is

1000

(c)

100

(c)

(d)
10
520

540

560

580

600

620

640

660

680

wavelength [nm]Figure 2: (Left) Acquired coronagraphic images (a,b) before and (c)after differentiation. (Right) Objective spectra of these coronagraphic images at the position of the planet model.
References[1] Rouan, D., et al.: 2000, PASP, 112, 1479.
[2] Baba, N., et al.: 2002, Optics Letters, 27, 1373.
[3] Baba, N., Murakami, N.: 2003, PASP, 115, 1363.

33

00eng 08.2.28 6:41 PM ページ34

High-Resolution Studies of the Dense Molecular Cores
toward Massive Star-Forming Regions
SAITO, Hiro, SAITO, Masao

MORIGUCHI, Yoshiaki, FUKUI, Yasuo(NAOJ)(University of Nagoya)

Figure 1: Color images of the 110 GHz continuum emission overlaid
with contours of C18O (J=1–0) emission. Contour levels arefrom 3 v in steps of 2 v. 1 v noise levels are 13 mJy. Threedashed squares denote the area of five right panels. Five rightpanels: (1, 3, 4, 5) 1 v = 30 mJy, (2) 1 v = 20 mJy). The integrated velocity ranges are (1,3) 3.0–4.0 km s–1, (2) 4.0–5.5 km
s–1, and (4) 1.6–2.6 km s–1.

We report the results of an imaging of dense molecularcores in three cluster-forming regions, IRAS 02461+6147,
IRAS 03035+5819, and IRAS 06058+2138, by the
Nobeyama Millimeter Array.
In these cluster-forming regions, there are massive(proto)stars with the high luminosity of 1–5 # 104L9 andthe massive dense clumps, which have a mass of ~ 500M9,
a radius of ~ 0.3 pc, and a line width of ~ 2.5 km s–3, areidentified by [1]. The goal of the present observation is toreveal the inner structure of the dense gas in the clumps
with the cluster formation including massive (proto)stars.
Most of the recent observations toward the massive
star-forming regions have focused on the identification of
hot cores, which have a luminosity larger than 104L9 andtemperatures of 100 K or higher [2]. Due to these characteristics, it has been suggested that hot cores contain massive (proto)stars. However, hot cores are unlikely to keep aphysical feature of the earlier stage of evolution, just before
the formation of massive (proto)stars, i.e., a cold core. It istherefore important to identify and study cold cores inappropriate molecular lines.
We have observed toward three cluster-forming regions
using the C18O molecular line, which can detect the coldcores, and we have identified 28 dense cores and four thermal dust millimeter continuum sources (MCSs) (Fig. 1).
The mass, effective radius, and line-width of these cores
range from 2.1 to 29M9, from 0.013 to 0.108 pc, and from

34

Figure 2: The correlation between the radius and the line width of thecores. The circles and squares are the cores and the clumps
identified by [1], respectively. The black and grey filled marks
are the objects with massive star formations and NIR sources,
respectively. The solid lines are the maximum and minimum
index of the line width-radius relation, respectively.

0.7 to 2.7 km s–1, respectively.
Sevral cores with various line widths exist in one
clump, and we found that the index of the radius–line width
relation is difference form cores to cores in one clump (Fig.
2). In addition, we divide the C18O cores into two types, aturbulent core and a non-turbulent core. The non-turbulent
cores are similar to the typical cores in the low-mass starforming regions. On the other hand, the turbulent cores
have a higher average H2 density than those of the non-turbulent cores and the external pressure of these cores is 100– 1000 times higher than that of low-mass star-forming
regions. In particular, three of the turbulent cores are associated with massive protostar candidates and the intensity
peak of MCS. From these results, we suggest that massive
stars are formed from the turbulent cores which are gravitationally bound. This suggestion is consistent with the theorretical suggestion by [3]. In addition, in order to form sucha turbulent core in a molecular cloud, the molecular musthas a large kinetic motion and a large mass.
The observation of the cores in the clump with the cluster
formation is in progress by the Nobeyama Millimeter Array.
References[1] Saito, H., et al.: 2007, ApJ, 659, 459.
[2] Churchwell, E., et al.: 1992, A&A, 253, 541.
[3] McKee, C. F., Tan, J. C.: 2003, ApJ, 585, 850.

00eng 08.2.28 6:41 PM ページ35

Improvement of Gravitational Wave Detector TAMA300
by the Seismic Attenuation System (SAS)
FUJIMOTO, Masa-Katsu, TAKAHASHI, Ryutaro, ARAI, Koji, TATSUMI, Daisuke
YAMAZAKI, Toshitaka, FUKUSHIMA, Mitsuhiro, ASO, Yoichi, NAKAGAWA, Yasunori
AGATSUMA, Kazuhiro, ARASE, Yuta, and the TAMA Collaboration(TAMA project office, NAOJ)
We started installation of the Seismic Attenuation
System (SAS) in 2005 in order to improve the vibration
isolation system in the interferometer gravitational wave
detector TAMA300. The second SAS, which was installedat the east-west front (NM1) in June, 2006, formed a 300-m
cavity with the SAS at the west end (EM1) installed in
2005. Length fluctuation of the cavity measured by feedback signals to lock the cavity showed the improvement of–24dB at 2 Hz as compared with old suspensions (Fig. 1a).
We confirmed the improvement of –25dB at 3 Hz on angular fluctuations too (Fig. 1b). As a result, we expect the
bandwidth of the alignment control feedback is set to belower than 5 Hz. This will result reduction of the noise dueto the alignment control system which limited the former
sensitivity of TAMA300. Then followed the installation of
two SASs to the north-south arm in October andNovember. We could lock the interferometer with fourSASs in March, 2007 successfully. There the east-west arm
cavity was locked by actuating the laser frequency for stabilization of the light source, while the north-south arm
cavity was locked to this stabilized light by actuating themirror of the north-south front (NM2). The basic behaviorof the interferometer with SASs was confirmed.
The natural frequencies of the inverted pendulum (IP),which characterize quality of each SAS, are shown as follows. Most of the horizontal modes (X and Y) were tuned to
be lower than 100mHz except for EM1 in which asymmetry of elastic spring components of the IP caused the large
splitting of the modes. Frequencies of rotational mode(i) are about 0.5 Hz.
X [mHz]Y [mHz]

i[Hz]

NM1

50

60

0.50

EM1

150

50

0.54

NM2

30

60

0.52

EM2

50

70

0.50

There are two kinds of control system for the SAS.
Each system is handled by a digital instrument using an all-purpose CPU (Pentium) + RTOS. One is the IP control system which feeds back signals of acceleration sensors and
LVDTs (position sensors) on the top of SAS to actuators
for the IP. Scince the lower stage is suspended by a single
wire from the IP, it has a torsion mode at ~ 50 mHz. The
system also damp this torsion mode using a differential
photo sensors and the actuators for the IP. The other is the
PF-TM control system which feeds back signals of mirror
rotation (Pitch and Yaw) detected by local optical levers toactuators for the mirror. After the 300-m cavity is locked,
the sensing signals are changed to global signals acquiredby the Wave Front Sensing (WFS) method from the interferometer.

Figure 1: Improvement of the vibration isolation system. Old suspension and New SAS are shown.
References[1] Kuroda, K., et al.: 2006, Progress of Theoretical Physics Supplement,
163, 54.
[2] Tatsumi, D., et al.: 2007, Classical and Quantum Gravity, 24, S399.

35

00eng 08.2.28 6:41 PM ページ36

Giant Molecular Association in Spiral Arms of M 31:
Evidence for Dense Gas Formation via Spiral Shock
Associated with Density Wave ?
TOSAKI, Tomoka, KUNO, Nario, NAKANISHI, Kouichiro(Nobeyama Radio Observatory, NAOJ)

SHIOYA, Yasuhiro

HASEGAWA, Takashi(Ehime University)(Gunma Astronomical Observatory)

MATSUSHITA, Satoki

KOHNO, Kotaro(Institute of Astronomy and Astrophysics, Academia Sinica)(Institute of Astronomy, University of Tokyo)

We present the observations of 12CO(J = 1 – 0), 13CO(J= 1 – 0) and 12CO(J = 3 – 2) emissions toward a GMA in
the southern spiral arm of M 31 using Nobeyama 45-m and
ASTE 10-m telescopes [1].
Spiral arms are the most striking structures in disk galaxies and a major site of massive star formation. Spiral arm,i.e., density waves, seem to enhance the star and dense gas
formation due to the accumulation and/or compression ofgases. On the other hand, it is well established that moleculargases in spiral arms show very large structures, which areoften referred to as Giant Molecular Associations (GMAs).
Observational studies of GMAs in galaxies provide us withinvaluable clues on the physics that governs the large scalestar formation in the disk regions of galaxies.
It is difficult to achieve this by observations of rather“distant” galaxies using current mm-wave facilities due totheir limitation on the angular resolutions and sensitivities.
The best method of overcoming this limitation is makevery wide-area observations of molecular lines in very
nearby galaxies; M 31, the nearest massive spiral galaxy at
a distance of 0.69 Mpc, is a suitable target for this purpose.
The observed region is 3' # 4' (0.6 kpc # 0.8 kpc) withresolutions of 16" – 17" for 12CO(J = 1 – 0) and 13CO(J =1 – 0). We obtained a 1.' 2 # 1.' 4 wide 12CO(J = 3 – 2) map
with a resolution of 23". The GMA has a size and mass of afew 100 pc and 5.6#106M9, respectively. The 12CO(J = 1 –0) to 13CO(J = 1 – 0) integrated intensity ratio (R12/13) andthe 12CO(J = 3 – 2) to 12CO(J = 1 – 0) integrated intensity
ratio (R3–2/1–0) averaged over the entire region of the GMA
are ~ 10 and 0.3, respectively. These line ratios suggest gas
densities of (3 – 6) # 102cm–3 at a temperature of 15 – 25
K, which are similar to or slightly larger than those of
GMCs in Galactic disk. We found a radial gradient of R12/13
within the GMA, over a range from 6 at the center of the
GMA to 14 at the edges of the GMA. The distribution of
R12/13 shows a smooth structure with an overall density gradient.
The GMA consists of two velocity components, blue(~ –505 km s –1) and red (≥ –490 km s –1). In Both the
12
CO(J = 1 – 0) and 13CO(J = 1 – 0) profiles, the blue component shows a strong peak intensity and narrow velocity
width, while the red component is weaker and wider. R12/13of the red components is 5, which is smaller than that of theblue one (16), indicating the red component has a higher
gas density. By considering the direction of galactic rotation in this region, we suggest that the red component is the“post-shock” dense gas decelerated by shock due to thedensity wave.
References[1] Tosaki, T., et al.: 2007, PASJ, 59, 33.

Figure 1: Integrated intensity maps of 12CO(J =1–0) (left) and 13CO(J =1–0) (middle) by NRO 45-m telescope, and 12CO(J =3–2) (right) by ASTE.

36

00eng 08.2.28 6:41 PM ページ37

MOIRCS Deep Survey : DRG Number Counts
KAJISAWA, Masaru

MOIRCS GTO team(Division of Optical and Infrared Astronomy, NAOJ)
MOIRCS GTO team is carrying out a deep imaging
survey with Subaru/MOIRCS in the GOODS-North region.
Our main objectives are 1) to search LBGs and Lya emitters at z > 7 and 2) to investigate the histories of star formation and mass assembly of galaxies at 1 < z < 4. Here
we present the result of the study of the number counts ofDistant Red Galaxies (DRGs) with J – K(Vega)> 2.3 down
to K = 23 [1].
We observed one field of view of MOIRCS (4 # 7
arcmin2) in the GOODS-North region. Our data reachedJ =24.6, H = 22.8 and K =23.2 (5σ limit, Vega system)with the FWHM of 0.42 arcsec for the point source. We
used the deep J and K-bands images to investigate the number counts of DRGs. About 90 DRGs were detected in ourfield of ~24.3 arcmin2.
Figure 1 shows the number counts of DRGs in ourfield. The number counts of DRGs turn over at K ~ 22,
while the number counts of all K-selected objects continue
to increase to at least K ~ 23. The number counts of DRGs
in our field agree well with those in other general fields at
K < 22 (the bottom panel). The dashed line in the figure
shows the result of the linear fit for the counts of DRGs at
K < 22 in our and other general fields. When we extrapolated this linear line to K ~ 23, the surface density of the faint
DRGs with K > 22 in our field was clearly deficient. The
density in the 22.5 < K < 23 bin is about a factor of three
lower than that expected from the number counts at abrighter magnitude.
At K > 22, only HDF-South data [2] have a sufficientdepth and can be used for a comparison with our data. The
number counts in HDF-South do not show a decrease at
K > 22, but are still consistent with our results within theuncertainty. Since DRGs show a strong angular clustering(Fig. 2), however, the small survey areas of the HDFs
could introduce large uncertainty and a wide area survey isessential for these galaxies.
While the number density of DRGs at 2 < z < 4decrease at K > 22, bluer galaxies with J – K < 2.3 at thesame redshift range do not show a similar decrease but continue to increase to K ~ 23 [1]. These results suggest thatthe mass-dependent color distribution, where most of thelow-mass galaxies are blue, while more massive galaxies
tend to have redder colors, had already been established atthat epoch.

Figure 1: Number counts of DRGs in MOIRCS Deep Survey field.
Top: the number counts of all K-selected objects (green
squares) and DRGs with J – K > 2.3 (red circles). Bottom:
comparison of DRG number counts with other general fields.
Dashed line shows a linear fit for the data points at K < 22.

Figure 2: Spatial distribution of DRGs in MOIRCS Deep Survey field.
The size of symbols is scaled according to apparent K-band
magnitude. The dashed line show the region of the original
HDF-North.
Reference[1] Kajisawa, M., et al.: 2006, PASJ, 58, 951.
[2] Labbe, I., et al.: 2003, AJ, 125, 1107.

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00eng 08.2.28 6:41 PM ページ38

Protocluster Search around Radio Galaxies at z ~ 2.5 with
Subaru/CISCO
KAJISAWA, Masaru, KODAMA, Tadayuki TANAKA, Ichi, YAMADA, Toru
(Division of Optical and Infrared Astronomy, NAOJ)
We report the discovery of protocluster candidates
aroundhigh-redshift radio galaxies at z ~ 2.5 on the basis ofclear statistical excess of color-selected galaxies aroundthem seen in the deep near-infrared imaging data obtainedwith Subaru/CISCO [1].
From many previous studies, it appears that major starformation in bright cluster galaxies was virtually completed
by z ~ 2. Therefore it is important to search protoclusters
up to z > 2 in order to directly see the forming phase of
these galaxies. It is not an easy task, however, since it
requires a large volume to survey in order to find such rare
objects.
We performed the JHK-bands imaging observations of
the fields of the six radio galaxies at z~2.5 with
Subaru/CISCO. High-z radio galaxies are expected to point
us towards protoclusters, since they are among the most
massive galaxies at any redshift, and in fact powerful radiogalaxies at intermediate redshift tend to inhabit rich environment. We make use of our NIR multicolor photometricdata in order to effectively pick up plausible protocluster
members at z ~ 2.5 associated with the central radio galaxies. In addition to J – K >2.3 (DRG selection), we apply a
new color cut of J – K>2.5 # (H – K) + 0.5 & J – K >1.5,
using JHK-bands data (Fig. 1). This two-color-based selection has several advantages over DRG selection: (1)younger or star-forming galaxies with relatively bluer
J – K color at z ~ 2.5 can also be sampled, (2) this selection
isrobust against dust extinction, (3) most of cool M, L andT dwarfstars can be excluded.
Over the range of 19<K(Vega)<21.5, we see a significant excess of these color-selected galaxies by a factor of
about 2 (for DRGs) or 3 (for JHK selection) around theradio galaxies fields compared to those found in the generalfield of GOODS-South (Fig. 2). In particular, two radiogalaxies (4C –00.62 & 4C +23.56) fields show very strong
density excess (factor of 5 excess of JHK-selected galaxies,
see right panel of Figure 2), and these are likely to be protoclusters associated with the radio galaxies.
Figure 3 shows J – K versus K CM diagrams of the 4C– 00.62 field. The JHK-selected galaxies in this field tend
to be relatively bluer than the expected CM relation (redline in the figure) calculated from the passive evolution(0.1 Gyr single burst) model with zform=5. These galaxies
might have been shifting from the actively star-forming
phase to passively evolving phase at the observed epoch.
Using such a useful NIR color-selection technique, we
expect to be able to understand how the CM relation ofgalaxies formed in protoclusters in the early universe.

38(Subaru Telescope, NAOJ)

BOWER, R.
(University of Durham)

Figure 1: Combined J–K vs H–K color-color diagram of all the six radiogalaxies fields. The thick line and horizontal thin line shows theboundaries of our two-color selection with JHK-bands and DRG
selection, respectively. Different symbols correspond to our different color selections (Circles show JHK-selected galaxies, andtheir red and blue colors represent their J–K colors).

Figure 2: Combined cumulative number counts of JHK-selected galaxies in the radio galaxies fields (red) and those in a controlled
field GOODS-South (blue). Solid symbols show red JHKselected galaxies with J–K>2.3. (left): for all the six radiogalaxies fields. (right): for only the two most plausible protoclusters of 4C – 00.62 & 4C +23.56.

Figure 3: J–K vs K CM diagram of 4C –00.62 field. Different types ofsymbols differentiate the adopted color selections as indicatedin Figure 1. The red line shows the expected CM relation atz~2.5 calculated from the 0.1 Gyr single burst model zform=5.
Reference[1] Kajisawa, M., et al.: 2006, MNRAS, 371, 577.

00eng 08.2.28 6:41 PM ページ39

12

CO(J =3–2) Line Observation of Elliptical Galaxies
NAKANISHI, Hiroyuki, TOSAKI, Tomoka, KUNO, Nario(NAOJ)

KOHNO, Kotaro, SOFUE, Yoshiaki(University of Tokyo)
We report 12CO(J =3–2) observations of 15 nearby
elliptical galaxies carried out with the ASTE telescope[1].
Cold interstellar medium (ISM) is a minor componentof elliptical galaxies. ISM present in ellipticals is thought toresult from stellar mass loss or accretion from outside. It isdifficult to study such mechanisms from ISM observations
for spiral galaxies because they contain much ISM fromearly stages of galaxy formation. Cold ISM observation for
elliptical galaxies is crucial for such a study.
Several surveys have been made using the CO(1–0) andCO(2–1) lines (e.g., [2]). However, all of these studies haveconcentrated on ellipticals which are detected at 100
microns by IRAS, and are therefore biased. This study
examines whether there is a difference in results, selecting
objects without regard to the presence of other tracers ofcold interstellar matter.
The observed galaxies were 13 elliptical galaxies lying
in the right ascension range 22h – 7h and between declinations of –30 degrees - +20 degrees, and having recession
velocities less than 5000 km s–1. No other criterion wasused for thirteen of the galaxies, so they are unbiased. In
addition, NGC 855 and NGC 2328 were observed to compare with CO(1–0) and CO(2–1) data. Fifteen ellipticals
were observed.
We carry out observations with the ASTE, 10m antenna
located in the Atacama Desert in Chile on August 21–24
2006. Observed line was 12CO(J =3–2) (345GHz). The
spectra were smoothed by 46 channels to a velocity resolution of 19.8 km s–1. The typical rms noise levels, ∆TMB, forthe smoothed spectra were 8 mK.
The spectra for fifteen observed galaxies are shown infigure 1. We detected CO(3–2) emission from three galaxies, all for the first time. Two of them are undetected by
IRAS at 100 microns.
Comparisons with CO(2–1) and CO(1–0) data give line
ratios of CO(3–2)/(1–0)=0.5 and CO(2–1)/(1–0)=0.8. We
calculated line ratios using the Large Velocity Gradient(LVG) model, and found that H2 density was 3 # 102 – 1 #10 3 cm –3 in the temperature range of 15 – 100 K. The
molecular gas masses were estimated to be 2.2 # 106 – 4.3#010 8 M 9 . These values are consistent with former

researches (e.g., [2])Figure 1: CO Spectra of the observed elliptical galaxies.

Figure 2: Relationship among density, temperature and line ratios
derived by LVG calculations. The solid and dotted lines
denote R31 and R21, respectively. The thick lines denote values
for NGC855.
References[1] Nakanishi, H., et al.: 2007, PASJ, 59, 61.
[2] Wiklind, T., Combes, F., Henkel, C.: 1995, A&A, 297, 643.

39

00eng 08.2.28 6:41 PM ページ40

Torsionally Excited Methyl Formate in Orion KL
KOBAYASHI, Kaori, OGATA, Kazumi, TSUNEKAWA, Shozo(University of Toyama)

TAKANO, Shuro(Nobeyama Radio Observatory, NAOJ / the Graduate University for Advanced Studies (Sokendai))
Methyl formate (HCOOCH3) is one of the moleculeswith dense rotational spectral lines, and more than 500
lines in the ground state have been detected in space [1]. It
has an internal rotation of the methyl group (-CH 3) asshown in Figure 1.
Large saturated organic molecules like methyl formate
are often found in hot cores in massive star-forming
regions. In such hot regions, it is probable that torsionalmotion of the methyl group is excited, because the energyof the tortional motion is generally not large. Rotationaltransitions in the torsionally excited state have already been
detected for methanol (e.g., [2]).
There are many radio signals whose origin is unknown
and efforts to identify these signals are under progress.
Recently researchers in the University of Toyama succeeded to assign laboratory spectra of methyl formate in thefirst torsionally excited state [3,4]. This success made it
possible to compare with the data observed with radio telescopes.
This time we report a successful assignment of unidentified lines in Orion KL to the first torsionally excited
methyl formate [5]. We have assigned 7 unidentified lines
from previous line surveys around 97 GHz with Nobeyama
45 m radio telescope [6] to this excited state. In addition, atleast 13 lines from other line surveys were also identified.
The temperature and the column density in the first torsionally excited state of this molecule were calculated to be
44±10 K and (8.6±3.2) #1014 cm–2, respectively, using arotation diagram method. The temperature obtained is similar to those of the ground state, but our column density israther high, considering that methyl formate is in the first
torsionally excited state. The diagram is shown in Figure 2.
It is quite likely that many remaining unidentified lines
can be explained by this kind of organic molecules in thetorsionally excited states.

40

Figure 1: Molecular structure of methyl formate is schematicallyshown. The internal rotation of the methyl group (-CH3) isindicated with a red arrow.

Figure 2: Rotational diagram for methyl formate in its first torsionallyexcited state. The data used are obtained with Nobeyama 45 mradio telescope [6]. The upper-state energy Eu/k was set to relative value to the lowest rotational state of methyl formate inthis excited state.
References[1] Lovas, F. J.: 2004, NIST Recommended Rest Frequencies for
Observed Interstellar Molecular Microwave Transitions(Gaithersberg:NIST), http://physics.nist.gov/PhysRefData/Micro/
Html/contents.html[2] Lovas, F. J., et al.: 1982, ApJ, 253, 149.
[3] Odashima, H., et al.: 2003, Molecules, 8, 139.
[4] Ogata, K., et al.: 2004, J.Mol.Spectrosc., 225, 14.
[5] Kobayashi, K., et al.: 2007, ApJ, 657, L17.
[6] Ohishi, M., et al.: 1988, ApJ, 329, 511.

00eng 08.2.28 6:41 PM ページ41

Universality of the c-process in core-collapse supernovae
HAYAKAWA, Takehito

IWAMOTO, Nobuyuki(JAEA/NAOJ)(JAEA)

KAJINO, Toshitaka

SHIZUMA, Toshiyuki(NAOJ / University of Tokyo)(JAEA)

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

Figure 1: Calculated ratios of an s-nucleus to a p-nucleus, N(s)/N(p). The
s-nucleus is two neutrons heavier than the p-nucleus with thesame atomic number. The filled circles are the calculated ratios
in the model with M = 40 M9 , Z = Z9 and E = 1051 erg. The triangles are those in the model with M = 25 M9 , Z = Z9 and E =20 # 1051 erg. The square are those in the model with M = 25
M9 , Z = 0.05 Z9 and E = 1051 erg. The dashed line is N(s)/N(p)= 3. The dot-dashed lines are 1 and 9. The dot lines show theatomic number corresponding to the neutron magic numbers of
N=50 and 82. All the calculated ratios in the region of N > 50
are almost centered around a specific number of 3.

The origin of the p-nuclei has been studied by theoretical and experimental methods over the last 50 years [2-7].
The p-nuclei are on the neutron-deficient side of the b-stability line and their isotopic fractions are small (typically
0.1 ~ 1 %). In our previous paper [4], we reported the scaling in the solar system abundances, which are the evidence
that the most probable origin of the pnuclei is the cprocess, which is photodisintegration reactions in supernova explosions [2], [3]. There are 22 p-nuclei associatedwith almost pure s-nuclei that have two more neutrons thanthe p-nuclei. We found the scaling that the abundance
ratios of N9(s)/N9(p), where N9 is each solar abundance,
are almost constant within a factor of 3 over a wide rangeof atomic number. This scaling leads a novel concept of“the universality of the c-process” that the N(s)/N(p) ratiosof nuclei produced in individual supernovae are almost
constant over this wide range [4]. However, the reason why
the scaling and universality appear in the solar abundances
has remained an open question.
We calculated the c-process in oxygen-neon layers incore-collapse supernovae under various conditions [1].

Figure 2: The abundance distribution of the seed nuclei for the p-process
after the weak s-process (filled circles), and as the initial composition (open circles) in a model with M = 25 M9, Z = Z9. The
open circles have been multiplied by 1000. The inset displays
the abundance ratios of the s-processed nuclei to the initial compositions for 22 nuclei, which are members of the scaling.

Figure 1 shows the calculated results, which are constantover a wide range of the atomic number. These results
show that the N(s)/N(p) ratios of nuclei produced by individual supernovae are independent of the astrophysicalconditions. We calculated the change of the abundance distributions of the initial seeds (Fig. 2).
We conclude that three mechanisms contribute to thisuniversality. The first is that both b+ decay and direct (c,n)
reactions contribute to the constant N(s)/N(p) ratios. The
second is a weak s-process before supernovae, which is thereason that the p-nucleus abundances are proportional to
the s-nucleus abundances. The third is the shift of cprocess layers, of which the peak temperature is almost
constant. Our calculations further suggest an extended universality that the s/p ratios in the c- process layers are not
only constant but also centered around a specific value 3(Fig. 1). To verify this, we propose an astronomical observation of Indium isotopic abundance fractions.
References[1] Hayakawa, T., et al.: 2006, ApJL, 648, L47.
[2] Arnould, M., et al.: 1976, A&A, 46, 117.
[3] Woosley, S. E., et al.: 1978, ApJS, 36, 285.
[4] Hayakawa, T., et al.: 2004, PRL, 93, 161102.
[5] Hayakawa, T., et al.: 2005, ApJ, 618, 533.
[6] Shizuma, T., et al.: 2005, PRC, 72, 025808.
[7] Hayakawa, T., et al.: 2006, PRC, 74, 065802.

4100eng 08.2.28 6:41 PM ページ42

Removal of Central Obscuration and Spider Arm Effects
with Beam-Shaping Coronagraphy
ABE, Lyu, TAMURA, Motohide

MURAKAMI, Naoshi, NISHIKAWA, Jun(Extra-Solar Planet Search Project, NAOJ)(MIRA Project, NAOJ)

In this paper, we describe a pre-optics system designed
for high contrast imaging. It is commonly said that highcontrast imaging instruments, like coronagraphs, should be
used on off-axis telescopes. The reason is that most coronagraphs are sensitive to the central obstruction pattern, as
well as supporting spider arms. This kind of pupil geometries usually create unwanted light distribution (diffracted
light) in the Lyot plane, thus limiting the performance ofcoronagraphs.
We propose to use a well suited combination of a small
diffraction mask, associated with a complex amplitude filter in the conjugated pupil plane (the beam shaping filter),to shape the output light beam (both in amplitude andphase), and especially remove the central obstruction andspider arms [1]. The diffraction mask produces a welldefined diffraction pattern in the pupil plane and sends
light at the central obstruction and spider arms locations, sothat coherent light is present in pupil areas where it didn’t
exist before (the original entrance pupil). By correctly modifying the amplitude and phase of the light in these areas(i.e. to perform a beam shaping), we can virtually produce
any kind of output pupil shape: e.g. flat or apodized [2].
The optical scheme is shown on Fig. 1. Note that this diffraction mask is different from the coronagraphic mask: an
independent coronagraph is used after this pre-optics setup.

Figure 1: Schematic of the beam-shaping coronagraphy. The diffraction
effect of a focal mask in the re-imaged pupil naturally fills thecentral obstruction and spider arms structures with coherent light.
A special complex amplitude filter is placed in this pupil in orderto shape the beam as needed for a downstream coronagraph.

We considered two types of focal plane diffraction
masks: simple occulters (circular masks, Lyot type) andπ phase-shifting mask (like in Roddier coronagraphy).
These diffraction masks produce different amplitude distributions in the pupil plane. We studied the optimal combination of such masks and beam shaping filters (in the pupil
plane) so that we can maximize the throughput of the system (which also depends on the desired output pupil amplitude distribution). For a flat (phase and amplitude) output
pupil, the throughput with occulting diffraction masks can

42

be about 60% with a mask as small as 1.2 m/D in diameter.
For Lyot type occulting masks, the complex amplitude filter always need to apply a π phase-shift at the central
obstruction and spider arms. If we use π phase-shiftingmasks as diffracting masks in the focal plane, there issometimes no need to perform other π phase-shifts in the
pupil plane, meaning that the complex amplitude filter canbe amplitude-only.
The phase or amplitude transitions for the complex
amplitude filter are ideally sharp transition, in other words
discontinuities. We studied possible realizations of suchpre-optics system by considering unperfect transition areas.
We conclude, as shown in Fig. 2, that our system offers asignificant gain, with no huge loss in transmission due tothe complex amplitude filter.
Liquid crystal amplitude and phase modulators (Spatial
Light Modulators) are possible candidates for the complex
amplitude filter. Our technique has some chromatic issues
that we did not fully address in this paper, but we point out
some technological solutions that could allow broader band
setups.

Figure 2: Performance of our system combined with a four quadrant
phase mask (FQPM) coronagraph with a Subaru/VLT-like
pupil shape. The curves correspond to the reference image
without coronagraphic mask but with Lyot stop and without
beam-shaping (dotted), the reference image without coronagraphic mask but with Lyot stop and with beam-shaping(dashed), the coronagraphic FQPM image without beam-shaping (dash-dotted green), the coronagraphic FQPM image withbeam-shaping (continuous red).
References[1] Abe, L., et al.: 2006, A&A, 451, 363.
[2] Abe, L., et al.: 2006, SPIE, 6269, 6269501.

00eng 08.2.28 6:41 PM ページ43

Imaging Spectroscopy of a Gradual Hardening Flareon 2000 November 25
TAKASAKI, Hiroyuki, KIYOHARA, Junko

ASAI, Ayumi, NAKAJIMA, Hiroshi(Kyoto University)(NSRO, NAOJ)

YOKOYAMA, Takaaki

MASUDA, Satoshi, SATO, Jun

KOSUGI, Takeo(University of Tokyo)(Nagoya University)(ISAS, JAXA)

Figure 1: Spatial distribution of the emission sources. Left: Ha image of theflare. A microwave and a HXR image are overlaid with the black
and white contours, respectively. Middle: Magnetogram of the active
region. Right: Cartoon which shows the geometrical features of theflare. The light gray shade shows the flare loop seen in soft X-rays.

We examined nonthermal emissions of an M8.2 long
duration flare that occurred on 2000 November 25 [1]. This
flare showed the peculiar hardening features in microwaves
obtained with NoRH 1 and NoRP 2 at Nobeyama Solar
Radio Observatory, and in hard X-rays (HXRs) obtainedwith Yohkoh/HXT3. In these flares it has been thought thatthe magnetic trapping works extremely efficiently. We performed a detailed imaging spectroscopic analysis of nonthermal emission sources for a gradual hardening flare.
We can see a two-ribbon structure (see Fig. 1). A compact HXR source appeared on the eastern flare ribbon,
while a dominant microwave source (source A) appearedon the western flare ribbon and showed no counterparts for
the HXR source in the eastern ribbon. The microwave
source A is located near the sunspot, and therefore, hasstrong magnetic field. We also identified an extended
microwave emission source (source B) which is locatedbetween the two flare ribbons. In the soft X-ray images, we
can see a faint loop structure which connects the flare ribbons. The source B just lies along the faint flare loop. We
performed the imaging spectroscopic analyses for thesemicrowave sources A and B and the HXR source (see Fig.
2). The temporal evolutions of the flux and the spectral
index of the source A are quite similar to those of the
HXRs, and both clearly showed gradual hardening tendencies in their spectra. Therefore, we concluded that almost
all of the accelerated electrons are trapped and dripping to
generate the footpoint microwave source and the HXR
source. However, there is a constant gap between the electron spectral index derived from the source A and that fromthe HXR source. On the other hand, the source B does not

Figure 2: Temporal variation of the spatially-resolved physical parametersof each emission source. Top: electron energy spectral index
derived from the HXR emission dHXR, and those derived from themicrowave dµ for emission sources, A and B. Middle: microwave(in 17 GHz) light curves integrated over each emission source(scaled arbitrarily). Bottom: light curve of the total HXR intensity.

show any similarity to the HXR and microwave footpoint
sources, while its observational features such as gradualtime profile and very hard spectrum show that this source isalso generated by trapped electrons. This is probably
because the effective energy of the trapped electrons that
emit the gyrosynchrotron emission at the loop top (sourceB) should be larger than about 1 MeV.
From these observational results, we suggest that
almost all of the accelerated electrons are trapped in theloops and dripping into the footpoints. The microwave
source A is generated by dripping of the trapped electrons,
and most of the electrons are reflected by mirror effect due
to strong magnetic field and precipitate into the HXR footpoint source. On the other hand, the source B just reflects
the trapped electrons. The gap of the indices is thought tobe essential in this flare, and the energy spectrum show abreakup feature in nature if we consider that effective energy of electrons which contribute to the source A is higher
than that in the HXR source. Since the magnetic loop is
quite asymmetric, the anisotropic pitch angle distribution
could be required for the forcible trapping effect in such an
asymmetrical magnetic loop. These results could show thatproperties of the gradual component must be produced by adifferent acceleration mechanism from that of the impulsive phase, and that the additional acceleration in theshrinking magnetic loops could be a candidate.

1

Nobeyama RadioheliographNobeyama Radio Polarimeters
3
Hard X-ray Telescope
2

References[1] Takasaki, H., et al.: 2007, ApJ, 661, 1234.

4300eng 08.2.28 6:41 PM ページ44

Solar Heating Effect on Meteoroids in Meteor Showers
KASUGA, Toshihiro(RISE Project, NAOJ)

WATANABE, Juni-chi

YAMAMOTO, Tetsuo(Public Relations Center, NAOJ)(Hokkaido University)

SATO, Mikiya

KIMURA, Hiroshi(Public Relations Center, NAOJ)(Hokkaido University)

The observed sodium abundance of meteoroids in meteor showers might differ from the original abundance
because of processing in interplanetary space after ejections
from their parent bodies. Among various processes, thermal
alteration of alkali silicate is most likely the major processof Na depletion [1], [2], [3].
Aim is for clarifying at which perihelion distances thethermal desorption alters the Na content of meteoroids thatare observed as meteor showers. Method is compilation Na
abundances of meteoroids in meteor showers at each perihelion distance and compare them to the sublimation temperatures of alkali silicates. Results are that Na abundancesof meteoroids do not depend on their perihelion distances
at 0.14 ≤ q ≤ 0.99AU. No Na depletion in these distances
constrains the temperature of meteoroids at q = 0.14AU to
be lower than the sublimation temperature of alkali silicates~ 900 K. We conclude that meteoroid particles are characterized as large, compact, blackbody - like particles. On
orbit with perihelion distances q < 0.1AU, meteoroids
would show evidence of thermal desorption of metals, inparticular, Na [3].
Solar heating effect on their parent bodies is also possible event. Asteroid 3200 Phaethon is suggested for a candidate of the direct Impact research. The object is considered
to be the dormant comet and the parent of the Geminid
meteor shower. Instead, one could say that there are somepossible arguments for a space impact mission, and thenshow the additional interesting possibility of artificiallygenerated meteor showers. Dust trail theory can calculate abundle of trails’ distribution and be used to show in which
years artificial meteors would be expected. Results indicatethat meteor showers are seen on Earth about 200 years laterfrom the event on 12 April in 2022 [2].

44

Figure 1: Temperatures of dust particle as a function of the perihelion
distance. Also plotted are the averaged Na/Mg ratios deduced
from data. Sublimation temperature of sodalite is shown by
the horizontal line (the right axis). The stripe band shows solar
Na/Mg ratio (the left axis) and sublimation temperature offeldspar (the right axis). The perihelion distances of meteor
showers are q ~ 0.14AU (A) for Geminid, 0.38AU (B) for
Taurid, 0.78AU (C) for Andromedid, 0.95AU (D) for Perseid,
0.98-0.99AU (E) for Leonid, Cygnid and Draconid.
References[1] Kasuga, T.: 2006, Planetary People, 15, 94.
[2] Kasuga, T., et al.: 2006, MNRAS, 373, 1107.
[3] Kasuga, T., et al.: 2006, A&A, 453, L17.

00eng 08.2.28 6:41 PM ページ45

Li Production by the Radiative Decay of Long-Lived
Particles
KUSAKABE, Motohiko

KAJINO, Toshitaka

MATHEWS, G. J.

(UT/NAOJ)(NAOJ/UT)(University of Notre Dame)

Figure 1: Gray regions are the excluded area in the parameter space ( x X ,g X ) for models with a fixed baryon to photon ratio of
h =6.1 # 10–10. The dark gray region is excluded by an overabundance of 3He, whereas the light shaded region is mostly
excluded by an underabundance of deuterium. The black shaded region is excluded by the CMB blackbody energy spectrum.
The curved line identifies the contour of 6Li/H = 6.6 # 10–12 ,the abundance of 6Li observed in MPHSs. The region above
the contour and below the nucleosynthesis and CMB constraints is allowed and abundant in 6Li.

Recent spectroscopic observations of metal poor stars
have indicated that both 7 Li and 6 Li have abundanceplateaus with respect to the metallicity~[2]. Abundances of7
Li are about a factorthree lower than the primordial abundance predicted by standard big-bang nucleosynthesis(SBBN), and 6Liabundances are ~ 1/20 of 7Li, whereas
SBBN predicts negligibleamounts of 6Li compared to thedetected level. Thesediscrepancies suggest that 6Li has
another cosmological or Galacticorigin than the SBBN.
Furthermore, it could appear that 7Li (andalso 6Li) has been
depleted from its primordial abundance by somepost-BBN
processes [3]. We study the possibility that the radiative
decay of long-lived particleshas affected the cosmologicallithium abundances. We calculate thenon-thermal nucleosynthesis associated with the radiativedecay, and explore
the allowed region of the parametersspecifying the properties of long-lived particles X, i.e. a lifetime x X andg X = (n X0 /n c0 ) E c0 , where (n X0 /n c0 ) is equal to a number ratioof X to photon before X-decay and E c0 is the emitted photon

Figure 2: Ratio of calculated 6Li/H abundances to the observed abundance in MPHSs as a function of x X . Results in the allowed
parameter region of ( x X , g X ) producing 6Li/H larger than thevalue found in MPHSs, or the marked region “ 6Li ” in Fig. 1
are plotted by small squares. The horizontal line indicates afactor of three overproduction of 6Li. The large circles denotevalues in the allowed region with abundances of
3
He/H=1.3–2.5×10-5 and 6Li/H $ 3 # 6.6 # 10 - 12 ..

energy in theradiative decay. We also impose constraints
from observations of the CMB energy spectrum. It is foundthat non-thermalnucleosynthesis produces 6Li at the level
detected in metal poor halostars (MPHSs) , when the lifetimeof the unstable particles is of the order ~ 108 – 1012s andtheir initial abundance with respect to that of thephotons is~ (10–13 – 10–12 ~ GeV)/ Ec0 (Fig. 1, 2).
We conclude that a combination of two different
processes could explain thelithium isotopic abundances in
MPHSs. First, a non-thermal cosmological nucleosynthesis
associated with theradiative decay of unstable particles; andsecond, about the same degreeof stellar depletion of bothprimordial lithium isotopic abundances. If MPHSs experience 6Li depletion of factor much greater than ~3, the simple radiative decay process can not be the cause of large 6Li
abundances in MPHSs.
References[1] Kusakabe, M., et al.: 2006, PRD, 74, 023526[2] Asplund, M., et al.: 2006, ApJ, 644, 229.
[3] Lambert: 2005, AIP Conf. Proc.743, 206.

45

文献英文 08.3.2 10:34 AM ページ46

II Publications, Presentations
1. Referenced Publications
Abbott, B., et al. including Arai, K., Beyersdorf, P., Fujimoto,M., Fukushima, M., Hayama, K., Kawamura, S., Kozai,Y., Miyama, S., Ohishi, N., Sato, S., Takahashi, R.,
Tatsumi, D., Tsunesada, Y., Ueda, A., Waseda, K.,
Yamazaki, T., Zhu, Z. H.: 2006, Joint LIGO and TAMA300
Search for Gravitational Waves from Inspiralling NeutronStar Binaries, Phys. Rev. D, 73, 102002.
Abbott, B., et al. including Kawamura, S.: 2006, Search for
Gravitational Waves from Binary Black Hole Inspirals in
LIGO data, Phys. Rev. D, 73, 62001.
Abbott, B., et al. including Kawamura, S.: 2006, Search for
Gravitational-Wave Bursts in LIGO’s Third Science Run,Class. Quantum Grav., 23, S29-S39.
Abe, L., Murakami, N., Nishikawa, J., and Tamura, M.:
2006, Removal of Central Obscuration and Spider Arms
Effects with Beam Shaping Coronagraphy, A&A, 451, 363373.
Abe, L., Beaulieu, M., Vakili, F., Gay, J., Rivet, J.-P., Dervaux,S., et Domiciano de Souza, A.: 2007, On-Sky Observations
with an Achromatic Hybrid Phase Knife Coronagraph in the
Visible, A&A, 461, 365-371.
Akutsu, T., et al. including Arai, K., Beyersdorf, P., Fujimoto,M., Fukushima, M., Kawamura, S., Miyama, S., Ohishi,N., Sato, S., Takahashi, R., Tatsumi, D., Tsunesada, Y.,
Ueda, A., Waseda, K., Yamazaki, T., Zhu, Z, H.: 2006,
Results of the Search for Inspiraling Compact Star Binaries
from TAMA300’s Observation in 2000-2004, Phys. Rev. D,
74, 122002.
Akutsu, T., Ando, M., Kanda, N., Tatsumi, D., Telada, S.,
Miyoki, S., Ohashi, M.: 2006, Veto Analysis for
Gravitational Wave Burst Signals in TAMA300 Data Usingan ALF Filter, Class. Quantum Grav., 23, S23-S28.
Akutsu, T., Ando, M., Kanda, N., Tatsumi, D., Telada, S.,
Miyoki, S., Ohashi, M.: 2006, Analysis of Gravitational
Wave Bursts in TAMA300 Data Using an ALF Filter, Class.
Quantum Grav., 23, S715-S721.
Ando, M., Ohta, K., Iwata, I., Akiyama, M., Aoki, K.,
Tamura, N.: 2006, Deficiency of ｌarge equivalent widthLy emission in luminous lyman break galaxies at z ~ 5-6?,
ApJ, 645, L9.
Aoki, K., Iwata, I., Ohta, K., Ando, M., Akiyama, M.,
Tamura, N.: 2006, Discovery of H Absorption in the
Unusual Broad Absorption Line Quasar SDSS
J083942.11+380526.3, ApJ, 651, 84.
Aoki, W., Frebel, A., Christlieb, N., Norris, J. E., Beers, T. C.,
Minezaki, T., Barklem, P. S., Honda, S., Takada-Hidai, M.,
Asplund, M., Ryan, S. G., Tsangarides, S., Eriksson, K.,
Steinhauer, A., Deliyannis, C. P., Nomoto, K., Fujimoto, M.
Y., Ando, H., Yoshii, Y., Kajino, T.: 2006, HE1327-2326,
an Unevolved Star with [Fe/H]<-5.0. I. A Comprehensive
Abundance Analysis, ApJ, 639, 897-917.
Aoki, W., Beers, T. C., Christlieb, N., Norris, J. E., Ryan, S. G.,
Tsangarides, S.: 2007, Carbon-Enhanced Metal-Poor Stars. I.

46

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Shigeyama, T., Nakamura, K., Wanajo, S., Inoue, S.: 2006,
Light Element Production in Type Ic Supernovae, AIP Conf.
Ser. 847, Eds. S. Kubono, W. Aoki, T. Kajino, T.
Motobayashi, K. Nomoto, 105.
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.,
Sakamoto, M.: 2006, Constructing the Subaru Advanced Data
and Analysis Service on VO, ADASS XVI Proc.
Shirasaki, Y., Tanaka, M., Kawanomoto, S., Honda, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J.: 2006, Japanese Virtual
Observatory (JVO) as an Advanced Astronomical Research
Environment, SPIE 6274, 42-54.
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Mizumoto, Y., Ohishi, M., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J.: 2006, Japanese Virtual
Observatory (JVO): Implementation of VO Standard
Protocols, Astronomical Data Analysis Software and Systems
XV, 456-459.
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J.: 2006, Study on the Environment
around QSOs with redshift of 1~3 Using the JVO System,
26th meeting of the IAU General Assembly, Special Session 3,
17.
Shitov, S. V., Vystavkin, A. N.: 2006, A Design Analysis of
Imaging Radiometer with Antenna-Coupled Transition-Edge
Sensors, Proc. of the 11th Int. Workshop on Low
Temperature Detectors, 503-505.
Sôma, M.: 2006, Results from the Recent Lunar Occultations ofUpsilon Geminorum and Antares, Journées 2005 - Systèmesde Référence Spatio-Temorels on Earth dynamics and reference systems: five years after the adoption of the IAU 2000
Resolutions, Eds. A. Brzeziński, N. Capitaine, B. Kolaczek,
83-84.
Sôma, M., Hayamizu, T.: 2006, (22) Kalliope and (22) Kalliope
I, Central Bureau Electronic Telegram No. 732, 733, IAU
CBAT.
Sôma, M., Tanikawa, K.: 2006, Abrupt Changes of the Earth's

Rotation Speed in Ancient Times, Journées 2005 - Systèmesde Référence Spatio-Temorels on Earth dynamics and reference systems: five years after the adoption of the IAU 2000
Resolutions, Eds. A. Brzeziński, N. Capitaine, B. Kolaczek,
133-134.
Stepanov, A. V., Shibasaki, K., Kopylova, Y. G., Tsap, Y. T.:
2006, MHD-Oscillations of Coronal Loops and Diagnostics
of Flare Plasma, Proc. of Nobeyama Symp. 2004, Solar
Physics with the Nobeyama Radioheliograph, 23-32.
Suganuma, M., Kobayashi, Y., Gouda, N., Yano, T.,
Yamada, Y., Takato, N., Yamauchi, M.: 2006, AluminumMade 5-cm Reflecting Telescope for Nano-JASMINE, SPIE
6265, Eds. J. C. Mather, H. A. MacEwen, M. W. M. deGraauw, 626545-1-626545-12.
Suganuma, M., Kobayashi, Y., Gouda, N., Yano, T.,
Yamada, Y., Takato, N., Yamauchi, M.: 2006, Developmentof a Very Small Telescope for Space Astrometry Surveyor,
Exploiting Large Surveys for Galactic Astronomy (IAU26
JD13), #29.
Suganuma, M., Kobayashi, Y., Gouda, N., Yano, T.,
Yamada, Y., Takato, N., Yamauchi, M.: 2006, Developmentof a Very Small Telescope for Space Astrometry Surveyor,
Journal of the Italian Astronomical Society, 77, Eds. C.
Corbally, C. Bailer-Jones, S. Giridhar, T. Lloyd Evans, 1187.
Sumiyoshi, K., Suzuki, H., Yamada, S.: 2006, Fate of CoreCollapse Supernovae: Formation of Neutron Star and Black
Hole, AIP Conf. Proc. 847, Eds. S. Kubono, W. Aoki, T.
Kajino, T. Motobayashi, K. Nomoto, 473-475.
Suwa, Y., Takiwaki, T., Kotake, K., Sato, K.: 2006,
Magnetorotational Collapse of Very Massive Stars:
Formation of Jets and Black Holes, AIP Conf. Ser. 847, Eds.
S. Kubono, W. Aoki, T. Kajino, T. Motobayashi, K. Nomoto,476-478.
Suzuki, T., Chiba, S., Iwamoto, O., Kajino, T.: 2006, NeutrinoNucleus Reactions Induced by Supernova Neutrinos, AIP
Conf. Ser. 847, Eds. S. Kubono, W. Aoki, T. Kajino, T.
Motobayashi, K. Nomoto, 479-481.
Tada, H., Kawaguchi, K., Izumiura, H., Civis, S., Sedivcova',
T.: 2006, Observational Studies Relating To Diffuse
Interstellar Bands, AIP Conf. Proc. 855, Eds. R. I. Kaiser, P.
Bernath, Y.Osamura, S. Petrie, 219-224.
Tajitsu, A., Otsuka, M.: 2006, High Dispersion Spectroscopyof the PN K 648 in the Globular Cluster M 15, IAU Symp.
234, Eds. M. J. Barlow, R. Mendez, 523-524.
Takahashi, R.: 2006, Amplitude and Phase Fluctuations for
Gravitational Waves Propagating Through Inhomogeneous
Mass Distribution in the Universe, 6th Int. LISA Symp., Eds.
S. M. Merkowitz, J. C. Livas, 120.
Takahashi, R., Chiba, T.: 2006, Weak Lensing of Galaxy
Clusters in Relativistic MOND theory, The 16th Workshop on
General Relativity and Gravitation, Ed. K. Oohara.
Takahashi, S., Shimajiri, Y., Takakuwa, S., Saito, M., Kawabe,
R.: 2007, Survey Observations of Large-Scale Molecular
Outflows Associated with Intermediate-Mass Protostar
Candidates in the OMC-2/3 Region, IAU Symp. 237, Eds. B.
G. Elmegreen, J. Palous, 479.
Takami, H., Colley, S., Dinkins, M., Eldred, M., Guyon, O.,
Golota, T., Hattori, M., Hayano, Y., Ito, M., Iye, M., Oya,S., Saito, Y., Watanabe, M.: 2006, Status of Subaru Laser63文献英文 08.3.2 10:34 AM ページ64

Guide Star AO System, SPIE 6272, Eds. B. L. Ellenbroek, D.
Bonaccini Calia, 10.
Takano, S.: 2006, Molecular Abundances in Galaxies, AIP
Conf. Proc. 855, Eds. R. I. Kaiser, P. Bernath, Y.Osamura, S.
Petrie, 170-175.
Takano, S., Nakai, N., Kawaguchi, K., Takano, T., Schilke, P.,
Winnewisser, G.: 2006, Systematically Peculiar MolecularComposition in M 82: Regarding the Formation Mechanisms,
Highlights of Astronomy, Vol. 13 : As Presented at the XXVthGeneral Assembly of the IAU, 875-878.
Takato, N., Terada, H.: 2006, Near-infrared Direct VisionPrism for Wide-Wavelength Coverage Spectroscopy at theSubaru Telescope, SPIE 6269, Eds. I. S. McLean, M. Iye,
626923.
Takeda, T., Ohtsuki, K.: 2007, Angular Momentum Transfer
Efficiency in Collisions Between Rubble Pile Objects, 38th
Lunar ad Planetary Sci. Conf., #1473.
Tamura, M., Abe, L.: 2006, Direct Explorations of Exoplanetswith the Subaru Telescope and Beyond, IAU Colloq. 200,
Eds. C. Aime, F. Vakili, 323-328.
Tamura, M., Hodapp, K., Takami, H., Abe, L., Suto, H.,
Guyon, O., Jacobson, S., Kandori, R., Morino, J.,
Murakami, N., Stahlberger, V., Suzuki, R., Tavrov, A.,
Yamada, H., Nishikawa, J., Ukita, N., Hashimoto, J.,
Izumiura, H., Hayashi, M., Nakajima, T., Nishimura, T.:2006, Concept and Science of HiCIAO: High Contrast
Instrument for the Subaru Next Generation Adaptive Optics,
SPIE 6269, Eds. I. S. McLean, M. Iye, 62690V.
Tanaka, M., Kodama, T.: 2006, The Build-up of the ColourMagnitude Relation, Galaxy Evolution Across the Hubble
Time, IAU Symp. 235.
Tanaka, M., Shirasaki, Y., Kawanomoto, S., Honda, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Ishihara, Y.,
Tsutsumi, J., Kobayashi, Y.: 2006, Web Service Interface andWorkflow Mechanism for JVO, Astronomical Data Analysis
Software and Systems XV, 460-462.
Tanaka, S., Nakagawa, T., Kataza, H., Enya, K., Tamura, M.,
Abe, L.: 2006, Shaped Pupil Coronagraphs for High-Contrast
Imaging with SPICA, IAU Colloq. 200, Eds. C. Aime, F.
Vakili, 481-484.
Tatsumi, D., Arai, K., the TAMA collaboration: 2006, Online
Monitoring of Alignment Noises in TAMA300, J. Phys.:Conf. Ser. 32, 94-98.
Terada, K., Yoshida, T., Iwamoto, N., Aoki, W., Williams, I.
S.: 2006, Eu Isotopic Analyses of SiC Grains from the
Marchison Meteorite, AIP Conf. Ser. 847, Eds. S. Kubono,
W. Aoki, T. Kajino, T. Motobayashi, K. Nomoto, 324-329.
Tolstoy, E., Hill, V., Irwin, M., Helmi, A., Battaglia, G.,
Letarte, B., Venn, K., Jablonka, P., Shetrone, M., Arimoto,N., et al.: 2006, The Dwarf galaxy Abundances and RadialVelocity Team (DART) Large Programme - A Close Look at
Nearby Galaxies, The Messenger, 123, 33.
Tosaki, T., Nakanishi, K., Tsuboi, M., Trushkin, S., Kameya,O., Fujisawa, K., Kotani, T., Kawai, N.: 2006, Cyg X-3 is in
the Active State, The Astronomer's Telegram, 952.
Tosaki, T., Shioya, Y., Kuno, N., Nakanishi, K., Hasegawa,T., Matsushita, S., Kohno, K., Miura, R., Tamura, Y.,
Okumura, S. K., Kawabe, R.: 2007, Dense Molecular Gas
Formation Triggered by Spiral Density Wave in M 31, IAU

64

Symp. 237, Eds. B. G. Elmegreen, J. Palous, 368-372.
Tsuboi, M., Okumura, S. K., Miyazaki, A.: 2006, Interaction
between the SNR Sagittarius A East and the 50-km S-1
Molecular Cloud, J. Phys.: Conf. Ser. 54, Eds. R. Schödel, G.
C. Bower, M. P. Muno, S. Nayakshin, T. Ott, 16-21.
Tsujimoto, T., Kobayashi, N., Ikeda, Y., Kondo, S., Yasui, C.,
Minami, A., Motohara, K., Gouda, N.: 2006, A Near-Infrared
High-Resolution Spectroscopic Survey of Galactic Bulge
Stars, Journal of the Italian Astronomical Society, 77, Eds. C.
Corbally, C. Bailer-Jones, S. Giridhar, T. Lloyd Evans, 1188.
Tzatzakis, V., Nindos, A., Alissandrakis, C. E., Shibasaki, K.:
2006, A Statistical Study of Microwave Flare Morphologies,
AIP Conf. Proc. 848, Ed. N. Solomos, 248-252.
Uchiyama, T., Miyoki, S., Ohashi, M., Kuroda, K., Yamamoto,K., Tokunari, M., Akutsu, T., Kamagasako, S., Nakagawa,N., Kirihara, H., Agatsuma, K., Ishitsuka, H., Tatsumi, D.,
Telada, S., Ando, M., Tomaru, T., Suzuki, T., Sato, N.,
Haruyama, T., Yamamoto, A., Shintomi, T.: 2006, Cryogenic
Systems of the Cryogenic Laser Interferometer Observatory,
J. Phys.: Conf. Ser. 32, 259-264.
Ukita, N., Saito, M., Ikenoue, B., Mangum, J. G., Emerson, N.
J., Otarola, A. C., Stanghellini, S.: 2006, Vortex Shedding
from a 12-m Antenna, SPIE 6267, Ed. L. M. Stepp, 122.
Uraguchi, F., Takato, N., Miyashita, A., Usuda, T.: 2006,
The DIMM Station at Subaru Telescope, SPIE 6267, Ed. L.
M. Stepp, 21.
Usuda, K. S.: 2006, Fiding Rainbows Everywhere: Making a
Spectroscope with a Compact Disk, CATALYST: The Hawaii
Science Teacher Association Newsletter, Ed. R. Warehime, 7.
Van Hoof, P. A. M., Bryce, M., Evans, A., Eyres, S. P. S.,
Hajduk, M., Herwig, F., Kerber, F., Kimeswenger, S., Lopez,
J. A., Matsuura, M., Pollacco, D. L., Van de Steene, G. C.,
Zijlstra, A. A.: 2006, The Real-Time Evolution of Sakurai sStar (V4334 Sgr) and other (V) LTP Objects, IAU Symp. 234,
Eds. M. J. Barlow, R. H. Mendez, 75.
Vystavkin, A. N., Shitov, S. V., Kovalenko, A. G., Pestriakov,
A. V., Cohn, I. A., Uvarov, A. V.: 2006, Arrays of TES
Direct Detectors for Supersensitive Imaging Radiometers of
1.0 – 0.2 mm Waveband Region, Proc. WPP264 of European
Space Agency, Seventh Int. Workshop on Low Temperature
Electronics", 101-108.
Watanabe, T., Kato, T., Murakami, I., Yamamoto, M.: 2007,
Solar and LHD Plasma Diagnostics, AIP Conf. Proc. 901, Ed.
E. Roueff, 215-220.
Winnberg, A., Deguchi, S., Habing, H. J., Nakashima, J.,
Olofsson, H., Reid, M. J.: 2006, Circumstellar CO in OH/IR
Stars Close to the Galactic Centre, J. Phys.: Conf. Ser. 54,
Eds. R. Schödel, G. C. Bower, M. P. Muno, S. Nayakshin, T.
Ott, 166-170.
Yamada, M., Koyama, H., Omukai, K., Inutsuka, S.: 2006,
Synthetic Observations of Turbulent Flows in Diffuse
Multiphase Interstellar Medium, IAU Symp. 237, Eds. B. G.
Elmegreen, J. Palous.
Yamada, Y., Gouda, N., Yano, T., Kobayashi, Y., Tsujimoto,T., Suganuma, M., Niwa, Y., Sako, N., Hatsutori, Y.,
Tanaka, T., JASMINE WG: 2006, JASMINE Simulator,
SPIE 6265, Eds. J. C. Mather, H. A. MacEwen, M. W. M. deGraauw, 626541-1 -626541-8.
Yamada, Y., Gouda, N., Yano, T., Sako, N., Hatsutori, Y.,文献英文 08.3.2 10:34 AM ページ65

Tanaka, T., Yamauchi, Y., JASMINE WG: 2006, JASMINE
Simulator, Journal of the Italian Astronomical Society, 77,
Eds. C. Corbally, C. Bailer-Jones, S. Giridhar, T. Lloyd
Evans, 1190.
Yamamoto, T., Sakurai, T.: 2006, Upward Velocities of theReconnection Points and Coronal Magnetic Field Strengths in
Flaring Regions Derived from the GOES X-Ray Light
Curves, IAU Symp. 233, Eds. V. Bothmar, A. A. Hady, 128129.
Yamamoto, H., Fukui, Y. F., Fujishita, M. F., Kudo, N. K.,
Nozawa, H. N., Takahashi, K. T., Matsumoto, R., Machida,M., Kawamura, A. K., Mizuno, N. M., Onishi, T. O., Mizuno,
A. M.: 2006, Molecular Loops in the Galactic Centre;
Evidence for Magnetic Floatation Accelerating MolecularGas, IAU Symp. 237, Eds. B. G. Elmegreen, J. Palous, 247.
Yamazaki, D. G., Ichiki, K., Kajino, T., Mathews, G. J.: 2006,
Constraint of Cosmological Magnetic Field from Likelihood
Analysis, Frontiers Sci. Ser., 46, Eds. H. Suzuki, J.
Yokoyama, Y. Suto, K. Sato, 215-216.
Yamazaki, D. G., Ichiki, K., Kajino, T., Mathews, G. J.: 2006,
Primordial Magnetic Field Constrained from CMB
Anisotropies, and its Generation and Evolution Before,
During and After the BBN, PoS(NIC-IX), 194.
Yanagisawa, K., Shimizu, Y., Okita, K., Nagayama, S., Sato,Y., Koyano, H., Okada, T., Iwata, I., Uraguchi, F.,
Watanabe, E., Yoshida, M., Okumura, S., Nakaya, H.,
Yamamuro, T.: 2006, ISLE: a General Purpose Near-Infrared
Imager and Medium-Resolution Spectrograph for the 1.88-m
Telescope at Okayama Astrophysical Observatory, SPIE
6269, Eds. I. S. McLean, M. Iye, 62693Q.
Yanagisawa, K., Kawai, N.: 2006, GRB 060403: MITSuME
Optical Observation., GRB Coordinates Network, CircularService, 4954, 1.
Yano, T., Araki, H., Gouda, N., Kobayashi, Y., Tsujimoto,T., Nakajima, T., Kawano, N., Tazawa, S., Yamada, Y.,
Hanada, H., Asari, K., Tsuruta, S.: 2006, CCD Centroiding
Experiment for JASMINE and ILOM, SPIE 6265, Eds. J. C.
Mather, H. A. MacEwen, M. W. M. de Graauw, 626543-1626543-12.
Yano, T., Gouda, N., Yamada, Y.: 2006, New Method for
Astrometric Measurements in Space Mission, JASMINE,
Journal of the Italian Astronomical Society, 77, Eds. C.
Corbally, C. Bailer-Jones, S. Giridhar, T. Lloyd Evans, 1189.
Yoshida, T.: 2006, Seven-Layer Supernova Mixtures
Reproducing Isotopic Ratios of Presolar Grains, AIP Conf.
Ser. 847, Eds. S. Kubono, W. Aoki, T. Kajino, T.
Motobayashi, K. Nomoto, 500-502.
Yoshida, T., Kajino, T., Yokomakura, H., Kimura, K.,
Takamura, A., Hartmann, D. H.: 2006, The Effect of Neutrino
Oscillations on Supernova Light Element Synthesis, AIP
Conf. Ser. 847, Eds. S. Kubono, W. Aoki, T. Kajino, T.
Motobayashi, K. Nomoto, 134-139.
Yoshida, M., Yanagisawa, K., Kawai, N.: 2007, GRB 070125:
MITSuME Okayama Optical Observation., GRB Coordinates
Network, Circular Service, 6050, 1.
Yoshida, M., Yanagisawa, K., Kawai, N.: 2007, GRB 070220:
MITSuME Okayama Optical Observation., GRB Coordinates
Network, Circular Service, 6123, 1.
Yoshida, M., Yanagisawa, K., Shimizu, Y., Kawai, N.: 2007,

GRB 070311: MITSuME Okayama Optical Observation,
GRB Coordinates Network, Circular Service, 6193, 1.
Yoshizawa, M., Nishikawa, J., Ohishi, N., Suzuki, S., Torii,
Y., Iwashita, H., Kubo, K., Matsuda, Ko., Murakami, N.,
Matsukawa, A., Nishimura, T., Okayasu, N., Watanabe, S.:
2006, MIRA Status Report: Recent Progress of MIRA-I.2 andFuture Plans, SPIE 6268, Eds. J. D. Monnier, M. Schöller, W.
C. Danchi, 626808.
Zijlstra, A., Lagadec, E., Matsuura, M., Chesneau, O., Etoka,
S.: 2006, The Compact Discs of Post-AGB Stars, ESO
Messenger, 124, 21.
5. Publications in English
McLean, I., Iye, M.: 2006, Ground-base and Airborne
Instrumentation for Astronomy, SPIE, USA.
Kubono, S., Kajino, T., Aoki, W., Nomoto, K.-I.,
Motobayashi, T.: 2006, Origin of Matter and Evolution of
Galaxies, AIP, USA.
6. Conference Presentations
Agata, H.: 2006, Science as a Culture, and an Introduction to
New Public Understanding of Research (PUR) Experiments
in Japan, The 9th Int. Conf. on Public Communication of
Science & Technology, (Seoul, Korea, May 17-19).
Akutsu, T., Kawamura, S., Arai, K., Tatsumi, D., Nagano, S.,
Yamamoto, K., Sugiyama, N., Chiba, T., Takahashi, R.,
Nishizawa, A., Nishida, E., Fukushima, M., Yamazaki, T.,
Fujimoto, M.: 2006, Development of a Laser Interferometer
for MHz Gravitational-Wave Detection, Gravitational Wave
Advanced Detector Workshop 2006, (Elba, Italy, May 27June 1).
Aoki, W.: 2006, Neutron-Capture Elements in Metal-PoorStars, Int. Program 06-2a The First Stars and Evolution of
the Early Universe, (Seattle, USA, July 3-7).
Aoki, W.: 2006, Neutron-Capture Processes in the Early
Galaxy, Int. Symp. on Nuclei in Cosmos IX, (CERN, Genève,
Switzerland, June 25-30).
Aoki, W., Beers, T. C., Christlieb, N., Frebel, A., Norris, J. E.,
Honda, S., Takada-Hidai, M., Asplund, M., Ando, H., Ryan,
S. G., Tsangarides, S.: 2006, Chemical Abundance Patterns ofExtremely Metal-Poor Stars, Int. Symp. on Nuclei in Cosmos
IX, (CERN, Genève, Switzerland, June 25-30).
Araki, H., Hanada, H., Noda, H., Matsumoto, K., Sasaki, S.,
Tsubokawa, T., Tsuruta, S., Asari, K., Tazawa, S.,
Kawano, N., Yano, T.: 2006, Investigations of Ilon Project in situ Lunar Orientation Measurement by a PZT Telescopeon the Moon, 25th Int. Symp. on Speace Technology and
Science, (Kanazawa, Japan, June 4-11).
Araki, H., Tazawa, S., Sasaki, S., Noda H., Tsubokawa, T.,
Asari K., Kawano, N.: 2006, Lunar Global Topography by
Laser Altimeter (LALT) on board SELENE, European
Planetary Science Congress 2006, (Berlin, Germany, Sept.
18-22).
Araki, H., Tazawa, S., Noda, H., Tsubokawa, T., Kawano,N.: 2006, Lunar Global Topography by Laser Altimeter(LALT) on board SELENE, 36th COSPAR Scientific
Assembly, (Beijing, China, July 16-23).

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Araki, H., Tazawa, S., Noda, H., Tsubokawa, T., Kawano,N.: 2006, Lunar Global Topography by Laser Altimeter(LALT) on board SELENE, 8th ILEWG Conf., (Beijing,
China, July 23-27).
Araki, H., Tazawa, S., Noda, H., Tsubokawa, T., Kawano,N., Sasaki, S.: 2006, Observation of the Lunar Topography
by the Laser Altimeter (LALT) on board SELENE, 1st
SELENE SWTM, (Tsukuba, Japan, Jan. 9-11).
Araki, H., Tazawa, S., Tsubokawa, T., Noda, H., Kawano,N.: 2006, Observation and Sciences of Lunar Topography by
Laser Altimeter (LALT) on board SELENE, 25th Int. Symp.
on Speace Technology and Science, (Kanazawa, Japan, June
4-11).
Arimoto, N.: 2006, A Wide Area Survey for High-Redshift
Massive BzK Galaxies, Galaxies and Structures throughCosmic Times, (Venice, Italy, Mar. 26-31).
Arimoto, N.: 2006, Galactic Archaeology of the Local Group
Galaxies, Cosmology with wide-field Photometric andSpectroscopic Galaxy Survey, (Tokyo, Japan, Nov. 9-10).
Arimoto, N.: 2006, Origin of Two Distinct Populations in
Dwarf Spheroidal Galaxies, Mapping the Galaxy and Nearby
Galaxies, (Ishigaki Island, Okinawa, Japan, June 26-30).
Arimoto, N.: 2006, Stellar Populations of BzK Galaxies, IAU
Symp. 241 Stellar Populations as Building Blocks of
Galaxies, (La Palma, Canary Islands, Spain, Dec. 10-16).
Ariyoshi, S., Otani, C., Dobroiu, A., Matsuo, H., Sato, H.,
Taino, T., Kawase, K., Shimizu, H. M.: 2006, Terahertz
Imaging with a Linear Array Detector Based on
Superconducting Tunnel Junctions, The Joint 32nd Int. Conf.
on Infrared and Millimetre Waves and 15th Int. Conf. on
Terahertz Electronics, (Shanghai, China, Sept. 18-22).
Asada, K.: 2006, Expanding Radio Lobe Revealed by VSOP
Observations, Challenges of Relativistic JETS, (Cracow,
Poland, June 25-July 1).
Asada, K., et al.: 2006, Further Evidence of Helical Magnetic
Field, The Central Engine of Active Galactic Nuclei, (Xian,
China, Oct. 16-21).
Asai, A.: 2006, Loop Top Nonthermal Emissin Sources
Associated with an Over-the-Limb Flare Observed with
NoRH and RHESSI, 36th COSPAR Scientific Assembly,(Beijing, China, July 16-23).
Asai, A., Ishii, T. T., Shibata, K., Gopalswamy, N.: 2006,
Anemone Structure of Active Region NOAA 10798 andRelated Geoeffective Flares/CMEs, Int. Astronomical Union
XXVIth General Assembly, (Prague, Czech, Aug. 14-25).
Asai, A., Ishii, T. T., Shibata, K., Gopalswamy, N.: 2006,
Anemone Structure of AR NOAA 10798 and Related GeoEffective Flares and CMEs, 36th COSPAR Scientific
Assembly, (Beijing, China, July 16-23).
Asai, A., Ishii, T. T., Shibata, K., Gopalswamy, N., Kataoka,
R., Oka, M.: 2006, Anemone Structure of Active Region
NOAA 10798 and Related Geoeffective Flares/CMEs,
CAWSES Int. Workshop on Space Weather Modeling,(Yokohama, Japan, Nov. 14-17).
Asai, A., Nakajima, H., Oka, M., Nishida, K., and Tanaka, Y.:
2006, Loop Top Nonthermal Emission Sources Associatedwith an Over-the Limb Flare Observed with NoRH and
RHESSI, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).

66

Asano, K.: 2006, Neutrino and Gamma-ray Emissions
Originated from Hadrons in GRBs, Swift and GRBs:
Unveiling the Relativistic Universe, (Venezia, Italy, June 59).
Asano, K.: 2006, Photons and Neutrinos Originating fromAccelerated Protons in GRBs, 4th Korean Astrophysics
Workshop, Origin, Propagation and Interaction of Energetic
Particles, (Daejeon, Korea, May 17-19).
Asano, K.: 2007, EECRs from Gamma-Ray Bursts, Int. Symp.
on Astronomy and Astrophysics of Extreme Universe, (Tokyo,
Japan, Mar. 22-23).
Asano, K.: 2007, Fate of Accelerated Particles in Gamma-Ray
Bursts IRCS Int. Workshop on Shock Formation under
Extreme Environments in the Universe, (Tokyo, Japan, Feb.
20-22).
Asayama, S., Kawashima, S., Iwashita, H., Takahashi, T.,
Inata, M., Obuchi, Y., Suzuki, T., Wada, T.: 2007,
Progress and Status of the ALMA Band 4 Cartridge Receiver,
7th Workshop on Submm-Wave Receiver Technologies in
Eastern Asia, (Osaka, Japan, Jan 17-19).
Beck, T., McGregor, P., Takami, M.: 2006, Gemini NIFS
Integral Field Spectroscopy of YSO Environments: Spatially
Extended Molecular Hydrogen Emission in the Inner 200
AU, AAS/AAPT Joint Meeting, (Seattle, USA, Jan. 5-10).
Bowler, B. P., Waller, W. H., Megeath, S. T., Patten, B. M.,
Tamura, M.: 2007, A Search for Young Stellar Objects in
the Horsehead Nebula, AAS/AAPT Joint Meeting, (Seattle,
USA, Jan. 5-10).
Choi, Y. K., et al.: 2006, Maser Observation in VY CMa with
VERA, 8th EVN Symp. 2006, Exploring the Universe with thereal-time VLBI, (Torun, Poland, Sept. 26-29).
Deguchi, S., Fujii, T., Ita, Y., Izumiura, H., Kameya, O.,
Miyazaki, A., Nakada, Y., Ideta, M.: 2006, Dynamics of Stars
in the Inner Galactic Bulge revealed from SiO Maser
Surveys, Mapping the Galaxy and Nearby Galaxies, (Ishigaki
Island, Okinawa, Japan, June 26-30).
Egusa, F., Sofue, Y., Nakanishi, H.: 2006, Determination ofStar Formation Timescale and Pattern Speed of Spiral
Galaxies, IAU XXVIth General Assembly, (Pragua, Czech,
Aug. 14-25).
Endo, A.: 2006, Development of Nb/Al-AlN x/Nb SIS Tunnel
Junctions for Submillimeter-Wave Mixers, Applied
Superconductivity Conf. 2006, (Seattle, USA, Aug. 27-Sept.
1).
Endo, A.: 2007, Logarithmic Growth of AlNx Barriers in
Nb/Al-AlNx/Nb SIS Tunnel Junctions, 18th Int. Symp. on
Space Terahertz Technology, (Pasadena, California, USA,
Mar. 23).
Endo, A.: 2007, Novel Techniques for Controlling the RnA of
RF Plasma Nitridized AlN Barriers for SIS Tunnel Junctions,
7th Workshop on Submm-Wave Receiver Technologies in
Eastern Asia, (Osaka, Japan, Jan 17-19).
Enoki, M., Nakata, F.: 2006, New features of Subaru
Telescope Science Archive System, SMOKA, Astronomical
Data Analysis Software & Systems XVI, (Tucson, USA, Oct.
15-18).
Fujimoto, M.-K.: 2006, Status of the TAMA300 Detector, 11th
Marcel Grossmann Meeting, (Berlin, Germany, July 23-29).
Furusho, R., Chang, M.-S., Ikeda, Y., Kasuga, T., Kinoshita, D.

文献英文 08.3.2 10:34 AM ページ67

Lin, H.-C., Sato, Y., Ip, W.-H., Kawakita, H., Lin, Z.-Y.,
Watanabe, J.: 2006, Imaging Polarimetry of 9P/Tempel for
the Deep Imapct Event, AOGS 3rd Annual Meeting,(Singapore, Singapore, July 10-14).
Furusho, R., Kawakita, H., Ikeda, Y., Kasuga, T., Sato, Y.,
Watanabe, J.: 2006, Early Results of Polarimetric Imager for
Comets (PICO), AOGS 3rd Annual Meeting, (Singapore,
Singapore, July 10-14).
Goossens, S., Matsumoto, K., Namiki, N., Hanada, H., Iwata,T., Tsuruta, S., Kawano, N., Saski, S.: 2006, Global Lunar
Gravity Field Determination Using Historical and Recent
Tracking Data in Preparation for SELENE, 2006 American
Geophysical Union Fall Meeting, (San Francisco, USA, Dec.
11-15).
Goossens, S., Matsumoto, K.: 2006, Lunar Satellite Orbit
Determination Analysis and Quality Assessment from Lunar
Prospector Tracking Data and SELENE Simulations, 36th
COSPAR Scientific Assembly, (Beijing, China, July 16-23).
Goossens, S., Matsumoto, K., Kikuchi, F., Sasaki, S., Ping,J.: 2006, Incorporating SMART-1 Tracking Data into Lunar
Gravity Field Determination, EPSC #1, European Planetary
Science Congress, (Berlin, Germany, Sept. 18-22).
Gouda, N., JASMINE Working Group: 2006, Infrared
Astrometric Saetllite JASMINE, IAU 26th GA: Commision 8
Buisiness Meeting & Science Sessions, (Prague, Czech, Aug.
21).
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T., JASMINE
Working Group: 2006, JASMINE-Position Reconstruction,
36th COSPAR Scientific Assembly, (Beijing, China, July 1623).
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T., Tsujimoto,T., Suganuma, M., Niwa, Y., Yamauchi, M., Kawakatsu,
Y., Matsuhara, H., Noda, A., Tsuiki, A., Utashima, M.,
Ogawa, A.: 2006, JASMINE: Galactic Structure Surveyor,
SPIE, Space Telescopes and Instrumentation Ⅰ :Optical,
Infrared, and Millimeter, (Orlando, USA, May 24-31).
Gouda, N., Kobayashi, Y., Yamada, Y., Yano, T., Tsujimoto,T., Suganuma, M., Niwa, Y., Yamauchi, M., Kawakatsu,
Y., Matsuhara, H., Noda, A., Tsuiki, A., Utashima, M.,
Ogawa, A., Sako, N.: 2006, JASMINE-Astrometric Map of
the Galactic Bulge, IAU 26th General Assembly, JointDiscussion 13, Exploiting large surveys for Galactic
Astronomy, (Prague, Czech, Aug. 22-23).
Guyon, O., Angel, J. R., Bowers, C., Burge, J., Burrows, A.,
Codona, J., Greene, T., Iye, M., Kasting, J., Martin, H.,
McCarthy, D. W., Meadows, V., Meyer, M., Pluzhnik, E. A.,
Sleep, N., Spears, T., Tamura, M., Tenerelli, D., Vanderbei,
R., Woodgate, B., Woodruff, R. A., Woolf, N. J.: 2007,
Telescope to Observe Planetary Systems (TOPS): A High
Efficiency Coronagraphic 1.2-m Visible Telescope,
AAS/AAPT Joint Meeting, (Seattle, USA, Jan. 5-10).
Noda, H., Heki, K., Hanada, H.: 2006, In-situ Lunar
Orientation Measurement (ILOM): Simulation of
Observation, 36th COSPAR Scientific Assembly, (Beijing,
China, July 16-23).
Hamana, T.: 2006, Sciences with Hyper Suprime-Cam,
Cosmology with wide-field photometric and spectroscopic
galaxy surveys, (Tokyo, Japan, Nov. 9-10).
Hanada, H., Iwata, T., Kawano, N., Namiki, N., Asari, K.,

Ishikawa, T., Kikuchi, F., Liu, Q., Matsumoto, K., Noda,
H., Tsuruta, S., Goossens, S., Iwadate, K., Kameya, O.,
Tamura, Y., Hong, X., Ping, J., Aili, Y., Ellingsen, S.,
Schlueter, W.: 2006, VRAD (differential VLBI RADio
Sources) Used for Gravimetry in SELENE, 36th COSPAR
Scientific Assembly, (Beijing, China, July 16-23).
Hanada, H., Iwata, T., Kawano, N., Namiki, N., Asari, K.,
Ishikawa, T., Kikuchi, F., Liu, Q., Matsumoto, K., Noda,
H., Tsuruta, S., Goossens, S., Iwadate, K., Kameya, O.,
Tamura, Y., Hong, X., Ping, J., Aili, Y., Ellingsen, S., andSchlueter, W.: 2006, Present Status of Differential VLBI
Experiments in SELENE Mission, 8th ILEWG Conf.,(Beijing, China, July 23-27).
Hanada, H., VRAD group: 2007, Present Status of VRAD, 1st
SELENE SWTM, (Tsukuba, Japan, Jan. 9-11).
Hanaoka, Y.: 2006, A New Magnetograph System for theObservation of the Three-Dimensional Vector Magnetic Fieldof the Sun, 36th COSPAR Scientific Assembly, (Beijing,
China, July 16-23).
Hanaoka, Y.: 2006, Simultaneous Full-Stokes Imaging
Polarimetry Observations in Fe I 6303 and H, IAU GA2006
JD03 Solar Active Regions and 3D Magnetic Structure,(Prague, Czech, Aug. 16-17).
Hara, H.: 2006, Hinode X-ray Telescope and EUV Imaging
Spectrometer, CAWSES Int. Workshop on Space Weather
Modeling, (Yokohama, Japan, Nov. 14-17).
Hara, H.: 2006, Hinode: A New Solar Observatory in Space,
16th Int. Toki Conf., (Gifu, Japan, Dec. 5-8).
Hara, H.: 2007, First Results from Hinode Mission, The
CAWSES workshop: Comparative Study of Solar Flares andMagnetospheric Substorms as a Basis of Space Weather
Research, (Fairbanks, USA, Mar. 18).
Harada, Y.: 2006, True Polar Wander Due to Surface Mass
Loading on Mars: Effect of Polar Tide on Rotational
Stability, 2006 American Geophysical Union Fall Meeting,(San Francisco, USA, Dec. 11-15).
Harada, Y., Heki, K.: 2006, Secular Obliquity Variations Due
to Climate Friction on Mars: Re-Examination in Influence ofMartian Internal Viscosity Structure, European Geosciences
Union General Assembly 2006, (Vienna, Austria, Apr. 2-7).
Harada, Y., Heki, K.: 2006, Secular Obliquity Variations Due
to Climate Friction on Mars: Re-Examination in Influence ofMartian Internal Viscosity Structure, AOGS 3rd Annual
Meeting, (Singapore, Singapore, July 10-14).
Harada, Y., Kurita, K.: 2006, The Effect of the NonSynchronous Rotation on the Surface Stress of Europa:
Constraints for the Rotation Period and the Surface Viscosity,
European Geosciences Union General Assembly 2006,(Vienna, Austria, Apr. 2-7).
Harada, Y., Kurita, K.: 2006, The Effect of the NonSynchronous Rotation on the Surface Stress of Europa:
Constraints for the Rotation Period and the Surface Viscosity,
AOGS 3rd Annual Meeting, (Singapore, Singapore, July 1014).
Hasegawa, T.: 2006, ASTE Observations of the Massive Star
Forming Region SgrB2: A Giant Impact Scenario, Science
with ALMA: a new era for Astrophysics, (Madrid, Spain,
Nov. 13-17).
Hashimoto, T., Iye, M., Aoki, K.: 2006, Investigation of67

文献英文 08.3.2 10:34 AM ページ68

Ionization Mechanism of Extended Narrow Line Region, IAU
26th General Assembly, (Prague, Czech, Aug. 14-25).
Hatsukade, B., Kohno, K., Endo, A., Tosaki, T., Ohta, K.,
Kawai, N., Cortes, J., Nakanishi, K., Okuda, T., Muraoka,
K., Vreeswijk, P., Ezawa, H., Yamaguchi, N., Sakamoto,S., Sakai, T., Kawabe, R.: 2006, A Search for Molecular
Gas toward the Host Galaxy of GRB 980425, Mapping the
Galaxy and Nearby Galaxies, (Ishigaki Island, Okinawa,
Japan, June 26-30).
Hatsukade, B., Kohno, K., Endo, A., Tosaki, T., Ohta, K.,
Kawai, N., Cortes, J., Nakanishi, K., Okuda, T., Muraoka,
K., Vreeswijk, P., Ezawa, H., Yamaguchi, N., Sakamoto,S., Sakai, T., Kawabe, R.: 2006, A Possible Detection of
CO(J=3-2) Emission from the Host Galaxy of GRB 090425
with Atacam Submillimeter Telescope Experiment, Galaxy
Evolution across the Hubble Time, IAU Symp. 235, (Prague,
Czech, Aug. 13-20).
Hayakawa, T., Iwamoto, N., Shizuma, T., Kajino, T., Umeda,
H., Nomoto, K.: 2006, Universality of the p Process, Int.
Symp. on Nuclei in Cosmos IX, (CERN, Genève, Switzerland,
June 25-30).
Hayakawa, T., Shizuma, T., Kajino, T., Ogawa, K., andNakada, S.: 2006, Cosmic Clock and Thermometer for
Neutrino Process, Int. Symp. on Nuclei in Cosmos IX,,(CERN, Genève, Switzerland, June 25-30).
Hayakawa, T., Shizuma, T., Kajino, T., Ogawa, K., andNakada, S.: 2007, Cosmic Clock for Neutrino-Induced
Reaction Nucleosynthesis, 21st Century COE 6th Symp. on
Neutrino Processes and Stellar Evolution, (Tokyo, Japan,
Feb. 7-9).
Higuchi, A.: 2006, Evolution of the Oort Cloud andDistribution of New Comets Due to the Galactic Tide, IAU
Symp. 236, (Prague, Czech, Aug. 14-25).
Hiramatsu, M., Kamegai, K., Hayakawa, T., Tatematsu, K.,
Ohnishi, T., Mizuno, A., Hasegawa, T.: 2006, ASTE
Submillimeter Observations of a YSO Condensation in
Cederbald 110, Triggered Star Formation in a Turbulent
ISM, IAU Symp. 237, (Prague, Czech, Aug. 13-20).
Hirota, A., Kuno, N., Sato, N., Tosaki, T., Nakanishi, H.,
Sorai, K.: 2006, GMCs in the Nearby Galaxy IC 342,
Mapping the Galaxy and Nearby Galaxies, (Ishigaki Island,
Okinawa, Japan, June 26-30).
Hirota, T.: 2006, EA Winter School on Radio Astronomy, East
Asia Millimeter-VLBI Science Workshop, (Nanjing, China,
May 22-23).
Hirota, T.: 2006, Molecules in Space, Sokendai Asian WinterSchool, Frontiers in Molecular Science: Electronic andStructural Properties of Molecules and Nano Materials,(Okazaki, Japan, Nov. 20-22).
Hirota, T.: 2006, Observations of H 2O Maser Sources in
Nearby Molecular Clouds with VERA, East Asia MillimeterVLBI Science Workshop, (Nanjing, China, May 22-23).
Hirota, T.: 2006, Parallax Measurements of Nearby Star
Forming Regions, 2006 Korea-Japan VLBI meeting, (Ulsan,
Korea, Nov. 21-22).
Hirota, T.: 2007, Proposal Writing and Observation Planning,
Sokendai Asian Winter School, (Mitaka, Japan, Jan. 22-26).
Hirota, T. et al.: 2006, Observations of H2O Maser Sources in
Nearby Molecular Clouds with VERA, Mapping the Galaxy

68

and Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June
26-30).
Hirota, T. et al.: 2007, Observations of H2O Maser Sources in
Nearby Molecular Clouds with VERA, IAU Symp. 242,
Astrophysical masers and their environments, (Alice Springs,
Australia, Mar. 12-16).
Honma, M.: 2006, Maser Astrometry with VERA and EastAsian Array, East Asia Millimeter-VLBI Science Workshop,(Nanjing, China, May 22-23).
Honma, M.: 2006, Science Review of VERA Project, 2006
Korea-Japan VLBI meeting, (Ulsan, Korea, Nov. 21-22).
Honma, M.: 2006, VERA Observation of S269, 2006 KoreaJapan VLBI meeting, (Ulsan, Korea, Nov. 21-22).
Honma, M., et al.: 2006, Parallax measurements of water maser
sources beyond 5 kpc with VERA, 8th EVN Symp. 2006,
Exploring the Universe with the real-time VLBI, (Torun,
Poland, Sept. 26-29).
Honma, M., et al.: 2006, VERA Project, Mapping the Galaxy
and Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June
26-30).
Honma, M., et al.: 2007, Galactic Rotation Measurements
Based on H2O Maser Astrometry with VERA, IAU Symp.
242, Astrophysical masers and their environments, (Alice
Springs, Australia, Mar. 12-16).
Hori, K., NAOJ NOGIS team: 2006, Coronal Transient
Activities Observed with Norikura Green-Line Imaging
System "NOGIS", CAWSES Int. Workshop on Space Weather
Modeling, (Yokohama, Japan, Nov. 14-17).
Hori, K., Pohjolainen, S., Sakurai, T.: 2006, Radio and Hard
X-Ray Quasi-Periodic Pulsations during the 2004 July 13
Flare, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).
Hori, K., Pohjolainen, S., Sakurai, T.: 2007, Radio and Hard
X-ray Observations of Quasi-Periodic-Pulsations during the2004 July 13 Flare, 2007 Spring Meeting for the Korea-Japan
Collaborative Research on the Solar Activity, (Seoul, Korea,
Feb. 8-9).
Hori, K.: 2007, Coronal Transient Activities Observed with
Norikura Green-line Imaging System "NOGIS",CAWSES/IHY workshop, (Nagoya, Japan, Mar. 14-16).
Horii, S., Koyama, T., Tanigawa, Y., Terasawa, T., Yoshikawa,I., Yoshida, H., Watanabe, J.: 2006, Observations of
Meteors at Multiple Stations by Radio Waves Using GPS,AOGS 3rd Annual Meeting, (Singapore, Singapore, July 1014).
Hosokawa, T., Inutsuka, S.: 2006, Dynamical Formation of
the Dark Molecular Hydrogen Clouds around Diffuse HIIRegions, The 2nd East-Asia Numerical Astrophysics Meeting,(Daejeon, Korea, Nov. 1-3).
Ichimoto, K.: 2006, Solar Optical Telescope onboard HINODE
for Diagnosing the Solar Magnetic Fields, 16th Int. Toki
Conf., (Gifu, Japan, Dec. 5-8).
Ichimoto, K.: 2006, Three-Dimensional Magnetic Structures ofSolar Photosphere and Chromosphere, 16th Int. Toki Conf.,(Gifu, Japan, Dec. 5-8).
Imanishi, M.: 2006, AGNs in nearby ULIRGs Revealed
through Subaru 3-4 micron and Spitzer 5-35 micron
Combined Spectroscopy, Studying Galaxy Evolution with
Spitzer and Herschel, (Agios Nikolaos, Greece, May 28-June文献英文 08.3.2 10:34 AM ページ69

2).
Imanishi, M.: 2006, An Infrared Observational Discovery of
the Luminosity Correlation between AGNs and Nuclear
Starbursts in Dusty Tori -its Implications for an AGN Fueling
Mechanism, Mapping the Galaxy and Nearby Galaxies,(Ishigaki Island, Okinawa, Japan, June 26-30).
Imanishi, M.: 2006, Buried AGNs in Distant ULIRGs, SPICA
U.S. workshop, (Pasadena, California, USA, Nov. 1-3).
Imanishi, M.: 2006, Buried AGNs in nearby ULIRGs Revealed
through Subaru 3-4 micron and Spitzer 5-35 micron
Combined Spectroscopy, Dust and gas in ULIRGs: Tracing
Star Formation and Black Hole Growth at the Centers of
Ultraluminous Infrared Galaxies, (Ithaca, USA, June 19-22).
Imanishi, M.: 2006, Luminous Buried AGNs in the Local
Universe, The Central Engine of Active Galactic Nuclei,(Xian, China, Oct. 16-21).
Imanishi, M.: 2006, Millimeter Interferometric Follow-up of
Infrared-Selected Buried AGN Candidates, Studying Galaxy
Evolution with Spitzer and Herschel, (Agios Nikolaos,
Greece, May 28-June 2).
Imanishi, M.: 2006, Millimeter Interferometric Follow-up of
IR-Selected Buried AGN Candidates, Dust and gas in
ULIRGs: Tracing Star Formation and Black Hole Growth at
the Centers of Ultraluminous Infrared Galaxies, (Ithaca,
USA, June 19-22).
Imanishi, M.: 2006, Nuclear Starbursts in the Dusty Tori of
Seyfert 1 and 2 Galaxies, The Central Engine of Active
Galactic Nuclei, (Xian, China, Oct. 16-21).
Imanishi, M.: 2006, XDR Signatures in Nearby ULIRGs, The
Central Engine of Active Galactic Nuclei, (Xian, China, Oct.
16-21).
Inoue, M., et al.: 2006, Possible Detection of Faraday Screen,
The Central Engine of Active Galactic Nuclei, (Xian, China,
Oct. 16-21).
Inoue, M., et al.: 2006, Possible Detection of Outer Plasmaaround AGN Jets, Mapping the Galaxy and Nearby Galaxies,(Ishigaki Island, Okinawa, Japan, June 26-30).
Inoue, M., et al.: 2006, The Next-Generation Space VLBI
Project: VSOP-2, The Central Engine of Active Galactic
Nuclei, (Xian, China, Oct. 16-21).
Inoue, S.: 2006, Probing the Cosmic Dark Ages with the
Broadband Emission of Very High-z GRBs, SWIFT and
GRBs: Unveiling the Relativistic Universe, (Venezia, Italy,
June 5-9).
Inoue, S.: 2007, Cosmic Ray Acceleration and High Energy
Emission due to Cosmological Structure Formation Shocks,
IRCS Int. Workshop on Shock Formation under Extreme
Environments in the Universe, (Tokyo, Japan, Feb. 20-22).
Inoue, S.: 2007, Particle Acceleration and High Energy
Emission by Clusters of Galaxies, Astro Particle CPV in
Topical Physics, (Yongpyong, Korea, Feb. 21-24).
Inoue, S.: 2006, Gamma-rays and UHE Cosmic Rays from
Clusters of Galaxies, The Multi-Messenger Approach to HighEnergy Gamma-ray Sources, (Barcelona, Spain, July 4-7).
Inoue, S.: 2006, Hard X-rays and Gamma-rays from UltraHigh-Energy Processes in Clusters of Galaxies, The Extreme
Universe in the Suzaku Era, (Kyoto, Japan, Dec. 4-8).
Inoue, S.: 2006, High Energy Radiation and Cosmic Rays from
Clusters of Galaxies, 4th Korean Astrophysics Workshop on

Origin, Propagation and Interaction of Energetic Particles,(Daejeon, Korea, May 17-19).
Inoue, S.: 2007, Astrophysical Origin of Extremely HighEnergy Cosmic Rays, Astronomy and Astrophysics of theExtreme Universe, (Tokyo, Japan, Mar. 22-23).
Inoue, S.: 2007, Origin of Ultra High Energy Cosmic Rays,
Astro Particle CPV in Topical Physics, (Yongpyong, Korea,
Feb. 21-24).
Inuzuka, S.: 2006, Dynamics of Multi-Phase Interstellar
Medium, The 2nd East-Asia Numerical Astrophysics
Meeting, (Daejeon, Korea, Nov. 1-3).
Inuzuka, S.: 2006, The Role of Magnetic Fields in Planet
Formation, The Third Workshop on Development of Extrasolar Planetary Science, (Tokyo, Japan, Dec. 11-13).
Inuzuka, S.: 2007, Collapse and Outflow in Star Formation,
Supernovae Conf. 2007, (Tokyo, Japan, Feb. 1-3).
Ishitsuka, J. K., Ishitsuka, M., Inoue, M., Kaifu, N., Miyama,S., Tsuboi, M., Ohishi, M., Fujisawa, K., Kasuga, T.,
Kondo, T., Horiuchi, S., Umemoto, T., Miyoshi, M.,
Miyazawa, K., Bushimata, T., Vidal, E. D.: 2006, A New
Astronomical Facility for Peru: Converting a
Telecommunication's 32 Meter Parabolic Antenna into aRadio Telescope, Int. Astronomical Union XXVIth General
Assembly, (Prague, Czech, Aug. 14-25).
Ito, H., Kino, M., Kawakatu, N., Isobe, N., Yamada, S.: 2006,
Large Kinetic Power in FRII Radio Jets, The 5th StromloSymp.: Disks, Winds & Jets - From Planets to Quasars,(Canberra, Australia, Dec. 4-8).
Ito, T., Malhotra, R.: 2006, Dynamical Transport of Asteroid
Fragments from the nu6 Resonance, The 2nd East-Asia
Numerical Astrophysics Meeting, (Daejeon, Korea, Nov. 1-3).
Iwata, I.: 2006, Luminosity Dependent Evolution of Lyman
Break Galaxies from redshift 5 to 3, IAU Symp. 235, Galaxies
Across the Hubble Time, (Prague, Czech, Aug. 14-17).
Iwata, T., Minamino, H., Namiki, N., Hanada, H., Kawano,N., Takano, T.: 2006, Development of SELENE Small SubSatellites for Lunar Gravity Observation, 36th COSPAR
Scientific Assembly, (Beijing, China, July 16-23).
Iwata, T., Minamino, H., Namiki, N., Hanada, H., Kawano,N., Takano, T.: 2006, Development of SELENE Small SubSatellites for Lunar Gravity Observation, 8th ILEWG Conf.,(Beijing, China, July 23-27).
Iwata, T., Minamino, H., Satoh, H., Sasaki, T., Namiki, N.,
Hanada, H.: 2007, Development of SELENE Small SubSatellites: Rstar and Vstar and Their Applications for
Selenodesy, SELENE SWTM, (Tsukuba, Japan, Jan. 9-11).
Iwata, T., Namiki, N., Hanada, H., Minamino, H., Takano, T.,
Kawano, N., Matsumoto, K., Sasaki, S.: 2007, SELENE
Small Sub-Satellites for Lunar Gravity Observation, 38th
Lunar and Planetary Science Conf., (Houston, TX, USA,
Mar. 12-16).
Iye, M.: 2006, Japan's Optical/Infrared Astronomy Plan, IAU
26th General Assembly, (Prague, Czech, Aug. 14-25).
Iye, M., Ota, K., Kashikawa, N.: 2006, Discovery of a Galaxy
at Redshift 6.96 and Its Implications on Galaxy Formation
Era, AAS/AAPT Joint Meeting, (Seattle, USA, Jan. 5-10).
Kadono, T., Sugita, S., Ootsubo, T., Sako, S., Miyata, T.,
Kawakita, H., Furusho, R., Honada, M., Watanabe, J.: 2006,
Time and Spatial Distributions of Dust Ejected by Deep69

文献英文 08.3.2 10:34 AM ページ70

Impact Collision with Comet 9P/Tempel 1, AOGS 3rd Annual
Meeting, (Singapore, Singapore, July 10-14).
Kajino, T.: 2006, Explosive Nucleosynthesis in the Big-Bangand Supernovae: New Determination Method of ν Oscillation Parameters and Mass Hierarchy, Mitchell Symp.,(TX, USA, Apr. 10-14).
Kajino, T.: 2006, Neutrino and Weak Processes in Astronuclear
Physics, The 2nd Int. Symp. On Neutrinos and Dark Matter in
Nuclear Physics, (Paris, France, Sept. 3-9).
Kajino, T.: 2006, Supernova Neutrino Nucleosynthesis, Int.
Neutrino Oscillation Workshop, (Conca Specchiulla, Italy,
Sept. 9-16).
Kajino, T.: 2006, Supernova Neutrinos and New CosmologicalModel without Dark Energy, Int. Symp. on Cosmology andParticle Astrophysics, (Taipei, Taiwan, Nov. 15-17).
Kajino, T.: 2006, UHE Neutrinos and Nucleosynthesis in
Collapsar as Evidence for GRB Central Engines, 2nd Int.
Workshop On TeV Particle Astrophysics, (Wisconsin, USA,
Aug. 28-31).
Kajino, T.: 2007, Neutrino Oscillation in Supernova and GRBCollapsar Nucleosynthesis, 21st Century COE 6th Symp. on
Neutrino Processes and Stellar Evolution, (Tokyo, Japan,
Feb. 7-9).
Kamegai, K., Hiramatsu, M, Hayakawa, T., Tatematsu, K.,
Hasegawa, T., Onishi, T., Mizuno, A.: 2006, Submillimeterwave Observations of Outflow and Envelop around the Low
Mass Protpstar IRAS 13036-7644, Triggered Star Formation
in a Turbulent ISM, IAU Symp. 237, (Prague, Czech, Aug. 1320).
Kameya, O.: 2006, VLBI Observations of NGC7538 Region,
East Asia Millimeter-VLBI Science Workshop, (Nanjing,
China, May 22-23).
Kameya, O., et al.: 2006, H 2O Maser Distributions in the
NGC7538 Morecular Cloud Core, Mapping the Galaxy and
Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June 2630).
Kameya, O., et al.: 2006, Water Masers in NGC7538 Region,
8th EVN Symp. 2006, Exploring the Universe with the realtime VLBI, (Torun, Poland, Sept. 26-29).
Kamio, S.: 2006, dBz/dz Derivation by Artificial Neural
Network, The 2nd ambiguity resolution workshop, (Boulder,
CO, USA, Oct. 4).
Kamikura, M., Shan, W., Tomimura, Y., Sekimoto, Y.,
Asayama, S.-I., Satou, N., Iizuka, Y., Ito, T., Kamba, T.,
Serizawa Y., Noguchi, T.: 2006, A 385-500 GHz 2SB SIS
Mixer Based on a Waveguide Split-Block Coupler, Int. Space
Science and Teraherz Technology, (Paris, France, May 1113).
Kamohara, R.: 2006, Registration Map of two SiO Maser
Transitions with VERA, 2006 Korea-Japan VLBI meeting,(Ulsan, Korea, Nov. 21-22).
Kamohara, R., et al.: 2007, VLBI Phase-Referencing
Observation of SiO Masers toward R Aqr, IAU Symp. 242,
Astrophysical masers and their environments, (Alice Springs,
Australia, Mar. 12-16).
Kano, R.: 2006, Multiplicity of Solar X-Ray Corona in Timeand Space, 16th Int. Toki Conf., (Gifu, Japan, Dec. 5-8).
Kanzawa, T., et al.: 2006, Improvement of the Pointing
Accuracy of the Subaru Telescope by Suppressing Vibrations,

70

SPIE 6267, Ground-based and Airborne Telescopes,(Orlando, USA, May 24-31).
Karr, J., Puravankara, M., Tamura, M., Kudo, T., Ohashi, N.:
2007, Coronographic Observations of Circumstellar Disks
with Subaru, AAS/AAPT Joint Meeting, (Seattle, USA, Jan. 510).
Kashikawa, N.: 2006, The End of the Reionization Epoch
Probed by Ly Emitters at z=6.5, The Universe at z > 6, 26th
meeting of the IAU, Joint Discussion 7, JD07, #13, (Prague,
Czech, Aug. 17-18).
Kashikawa, N.: 2006, The End of the Reionization Epoch
Probed by Ly Emitters at z=6.5, At the Edge of the Universe- Latest results from the deepest astronomical surveys -,(Sintra, Portugal, Oct. 9-13).
Kasuga, T.: 2006, Metal Compositions of Meteoroids in
Meteor Showers, AOGS 3rd Annual Meeting, (Singapore,
Singapore, July 10-14).
Kasuga, T., Watanabe, J., Sato, M.: 2006, Mission to 3200
Phaethon, AOGS 3rd Annual Meeting, (Singapore, Singapore,
July 10-14).
Kasuga, T., Watanabe, J., Sato, M.: 2006, Direct Impact
Mission to (3200) Phaethon: Artificial Meteor Shower of theOnce Active Comet, 36th COSPAR Scientific Assembly,(Beijing, China, July 16-23).
Kato, T.: 2006, Mitaka - An Interactive 3D Viewer of the
Hierarchical Structure of the Universe, 18th Int. Planetarium
Society Conf., (Melbourne, Australia, July 23-27).
Katsukawa, Y.: 2006, First Light of Solar Optical Telescope(SOT) on Hinode, CAWSES Int. Workshop on Space Weather
Modeling, (Yokohama, Japan, Nov. 14-17).
Kawagoe, S.: 2006, Neutrino Signal of Supernova Shock Wave
Propagation: MSW Distortion of the Spectra andNucleosynthesis, Int. Symp. on Nuclei in Cosmos IX,, (CERN,
Genève, Switzerland, June 25-30).
Kawagoe, S.: 2007, Neutrino Oscillations and Supernova
Shock Wave, 21st Century COE 6th Symp. on Neutrino
Processes and Stellar Evolution, (Tokyo, Japan, Feb. 7-9).
Kawagoe, S.: 2007, Neutrino Signal of Supernova-Shock
Propagation: A clue to Study Unknown Neutrino Oscillation
Parameters, Twenty Years after SN1987A, (Hilton Waikoloa,
Hawaii, USA, Feb. 23-25).
Kawagoe, S., Suzuki, H., Sumiyoshi, K., Yamada, H., Kajino,
T.: 2006, Neutrino Signal of Supernova Shock Wave
Propagation: MSW Distortion of the Spectra andNucleosynthesis, Int. Symp. on Nuclei in Cosmos IX, (CERN,
Genève, Switzerland, June 25-30).
Kawaguchi, N.: 2006, e-VLBI in Japan, 2006 Korea-JapanVLBI meeting, (Ulsan, Korea, Nov. 21-22).
Kawaguchi, N.: 2006, Japanese Optical eVLBI Network using
GALAXY/GEMnet2, JGN2 and Super SINET, GemNet2
Nagasaki Symp., (Nagasaki, Japan, June 1).
Kawaguchi, N.: 2007, Correlation, Phase-Tracking System,
Spectroscopy, Digital Signal Processing, Sokendai Asian
Winter School, (Mitaka, Japan, Jan. 22-26).
Kawakatu, N., Andreani, P., Granato, G. L., Danese, L.: 2006,
Detectability of Massive Tori in Proto-QSOs with ALMA,
Mapping the Galaxy and Nearby Galaxies, (Ishigaki Island,
Okinawa, Japan, June 26-30).
Kawakatu, N., Andreani, P., Granato, G. L., Danese, L.: 2006,

文献英文 08.3.2 10:34 AM ページ71

Detectability of Massive Tori in Proto-QSOs with ALMA,The 4-th ALMA Science Meeting, (Mitaka, Japan, July 27-28).
Kawakatu, N., Kino, M.: 2006, Dyanamical Evolution ofPowerful Radio-Loud AGNs, Korea-Japan Young
Astronomers Meeting 2006, (Gyeonju, Korea, Aug. 21-23).
Kawakatu, N., Kino, M, Ito, H.: 2006, Dynamical Evolution of
Hot Spots in Radio Loud AGNs, The Central Engine of
Active Galactic Nuclei, (Xian, China, Oct. 16-21).
Kawakatu, N., Kino, M, Ito, H.: 2006, MeV Gamma Emission
Coccons of Young Radio Galaxies, High Energy
Astrophysics in the Next Decade–NeXT and future mission,(Tokyo, Japan, June 21-23).
Kawakita, H., Furusho, R., Ishiguro, M., Watanabe, J.: 2006,
Sensitive Search for Monodeuterio Methane in Comet C/2004
Q2, AOGS 3rd Annual Meeting, (Singapore, Singapore, July
10-14).
Kawamura, S., et al. including Arai, K., Aso, Y., Fujimoto,M., Fukushima, M., Ohishi, N., Sato, S., Takahashi, R.,
Takahashi, R., Yamazaki, T.: 2006, The Japanese Space
Gravitational Wave Antenna - DECIGO, Gravitational Wave
Advanced Detector Workshop 2006, (Elba, Italy, May 27June 1).
Kawano, N.: 2006, Activities in Japan on Astronomy from theMoon, IAU General Assembbly, (Prague, Czech, Aug. 14-25).
Kawazoe, F.: 2006, Current Status of the 4m RSE,
Gravitational Wave Advanced Detector Workshop 2006,(Elba, Italy, May 27-June 1).
Kawazoe, F., Volker, L., Sato, S., Morioka, T., Nishizawa, A.,
Yamazaki, T., Fukushima, M., Kawamura, S., Sugamoto,A.: 2007, Experimental Investigation of a Control Scheme fora Tuned Resonant Sideband Extraction Interferometer for
Next-Generation Gravitational-Wave Detectors, Rencontres
de Mirond, (Italy, Mar. 1).
Kikuchi, F., Liu, Q., Matsumoto, K., Hanada H., Kawano,N., Iwata, T.: 2007, Orbit Determination of Lunar Orbiter
SMART-1 by Using DORR and Doppler, 1st SELENE
SWTM, (Tsukuba, Japan, Jan. 9-11).
Kimura, K., Uchio, Y., Ogawa, Y., Agata, H., Mikami, H., etal.: 2006, The Future View of the Science Education in Japan- Workshop Focused on Science Communication for the
Association of Pfomoting the Science Education for the 21stCentury (APSE21), The 9th Int. Conf. on Public
Communication of Science & Technology, (Seoul, Korea,
May 17-19).
Kinoshita, D., Lin, H.-C., Otsuka, K., Sekiguchi, T.,
Watanabe, J., Ito, T., Arakida, H., Kasuga, T., Miyasaka,S.: 2006, Photometric Observations of 2005 UD at Lulin
Observatory, AOGS 3rd Annual Meeting, (Singapore,
Singapore, July 10-14).
Kiuchi, H.: 2006, High-Extinction Ratio LiNbO3 Intensity
Modulator Applied to the Radio Interferometer, AP-mwp
2006 (2006 Asia-Pacific microwave photonic Conf.), (Kobe,
Japan, Apr. 24-26).
Kobayashi, C.: 2006, Simulations of Cosmic Chemical
Enrichment with Hypernova, CRAL Conf.: Chemodynamics
from first stars to local galaxies, (Lyon, France, July 10-14).
Kobayashi, C.: 2006, Simulations of Cosmic Chemical
Enrichment: Hypernova Feedback, Galactic Winds, and
Mass-Metallicity Relations, IAU General Assembly, S235,(Prague, Czech, Aug. 16).
Kobayashi, H.: 2006, Current Status of VERA Project, East
Asia Millimeter-VLBI Science Workshop, (Nanjing, China,
May 22-23).
Kobayashi, H.: 2006, Status of VERA Project, 2006 KoreaJapan VLBI meeting, (Ulsan, Korea, Nov. 21-22).
Kobayashi, H.: 2007, Radio Telescopes/Interferometers inAsia, Sokendai Asian Winter School, (Mitaka, Japan, Jan. 2226).
Kobayashi, H., et al.: 2007, East Asian VLBI Network, IAU
Symp. 242, Astrophysical masers and their environments,(Alice Springs, Australia, Mar. 12-16).
Kobayashi, Y., Gouda, G., Tsujimoto, T., Yano, T.,
Suganuma, M., Yamauchi, M., Takato, N., Miyazaki, S.,
Yamada, Y., Sako, N., Nakasuka, S.: 2006, A Very Small
Astrometry Satellite Mission: Nano-JASMINE, IAU 26th
General Assembly, Joint-Discussion 13, Exploiting large surveys for Galactic astronomy, (Prague, Czech, Aug. 22-23).
Kobayashi, Y., Gouda, N., Tsujimoto, T., Yano, T.,
Suganuma, M., Yamauchi, M., Takato, N., Miyazaki, S.,
Yamada, Y., Sako, N., Nakasuka, S.: 2006, Nano-JASMINE:
A 10-kilogram Satellite for Space Astrometry, SPIE, Space
Telescopes and Instrumentation Ⅰ: Optical, Infrared, andMillimeter, (Orlando, USA, May 24-31).
Kobayashi, Y., Gouda, N., Yano, T., Suganuma, M.,
Yamauchi, M., Yamada, Y.: 2006, Nano-JASMINE: A 10kilogram Satellite For Space Astrometry, 36th COSPAR
Scientific Assembly, (Beijing, China, July 16-23).
Kodama, T.: 2006, Galaxy Evolution Viewed as Functions ofEnvironment and Mass, Mapping the Galaxy and Nearby
Galaxies, (Ishigaki Island, Okinawa, Japan, June 26-30).
Kodama, T.: 2006, Proto-Clusters with Evolved Populations
around Radio Galaxies at 2<z<3, Cosmic Frontiers, (Durham,
UK, July 31-Aug. 4).
Kodama, T.: 2007, Panoramic Views of Cluster Evolution
since z=3: Build-up of the Red Sequence of Galaxies, A New
Zeal for Old Galaxies, (Rotorua, New Zealand, Mar. 25-30).
Kodama, T., Tanaka, M., Kajisawa, M., Koyama, Y., Nakata,F., Hoshi, T.: 2006, Panoramic Views of Cluster Evolution
since z=3, Galaxy Evolution Across the Hubble Time, IAU
Symp. 235, (Prague, Czech, Aug. 14-17).
Kohjiro, S., Shi, S.-C., Inatani, J., Maezawa, M., Uzawa, Y.,
Wang, Z., Shoji, A.: 2007, An Octave Bandwidth SIS Mixer
for Compact Spectrometers, 7th Workshop on Submm-Wave
Receiver Technologies in Eastern Asia, (Osaka, Japan, Jan
17-19).
Kohno, K., Muraoka, K., Nakanishi, K., Tosaki, T., Kuno, N.,
Miura, R., Sawada, T., Sorai, K., Okuda, T., Kamegai, K.,
Tanaka, K., Endo, A., Hatsukade, B., Ezawa, H.,
Sakamoto, S., Cortes, J. R., Yamaguchi, N., Matsuo, H.,
Kawabe, R.: 2006, ASTE Observations of Dense Molecular
Gas in Galaxies, Triggered Star Formation in a Turbulent
ISM, IAU Symp. 237, (Prague, Czech, Aug. 13-20).
Kojiro, S., Inatani, J., Shi, S.-C., Maezawa, M., Shoji, A.,
Uzawa, Y., Wang, Z., Nagatsuma. T., Ito, H.: 2006, WideRF-Band SIS Mixers for Accurate and Compact Terahertz
Spectrometer, Applied Superconductivity Conf. 2006,(Seattle, USA, Aug. 27-Sept. 1).
Kokeyama, K., Ward, R., Chen, Y., Sato, S., Fukushima, M.,71文献英文 08.3.2 10:34 AM ページ72

Kawamura, S., Sugamoto, A.: 2006, Cancelation of
Displacement Noise Using a Mach-Zehnder Interferometer,
Gravitational Wave Advanced Detector Workshop 2006,(Elba, Italy, May 27-June 1).
Kokubo, E.: 2006, Formation of the Comet Cloud by the
Galactic Tide, Mapping the Galaxy and Nearby Galaxies,(Ishigaki Island, Okinawa, Japan, June 26-30).
Kokubo, E.: 2006, 4-Dimensional Digital Universe Project,
18th Int. Planetarium Society Conf., (Melbourne, Australia,
July 23-27).
Komugi, S., Sofue, Y., Kohno, K., Nakanishi, H., Onodera, S.,
Egusa, F., Tosaki, T., Muraoka, K., Young, J.: 2006,
CO(J=1-0) and CO(J=3-2) Survey of Nearby Galactic
Centers: The Schmidt Law as a Function of Galactic
Properties, Int. Astronomical Union XXVIth General
Assembly, (Prague, Czech, Aug. 14-25).
Komugi, S., Sofue, Y., Kohno, K., Nakanishi, H., Onodera, S.,
Egusa, F., Tosaki, T., Muraoka, K., Young, J.: 2006,
CO(J=1-0) and CO(J=3-2) Survey of Nearby Glactic Centers:
The Schmidt Law as a Function of Galactic Properties,
Triggered Star Formation in a Turbulent ISM, IAU Symp.
237, (Prague, Czech, Aug. 13-20).
Koryukin, V., Shitov. S. V., Bukovski, M. A., Uvarov, A. V.,
Uzawa, Y., Noguchi, T., Wang, Z., Kroug. M.: 2007,
Balanced Waveguide Mixer for ALMA Band 10: HFSS
Simulation, 7th Workshop on Submm-Wave ReceiverTechnologies in Eastern Asia, (Osaka, Japan, Jan 17-19).
Kotake, K.: 2006, Gravitational Radiation from Core-Collapse
Supernovae, invited seminar, (Swiss, Apr. 20).
Kotake, K.: 2007, Multidimensional Modeling of CoreCollapse Supernovae: the Neutrino Heating Mechanism and
Besides, 21st Century COE 6th Symp. on Neutrino Processes
and Stellar Evolution, (Tokyo, Japan, Feb. 7-9).
Kotake, K.: 2006, Aspherical Core-Collapse Supernovae, Onemillenium after SN1006, (Hangzhou, China, May 16-23).
Kudoh, T.: 2006, Application of CIP-Based MHD Code in
Astrophysics, 2006 Asia-Pacific Microwave Conf., Workshop
WS8, (Yokohama, Japan, Dec. 12).
Kuno, N., Sato, N., Nakanishi, H., Hirota, A., Tosaki, T.,
Shioya, Y., Sorai, K., Nakai, N., Nishiyama, K., Vila-Vilaro,B.: 2006, Distribution of Molecular Gas in Barred Spiral
Galaxies, Int. Astronomical Union XXVIth General Assembly,(Prague, Czech, Aug. 14-25).
Kuno, N., Sato, N., Nakanishi, H., Hirota, A., Tosaki, T.,
Shioya, Y., Sorai, K., Nakai, N., Nishiyama, K., Vila-Vilaro,B.: 2006, Nobeyama CO Atlas of Nearby Spiral Galaxies,
Mapping the Galaxy and Nearby Galaxies, (Ishigaki Island,
Okinawa, Japan, June 26-30).
Kurayama, T.: 2006, Data Analysis System, 2006 KoreaJapan VLBI meeting, (Ulsan, Korea, Nov. 21-22).
Kurayama, T.: 2006, Period-Luminosity Relation of Nearby
Mira Variables, 2006 Korea-Japan VLBI meeting, (Ulsan,
Korea, Nov. 21-22).
Kurayama, T., et al.: 2006, Parallax measurements of theMira-Type Star UX Cygni with Phase-Referencing VLBI, 8th
EVN Symp. 2006, Exploring the Universe with the real-time
VLBI, (Torun, Poland, Sept. 26-29).
Kurita, K., Harada, Y.: 2006, Effect of Non-Synchronous
Rotation on Surface Stress of Europa: Constraint for Surface

72

Rheology, 2006 American Geophysical Union Fall Meeting,(San Francisco, USA, Dec. 11-15).
Kusakabe, M., Kajino, T., Mathews, G. J.: 2006, Can
Radiative Decay of Long-Lived Particles after the BBN Solve
Cosmological Li6 Problem?, Int. Symp. on Nuclei in Cosmos
IX, (CERN, Genève, Switzerland, June 25-30).
Kusakabe, N., Tamura, M., Kandori, R., Hashimoto, J.,
Nakajima, Y., Nagayama, T., Nagashima, C., Nagata, T.,
Hough, J. H.: 2007, Wide-Field NIR Polarimetry of the Orion
Nebula, AAS/AAPT Joint Meeting, (Seattle, USA, Jan. 5-10).
Liu, Q., Kikuchi, F., Matsumoto, K., Hanada, H., Asari, K.,
Tsuruta, K., Sander, G., Ping, J., Kawano, N.: 2007, SameBeam Differential VLBI Technique Using Two Satellites of
SELENE, SELENE SWTM, (Tsukuba, Japan, Jan. 9-11).
Liu, Q., Matsumoto, K., Kikuchi, F., Asari, K., Tsuruta, S.,
Ping, J., Hanada, H., Kawano, N.: 2006, Same-BeamDifferential VLBI Technique Using Two Satellites of
SELENE, 36th COSPAR Scientific Assembly, (Beijing,
China, July 16-23).
Liu, Q., Matsumoto, K., Kikuchi, F., Ping, J., Asari, K.,
Hanada, H., Kawano, N.: 2006, Same-Beam Differential
VLBI Technique Using Two Satellites of SELENE, 25th Int.
Symp. on Speace Technology and Science, (Kanazawa, Japan,
June 4-11).
Ly, C., Malkan, M., Kashikawa, N., Shimasaku, K., Doi, M.,
Nagao, T., Iye, M., Kodama, T., Morokuma, T., Motohara,
K.: 2006, The Luminosity Function and Star Formation Rate
Between Redshifts of 0.07 and 1.47 for Narrow-band
Emitters in the Subaru Deep Field, American Astronomical
Society 208th meeting, (City of Calgary, Canada, June 4-8).
Machida, M., Matsumoto, R.: 2006, Global MHD Simulationsof State Transitions and QPOs in Black Hole Accretion
Flows, MIT Workshop on Magnetized Accretion Disks,(Massachusetts, USA, Oct. 19-20).
Machida, M., Matsumoto, R.: 2007, Global 3D MHD
Simulations of Accretion Disk Oscillation, US-JAPANWorkshop on Magnetic Reconnection 2007, (St. Michaels,
MD, USA, Mar. 29).
Machida, M., Matsumoto, R.: 2007, MHD Simulations ofBlack Hole Accretion Disk, Mini-workshop on QPOs,(Poland, Mar. 22).
Machida, M., Matsumoto, R., Nozawa, M., Takahashi, K.,
Fukui, Y., et al.: 2006, Magneto-Hydrodynamic Simulationsof the Formation of Loop Structures in our Galactic Center,
The 2nd East-Asia Numerical Astrophysics Meeting,(Daejeon, Korea, Nov. 1-3).
Makino, J.: 2006, Evolution of SMBH-SMBH and SMBHIMBH Binaries: Effect of Large Mass Ratio, Physics andAstrophysics of Supermassive Black-Holes, (Santa Fe, USA,
July 10-14).
Makino, J.: 2006, GRAPE-DR and its Programming
Environment, MODEST 6d, (Amsterdam, Netherlands, March
27-28).
Makino, J.: 2006, Next Generation GRAPE: GRAPE-DR, IAU
GA JD6, (Prague, Czech, Aug. 17).
Makino, J.: 2006, Special-Purpose Computing for Dense
Stellar Systems, IAU GA JD14, (Prague, Czech, Aug. 22).
Makino, J.: 2006, Symmetric Individual Timestep, MODEST
6d, (Amsterdam, Netherlands, March 27-28).

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Makino, J.: 2007, Virtual Galaxies, Japanese-French Frontiersof Science Symposium, (Kanagawa, Japan, Jan. 27-29).
Matsui, H., Habe, A., Saitoh, T. R.: 2006, Effects of aSupermassive Black Hole Binary on a Nuclear Gas Disk,
Galaxy Evolution Across the Hubble Time, Int. Astronomical
Union. Symp. no. 235, (Prague, Czech, Aug. 14-17).
Matsumoto, K, Shum, C. K., Han, S., Niwa, Y., Yi, Y., Wang,
Y., Braun, A.: 2006, A Southern Ocean Tide Model
Assimilating Multiple Altimeter Data and Comparison to
Tidal Observations by GRACE, Western Pacific Geophysics
Meeting, (Beijing, China, July 24-27).
Matsumoto, K., Hanada, H., Goossens, S., Tsuruta, S.,
Kawano, N., Namiki, N., Iwata, T., Rowlands, D.: 2006, A
simulation Study for Anticipated Accuracy of Lunar Gravity
Field Model by SELENE Tracking Data, 36th COSPAR
Scientific Assembly, (Beijing, China, July 16-23).
Matsuo, H.: 2006, Development of Superconducting Direct
Detectors and Related Technologies, The 3rd Int. Symp. on
Ultra-fast Phenomena & Terahertz Wave, (Nanjing, China,
Sept. 25-27).
Matsuo, H.: 2006, Direct Detection and Interferometer
Technologies in THz range, 17th Int. Symp. on Space
Terahertz Technology, (Paris, France, May 10-12).
Matsuo, H.: 2007, Wideband Imaging Techniques in Terahertz
Frequencies, 7th Workshop on Submm-Wave ReceiverTechnologies in Eastern Asia, (Osaka, Japan, Jan 17-19).
Matsuo, H., Mori, Y., Ezawa, H., Ariyoshi, S., Otani, C.:
2006, Submillimeter-wave Camera using SIS Photon
Detectors (Invited Keynote), The Joint 32nd Int. Conf. on
Infrared and Millimetre Waves and 15th Int. Conf. on
Terahertz Electronics (IRMMW-THz 2006), (Shanghai,
China, Sept. 18-22).
Matsuo, H., Nagata, H., Mori, Y., Kobayashi, J., Okaniwa,
T., Yamakura, T., Otani, C., Ariyoshi, S.: 2006, Performanceof SIS photon detectors for Superconductive Imaging
Submillimeter-Wave Camera (SISCAM), SPIE 6275
Millimeter and Submillimeter Detectors and Instrumentation
for Astronomy III, (Orlando, USA, May 29-31).
Matsuura, M.: 2006, Circum-Binary Disk in the Ppost AGB
Star OH 231.8+4.1, Evolution and chemistry of symbiotic
stars, binary post-AGB and related objects, (Wierzba,
Mazury Lakes, Poland, Aug. 28-30).
Matsuura, M.: 2006, Infrared molecular bands in AGB stars innearby galaxies, Why Galaxies Care About AGB stars: Their
importance as actors and problems, (Vienna, Austria, Apr. 711).
Matsuura, M.: 2006, Grand tour of evolved stars - fromasymptotic giant branch (AGB) stars to post-AGB stars andplanetary nebulae, The 4th ALMA Science Working Group
Meeting & The 2nd Japan-Taiwan ALMA Science Meeting,(Mitaka, Japan, July 27-28).
Mayama, S., Tamura, M., Hayashi, M., Ishii, M., Suto, H.,
Kudo, T.: 2006, SUBARU Near-Infrared Multi-Color Imagesof Class II Young Stellar Object, RNO91, Triggered Star
Formation in a Turbulent ISM - IAU Symp. 237, (Prague,
Czech, Aug. 14-18).
Miura, H., Agata, H., Kokubo, E., Hayashi, M., Kato, T.,
Takeda, T., Ninagawa, Y., Iwashita, Y., Ono, T., Kaifu,N., Miyama, S., Takahei, T., Nukatani, S., Tashiro, H.,

Okuno, H., Nakamura, T.: 2006, Introduction to the 4Dimensional Digital UniverseI, The 9th Int. Conf. on Public
Communication of Science & Technology, (Seoul, Korea,
May 17-19).
Miyashita, A., et al: 2006, Improvement of the Thermal
Environment around the Subaru Telescope Enclosure, SPIE
6267, Ground-based and Airborne Telescopes, (Orlando,
USA, May 24-31).
Miyazaki, A., Shen, Z.-Q., Miyoshi. M., Tsutsumi, T., Tsuboi,
M.: 2006, Flux varistions of Sagittarius A* at short millimeter wavelengths, 36th COSPAR Scientific Assembly, (Beijing,
China, July 16-23).
Miyoshi, M.: 2006, Short time variation of Sgr A*, Galactic
Center Workshop 2006, (Bonn, Germany, Apr. 18-22).
Miyoshi, M.: 2006, Beats and Rotation of the Accretion disk
Around Super massive Black Holes Sgr A*, Physics andAstrophysics of Supermassive Black Holes, (Santa Fe, New
Mexico, July 10-14).
Mori, Y., Okaniwa, T., Nakahashi, M., Ariyoshi, S., Otani, C.,
Sato, H., Matsuo, H.: 2006, Development ofSuperconductive Imaging Submillimeter-Wave Camera with
Nine Detector Elements (SISCAM-9), SPIE 6275 Millimeterand Submillimeter Detectors and Instrumentation for
Astronomy III, (Orlando, USA, May 29-31).
Mori, Y., Sekiguchi, T., Sugita, S., Matsunaga, N., Fukushi, H.,
Kaneyasu, N., Kawadu, T., Kandori, R., Nakajima, Y.,
Tamura, M.: 2006, A Month-Long Near-IR Photometry andImaging of Comet 9P/Tempel 1 with the IRSF Telescope inSouth Africa, Deep Impact as a World Observatory Event Synergies in Space, Time, and Wavelength, (Brussels,
Belgium, Aug. 7-10).
Mori, Y., Sekiguchi, T., Sugita, S., Matsunaga, N., Fukushi, H.,
Kaneyasu, N., Kawadu, T., Kandori, R., Nakajima, Y.,
Tamura, M.: 2006, Near-IR Monitoring Photometry of
Comet 9P/Tempel 1 in South Africa, AOGS 3rd Annual
Meeting, (Singapore, Singapore, July 10-14).
Morimoto, M. Y., Yamakawa, H.: 2006, Periodic Orbits in
Binary Asteroids Systems Utilizing Low Thrust Propulsion,
25th Int. Symp. on Speace Technology and Science,(Kanazawa, Japan, June 4-11).
Morimoto, M. Y., Yamakawa, H.: 2006, Station Keeping in a
Binary Asteroid System, 36th COSPAR Scientific Assembly,(Beijing, China, July 16-23).
Morimoto, M. Y., Yamakawa, H., Uesugi, K.: 2006, Stable
Periodic Orbits with Low Thrust Acceleration in the
Restricted Three Body Problem, 25th Int. Symp. on Speace
Technology and Science, (Kanazawa, Japan, June 4-11).
Motoyama, K., Umemoto, T., Shang, H.: 2006, Radiation
Driven Implosion Model for Star Formation Near an H II
Region, Int. Astronomical Union XXVIth General Assembly,(Prague, Czech, Aug. 14-25).
Müller, T. G., Sekiguchi, T., Kaasalainen, M., Abe, M.,
Hasegawa, S.: 2006, Itokawa: The Power Of Ground-Based
Mid-Infrared Observations, IAU Symp., (Prague, Czech, Aug.
14-18).
Muraoka, K, Kohno, K, Tosaki, T., Kuno, N., Nakanishi, K.,
Sorai, K., Sakamoto, S.: 2006, CO(3-2) Wide Area Imagingof M 83 with ASTE - Correlation between CO(3-2)/CO(1-0)
Ratios and Star Formation Efficiencies -, Mapping the Galaxy

73

文献英文 08.3.2 10:34 AM ページ74

and Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June
26-30).
Nagai, H.: 2006, Kinematic Aging and Spectral Aging inYoung Radio Galaxies, Mapping the Galaxy and Nearby
Galaxies, (Ishigaki Island, Okinawa, Japan, June 26-30).
Nagata, H., Kobayashi, J., Matsuo, H., Fujiwara, M.: 2006,
Progress on GaAs Cryogenic Readout Circuits for SISCAM,SPIE 6275 Millimeter and Submillimeter Detectors andInstrumentation for Astronomy III, (Orlando, USA, May 2931).
Nakajima, T., Kaiden, M., Korogi, J., Kimura, K., Yonekura,Y., Ogawa, H., Nishiura, S., Dobashi, K., Yoda, T., Handa,
T., Kohno, K., Morino, J., Asayama, S., Noguchi, T.: 2007,
New 60-cm Radio Survey Telescope with the SidebandSeparating SIS Receiver for the 200 GHz Band, 7thWorkshop on Submm-Wave Receiver Technologies in Eastern
Asia, (Osaka, Japan, Jan 17-19).
Nakamura, K.: 2007, Second-order Gauge Invariant
Cosmological Perturbation Theory: - Einstein Equations in
Terms of Gauge Invariant Variables -, The SixteenthWorkshop on General Relativity and Gravitation in Japan,(Niigata, Japan, Nov. 27 - Dec. 1).
Nakanishi, H., Sofue, Y.: 2006, Three-Dimensional HI and H2
Gas Maps of the Milky Way Galaxy Mapping the Galaxy and
Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June 2630).
Nakanishi, K., Sato, N., Kuno, N., Okumura, S. K., Kawabe,R., Kohno, K., Yamauchi, A., Nakai, N.: 2006, Radio
Continuum and Water Vapor Maser Monitoring toward the
Luminous Infrared Galaxy NGC 6240, Mapping the Galaxy
and Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June
26-30).
Nakata, F., Enoki, M.: 2006, Development of Quality
Assessment System for Subaru Data, Astronomical Data
Analysis Software & Systems XVI, (Tucson, USA, Oct. 1518).
Nakata, F., Kodama, T., Tanaka, M., PISCES team: 2007 The
Spectroscopic Study of Galaxies within the Structure around
Cl 0939+4713, A New Zeal for Old Galaxies, (Rotorua, New
Zealand, Mar. 25-30).
Namiki, N., Iwata, T., Matsumoto, K., Noda, H., Hanada, H.,
Tsuruta, S., Goossens, S., Asari, K., Kawano, N.,
Ishikawa, T., Kikuchi, F., Liu, Q., Sasaki, S., Ping, J.,
Ogawa, M., Fuke, F., Yahagi, Y., Masui, W.: 2007, Gravity
Experiment by Four-Way Doppler Measurement of SELENE
Mission, SELENE SWTM, (Tsukuba, Japan, Jan. 9-11).
Namiki, N., Matsumoto, K., Iwata, T., Noda, H., Hanada, H.,
Sasaki, S.: 2006, Scientific Outcomes Expected from Gravity
Experiments of Japanese SELENE Mission, 36th COSPAR
Scientific Assembly, (Beijing, China, July 16-23).
Namiki, N., Matsumoto, K., Iwata, T., Noda, H., Hanada, H.,
Kawano, N., Tsuruta, S., Sasaki, S.: 2006, Scientific
Outcomes Expected from Gravity Experiments of Japanese
SELENE Mission, 8th ILEWG Conf., (Beijing, China, July
23-27).
Nishikawa T., Takami M., et al.: 2006, SUBARU HighDispersion Spectroscopy of H and [NII] (6584Å) in the HL
Tau Jet, IAU Symp. 237, (Prague, Czech, Aug. 14-18).
Nishikawa, J.: 2006, Recent Coronagraph Experimental

74

Studies, TPF Coronagraph Workshop, (Pasadena, California,
USA, Sep. 28-29).
Nishikawa, J., Murakami, N., Abe, L., Kotani, T., Tamura,M., Yokochi, K., Kurokwa, T., Tavrov, A., Takeda, M.:
2006, Coronagraph Experiments with Dynamic Range
Absorption by Pre-Optics, The 4th Int. TPF/Darwin
Workshop, (Pasadena, California, USA, Nov. 8-10).
Nishiyama, S.: 2006, Structure of the Galactic Bulge: Is theMilky Way a Double-barred Galaxy?, Galactic Center
Workshop 2006, From The Center of the Milky Way to
Nearby Low-Luminosity Galactic Nuclei, (Bad Honnef,
Germany, Apr. 18-22).
Nishiyama, S.: 2006, Structure of the Galactic Bulge and Near
Infrared Interstellar Extinction Law, Mapping the Galaxy and
Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June 2630).
Nishizawa, A., Kawamura, S., Sakagami, M.: 2007, Quantum
Noise in Locked-type GW Interferometer and Signal
Recycling, LSC/VIRGO meeting, (Baton Rouge, Louisiana,
USA, Mar. 19-22).
Niwa, T., Itoh, Y., Tachihara, K., Oasa, Y., Sunada, K.,
Sugitani, K.: 2006, Radio Observation of Molecular Clouds
around the W5-East Triggered Star-Forming Region, IAU
26th General Assembly, (Prague, Czech, Aug. 14-25).
Niwa, Y., Arai, K., Sakagami, M., Gouda, N., Kobayashi, Y.,
Yamada, Y., Yano, T.: 2006, Laser Interferometric HighPrecision Angle Monitor for JASMINE, SPIE, Space
Telescopes and Instrumentation I: Optical, Infrared, andMillimeter, (Orlando, USA, May 24-31).
Noguchi, T.: 2006, Superconducting Mixers at Millimeter andSubmillimeter Wavelengths for ALMA, 19th Int. Symp. on
Superconductivity, (Nagoya, Japan, Oct. 30-Nov. 1).
Noguchi, T.: 2007, Status of SIS Device Development at
NAOJ, 7th Workshop on Submm-Wave ReceiverTechnologies in Eastern Asia, (Osaka, Japan, Jan 17-19).
Oh, C. S.: 2006, 22GHz VERA Survey, 2006 Korea-JapanVLBI meeting, (Ulsan, Korea, Nov. 21-22).
Ohta, I. S., Hattori, M., Takahashi, J., Chinone, Y., Luo, Y.,
Matsuo, H.: 2006, Astronomical mm and sub-mm
Observations with the Multi-Fourier TransformInterferometer in 2005 and 2006, SPIE 6275 Millimeter andSubmillimeter Detectors and Instrumentation for Astronomy
III, (Orlando, USA, May 29-31).
Oishi, M.: 2006, Building the International Virtual Observatory
Alliance (IVOA): Programmatic Challenges, COSPAR
General Assembly 2006, (Beijing, China, July 18).
Oishi, M.: 2006, International Virtual Observatory: A New,
Planet-wide Research Infrastructure for Astronomy, Korea
Science and Technology Infrastructure Conf., (Seoul, Korea,
Nov. 28).
Oishi, M.: 2006, Recent Progress in Building the Virtual
Observatories in the World, NAOC China-VO Seminar,(Beijing, China, July 19).
Oishi, M.: 2006, Recent Results on Small Carbon Molecules,
Carbon in Space, (Italy, May 23).
Oishi, M.: 2006, Virtual Observatory, IAU General Assembly
2006 Special Session 1, (Prague, Czech, Aug. 16).
Ojha, D. K., Tamura, M.: 2006, Luminosity Functions of YSO
Clusters in Sh-2 255, W3 Main and NGC 7538 Star Forming文献英文 08.3.2 10:34 AM ページ75

Regions, Triggered Star Formation in a Turbulent ISM - IAU
Symp. 237, (Prague, Czech, Aug. 14-18).
Oka, T., Nagai, M., Kamegai, K., Tanaka, K.: 2006, A Largescale CO J = 3-2 Survey of the Galactic Center, Galactic
Center Workshop 2006, From The Center of the Milky Way to
Nearby Low-Luminosity Galactic Nuclei, (Bad Honnef,
Germany, Apr. 18-22).
Okamoto, S., Arimoto, N., Yamada, Y., Onodera, M.: 2007,
The Stellar Populations and the Structual Properties of Ursa
Major I, A New Zeal for Old Galaxies, (Rotorua, New
Zealand, Mar. 25-30).
Okamoto, T.: 2006, Simulations of Coevolving Galaxies andSupermassive Black Holes, Mapping the Galaxy and Nearby
Galaxies, (Ishigaki Island, Okinawa, Japan, June 26-30).
Okoshi, K., Nagashima, M., Gouda, N.: 2006, Evolution ofDamped Lyman-alpha Galaxies From Hierarchical Structure
Formation Models, IAU GA: Symp. No.235 -Galaxy
Evolution Across the Hubble Time-, (Prague, Czech, Aug. 1417).
Omukai, K.: 2006, Star Formation in Low-Metallicity
Environments, IAU JD07 #34, (Prague, Czech, Aug. 17-18).
Ono, T., Agata, H., Watanabe, J., Fukushima, T.: 2006,
Outreach Activities of National Astronomical Observatory ofJapan (NAOJ), 25th Int. Symp. on Speace Technology and
Science, (Kanazawa, Japan, June 4-11).
Ono, T., Watanabe, J., Agata, H.: 2006, Outreach Activities
of National Astronomical Observatory of Japan, 25th Int.
Symp. on Speace Technology and Science, (Kanazawa, Japan,
June 4-11).
Onodera, M.: 2007, Star-Formation and Chemical Evolution of
Massive Star-Forming Galaxies at z~2, A New Zeal for Old
Galaxies, (Rotorua, New Zealand, Mar. 25-30).
Ootsubo, T., Watanabe, J., Honada, M., Sugita, S., Kawakita,
H., Kadono T., Furusho, R.: 2006, Mass Ratio of Crystalline
to Amorphous Silicates for the Ejecta Dust of Comet
9P/Tempel 1 Induced by Deep Impact, AOGS 3rd Annual
Meeting, (Singapore, Singapore, July 10-14).
Otsuka, M., Tajitsu, A., Tamura, S.: 2006, High Resolution
Spectroscopic Study of the Halo PNe: The Case of H 4-1,
IAU Symp. 234, Planetary Nebulae in our Galaxy and
Beyond, (Waikoloa Beach, Hawaii, USA, Apr. 3-7).
Ping, J., Yan, J., Matsumoto, K., CE-1 VLBI TEAM: 2006,
Possible Contribution to the Selenodesy by CE-1 lunar
Mission, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).
Ping, J., Wang, G., Jian, N., Shi, X., Yang, J., Hong, X., Qian,Z., Ye, S., CE-1 VLBI group, Hanada, H., Kawano, N.,
Matsumoto, K., Liu, Q., RISE/SELENE group, Mikhailov,
A.: 2006, To contribute S/C VLBI POD to Selenodesy from
Smart-1 to Chang'E-1 and SELENE-1, 8th ILEWG Conf.,(Beijing, China, July 23-27).
Pyo, T.-S.: 2006, Probing the Origin of the Winds/Jets from
YSOs, The 5th Stromlo Symp.: Disks, Winds & Jets - From
Planets to Quasars, (Canberra, Australia, Dec. 4-8).
Pyo, T.-S., Hayashi, M.: 2006, Three-Dimensional VelocitySpace Structure Of the L1551 IRS 5 Outflow in [Fe II]
Emission with Subarcsecond Resolution by Subaru, American
Astronomical Society Meeting 208, (Calgary, Canada).
Rich, R. M., Brown, T. M., Reitzel, D. B., Ferguson, H., Koch,

A., Smith, E., Guhathakurta, P., Kalirai, J., Renzini, A.,
Kimble, R., Sweigart, A., Gilbert, K., Chiba, M., Iye, M.,
Komiyama, Y., Tanaka, M.: 2006, Keck/Deimos
Spectroscopy of Distant M31 fields with Deep HST Imaging,
AAS/AAPT Joint Meeting, (Seattle, USA, Jan. 5-10).
Rodriguez, J. A. P.: 2006, Sources, Sinks and Migration
Patterns of Dark Veneers in the Northern Polar Deposits ofMars, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).
Saigo, K., Tomisaka, K.: 2006, Evolution of First Core in
Rotating Molecular Cores, IAU Symp. 237, Triggered Star
Formation in a Turbulent ISM, (Prague, Czech, Aug. 14-18).
Sakamoto, K.: 2006, Gas Dynamics and Structure of Galaxies,
Science with ALMA : a new era for Astrophysics, (Madrid,
Spain, Nov. 13-17).
Sakata, S., Volker, L., Numata, K., Kawamura, S., Sato, S.,
Nishizawa, A., Furusawa, A., Fukushima, M., Sugamoto,A.: 2006, Experimental Plan for Extraction of Ponderomotive
Squeezing, Gravitational Wave Advanced Detector Workshop
2006, (Elba, Italy, May 27-June 1).
Sakurai, T.: 2006, Observations of CME Source Regions byCoronal Emission Line Dopplergrams, UN/NASA Workshop
on Basic Space Science and IHY, (Balgalore, India).
Sakurai, T.: 2006, Outlook for Studies of Magnetic Fields with
Solar-B, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).
Sakurai, T.: 2006, Solar Magnetic Fields: From the Interior to
the Surface and Beyond, 36th COSPAR Scientific Assembly,(Beijing, China, July 16-23).
Sakurai, T.: 2007, Current Understanding of Coronal Heating,Int. Conf. on Challenges for Solar Cycle 24, (Ahmedabad,
India, Jan. 22-25).
Sasaki, S.: 2006, Albedo/Color Variations on Itokawa:
Difference of Space Weathering, 36th COSPAR Scientific
Assembly, (Beijing, China, July 16-23).
Sasaki, S.: 2006, Bright and Dark Regions on Itokawa:Evidence of Space Weathering, AOGS 3rd Annual Meeting,(Singapore, Singapore, July 10-14).
Sasaki, S.: 2006, Brightness/Color Variation of Itokawa: Space
Weathering and Mass Movement, Int. Science Symp. on
Sample Returns from Solar System Minor Bodies, the 2nd
Hayabusa Symp., (Tokyo, Japan, July 12-14).
Sasaki, S.: 2006, Brightness/Color Variation on Itokawa:Space Weathering and Seismic Shaking, Workshop on
Spacecraft Reconnaissance of Asteroid and Comet Interiors,(Santa Cruz, USA, Oct. 5-6).
Sasaki, S.: 2006, Itokawa is Heterogeneous in Albedo andColor: Space Weathering on Small Asteroids, AAS, DPS
meeting #38, (Pasadena, California, USA, Oct. 9-13).
Sasaki, S.: 2006, Japanese Mars Mission in the Future Space
Program, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).
Sasaki, S.: 2006, Origin of Surface Albedo/Color Variation on
Rubble-Pile Itokawa, 38th Lunar and Planetary Science
Conf., (Houston, TX, USA, Mar. 12-16).
Sasaki, S.: 2006, Rock Weathering on Small Asteroids: Space
Weathering Experiments and Close-Up Observation of
Itokawa, Int. Science Symp. on Sample Returns from Solar
System Minor Bodies, the 2nd Hayabusa Symp., (Tokyo,

75

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Japan, July 12-14).
Sasaki, S.: 2006, Space Weathering and Surface Gardening on
Mercury, AOGS 3rd Annual Meeting, (Singapore, Singapore,
July 10-14).
Sasaki, S.: 2006, Space Weathering: A Lesson from Itokawa,
36th COSPAR Scientific Assembly, (Beijing, China, July 1623).
Sasaki, S.: 2006, Brightness/Color Heterogeneity on Small
Asteroids: Space Weathering and Movement of Surface
Materials of Itokawa as Observed by Hayabusa, European
Planetary Science Congress 2006, (Berlin, Germany, Sept.
18-22).
Sasaki, T., et al.: 2006, A Collaborative Site Survey for
Astronomical Observations in West China (Tibet), SPIE
6267, Ground-based and Airborne Telescopes, (Orlando,
USA, May 24-31).
Sato, K.-H., et al.: 2006, Characteristics of Time
Synchronization Response of NTP Clients on MS-Windows
OS and Linux OS, Thirty-eighth Annual Precise Time andTime Interval (PTTI) Systems and Applications Meeting,(Virginia, USA, Dec. 4-7).
Sato, M., et al.: 2007, Absolute Proper Motions of Water
Masers in NGC 281 Measured with VERA, IAU Symp. 242,
Astrophysical masers and their environments, (Alice Springs,
Australia, Mar. 12-16).
Sato, M., Kasuga, T., Watanabe, J.: 2006, Elucidation of the
Phoenicids Outburst in 1956 by the Dust Trail Theory, AOGS
3rd Annual Meeting, (Singapore, Singapore, July 10-14).
Sato, S.: 2006, Diagonalizing Sensing Matrix of Broadband
RSE, Gravitational Wave Advanced Detector Workshop
2006, (Elba, Italy, May 27-June 1).
Sawada, T.: 2006, NRO/CSO/ASTE Galactic Plane CO
Survey, Mapping the Galaxy and Nearby Galaxies, (Ishigaki
Island, Okinawa, Japan, June 26-30).
Sawada, T., Koda, J., Handa, T., Sugimoto, M., Hasegawa, T.:2006, NRO/CSO/ASTE Galactic Plane CO Survey, Mapping
the Galaxy and Nearby Galaxies, (Ishigaki Island, Okinawa,
Japan, June 26-30).
Sekiguchi, T.: 2006, Thermal Continuum Observations of
TNOs and Debris Disks, Science with ALMA: a new era for
Astrophysics, (Madrid, Spain, Nov. 13-17).
Serizawa, Y., Sekimoto, Y., Ito, T., Shan, W. L., Ueda, A.,
Kamba, T., Satou, N., Kamikura, M.: 2006, A 385 - 500
GHz Balanced Mixer with a Waveguide Quadrature Hybrid
Coupler, Int. Space Science and Teraherz Technology, (Paris,
France, May 11-13).
Shan, W.-L., Shi, S.-C., Matsunaga, T., Endo, A., Noguchi, T.,
Uzawa, Y., Takizawa, M.: 2006, Design and Development of
SIS Mixers for ALMA Band 10, Applied Superconductivity
Conf. 2006, (Seattle, USA, Aug. 27-Sept. 1).
Shibasaki, K.: 2006, Microwave Measurements of Coronal
Magnetic Field, IAU 26th General Assembly, (Prague, Czech,
Aug. 14-25).
Shibasaki, K.: 2006, Multi-Wavelength Imaging of Solar
Plasma, 16th Int. Toki Conf., (Gifu, Japan, Dec. 5-8).
Shibata K. M.: 2006, Results of 3mm VLBI Experiments
Between Daeduke and Nobeyama, East Asia Millimeter-VLBI
Science Workshop, (Nanjing, China, May 22-23).
Shibata, K. M.: 2006, 43GHz VERA Survey, 2006 Korea-

76

Japan VLBI meeting, (Ulsan, Korea, Nov. 21-22).
Shimojo, M., Yokoyama, T., Asai, A., Nakajima, H.,
Shibasaki, K.: 2006, One Solar-Cycle Observations ofProminence Activities Using the Nobeyama Radioheliograph1992-2004, 36th COSPAR Scientific Assembly, (Beijing,
China, July 16-23).
Shin, J., Sakurai, T.: 2006, On the Imaging Characteristics of
Yohkoh Soft X-Ray Telescope, 36th COSPAR Scientific
Assembly, (Beijing, China, July 16-23).
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.,
Sakamoto, M.: 2006, Constructing the Subaru Advanced Data
and Analysis Service on VO, Astronomical Data Analysis
Software & Systems XVI, (Tucson, USA, Oct. 15-18).
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.,
Sakamoto, M.: 2006, Study on the Environment around QSOs
with redshift of 1~3 Using the JVO System, The Virtual
Observatory in Action: New Science, New Technology, andNext Generation Facilities, 26th meeting of the IAU, Special
Session 3, (Prague, Czech, Aug. 17-22).
Shirasaki, Y., Tanaka, M., Honda, S., Kawanomoto, S.,
Ohishi, M., Mizumoto, Y., Yasuda, N., Masunaga, Y.,
Ishihara, Y., Tsutsumi, J., Nakamoto, H., Kobayashi, Y.,
Sakamoto, M.: 2006, Japanese Virtual Observatory (JVO) as
an Advanced Astronomical Research Environment, SPIE
6267, (Orlando, USA, May 24-31).
Shitov, S. V., Koryukin, O. V., Uzawa, Y., Noguchi, T.,
Uvarov, A. V., Cohn, I. A.: 2006, Development of Balanced
SIS Mixers for ALMA Band-10, 17th Int. Symp. on Space
Terahertz Technology, (Paris, France, May 10-12).
Shitov, S. V., Koryukin, O. V., Uzawa, Y., Noguchi, T.,
Uvarov. A. V., Cohn, I. A., Bukovski, M. A.: 2006, Design ofBalanced Mixers for ALMA Band-10, Applied
Superconductivity Conf. 2006, (Seattle, USA, Aug. 27-Sept.
1).
Shitov, S. V., Uvarov, A. V., Koryukin, O. V., Bukovski, M.
A., Takeda, M., Wang, Z., Kroug, M., Uzawa, Y., Noguchi,
T.: 2007, Tolerance Analysis of THz-Range Lens-Antenna
and Balanced SIS Mixer, 18th Int. Symp. on Space Terahertz
Technology, (Caltech, CF, USA, Mar. 21-23).
Shum, C. K., Wang, Y., Yi, Y., Matsumoto, K., Niwa, Y., Han,G.: 2006, Coastal Ocean tide Modeling Circulation Studies
Using Multiple Satellite Altimetry, Western PacificGeophysics Meeting, (Beijing, China, July 24-27).
Sôma, M.: 2006, Abrupt changes in the Earth's rotation speed,
IAU 26th General Assembly, Joint-Discussion 13, Exploiting
large surveys for Galactic astronomy, (Prague, Czech, Aug.
21).
Sôma, M.: 2006, Japanese astronomical and meteorologicalarchives, IAU G.A., C41/ICHA Sessions Archives Working
Group Business Meeting, (Prague, Czech, Aug. 23).
Suematsu, Y.: 2006, Chromospheric Dynamics: Spicule fromHINODE to ATST, ATST Science Working Group Meeting,(Maui, Hawaii, USA, Oct. 17-19).
Suganuma, M., Kobayashi, Y., Gouda, N., Yano, T.,
Yamada, Y., Takato, N., Yamauchi, M.: 2006, Aluminum-文献英文 08.3.2 10:34 AM ページ77

made 5-cm Reflecting Telescope for Nano-JASMINE, SPIE,Space Telescopes and Instrumentation I: Optical, Infrared,
and Millimeter, (Orlando, USA, May 24-31).
Suganuma, M., Kobayashi, Y., Gouda, N., Yano, T.,
Yamada, Y., Takato, N., Yamauchi, M.: 2006, Developmentof a Very Small Telescope for Space Astrometry Surveyor,
IAU 26th General Assembly, Joint-Discussion 13, Exploiting
large surveys for Galactic astronomy, (Prague, Czech, Aug.
22-23).
Suganuma, M., Yoshii, Y., Kobayashi, Y., Minezaki, T.,
Enya, K, Tomita, H., Aoki, T., Koshida, S., Peterson, B. A.:
2006, Reverberation Measurements of the Inner Radius of theDust Torus in Nearby Seyfert 1 Galaxies, The Central Engineof Active Galactic Nuclei, (Xian, China, Oct. 16-21).
Sugita, S., Kadono, T., Sako, S., Ootsubo, T., Honda, M.,
Kawakita, H., Furusho, R., Watanabe, J.: 2007, Mid-IR
Observations of Deep Impact Reveal the Primordial Origin of
a Surface of Comet 9P/Tempe1 1, 38th Lunar and Planetary
Science Conf., (Houston, TX, USA, Mar. 12-16).
Sumiyoshi, K.: 2006, Core-Collapse Supernovae, Neutron Stars
and Black Holes in the Light of Physics of Unstable Nuclei,
The 6th China-Japan Joint Nuclear Physics Symp.,(Shanghai, China, Mar. 16-20).
Sumiyoshi, K.: 2006, Influence of Equation of State inSupernova Simulations:Neutrinos from Proto-Neutron Star
and Black Hole Formation, Yukawa Int. Seminar (YKIS06)
2006, New Frontiers in QCD - Exotic Hadrons and Hadronic
Matter -, (Kyoto, Japan, Dec. 4-8).
Sumiyoshi, K. : 2006, Influence of Nuclear Equation of State inCore-Collapse Supernovae, In Heaven and on Earth 2006,
The Nuclear Equation of State in Astrophysics, (Montreal,
Canada, July 5-7).
Sunada, K., Hongo, S., Ikeda, N., Kitamura, Y.: 2006, A Giant
Molecular Outflow Triggered the Formation of the High
Mass Dense Clumps in the NGC 7538 Region, Int.
Astronomical Union XXVIth General Assembly, (Prague,
Czech, Aug. 24-25).
Suzuki, I., Sakurai, T.: 2006, Relationship between the Massand the Acceleration of CMEs, 36th COSPAR Scientific
Assembly, (Beijing, China, July 16-23).
Suzuki, T., Chiba, S., Yoshida, T., Higashiyama, K., Honma,
M., Kajino, T., Otsuka, T.: 2006, Advances in Shell Model
Calculations and Neutrino-induced Reactions, Int. School of
Nuclear Physics on Radioactive Beams, Nuclear Dynamics
and Astrophysics, (Erice, Italy, Sept. 1-5).
Tajitsu, A., Otsuka, M.: 2006, High Dispersion Spectroscopyof the PN K 648 in the Globular Cluster M 15, IAU Symp.
234, Planetary Nebulae in our Galaxy and Beyond,(Waikoloa Beach, Hawaii, USA, Apr. 3-7).
Takahashi, S., Shimajiri, Y., Takakuwa, S., Saito, M.,
Kawabe, R.: 2006, Survey Observations of Large-Scale
Molecular Outflows Associated with Intermediate-Mass
Protostar Candidates in the OMC-2/3 Region, Triggered Star
Formation in a Turbulent ISM, IAU Symp. 237, (Prague,
Czech, Aug. 13-20).
Takato, N., Terada, H.: 2006, Near-Infrared Direct VisionPrism for Wide-Wavelength Coverage Spectroscopy at theSubaru Telescope, SPIE 6267, Ground-based and Airborne
Telescopes, (Orlando, USA, May 24-31).

Takato, N., Terada, H., Pyo, T.-S.: 2006, Crystalline Water
Ice on the Satellite of 2003 EL61, Trans Neptunian Objects
Dynamical and Physical properties, (Catania, Itally, July 27).
Takeda, M., Wang, Z., Uzawa, Y.: 2006, SIS Mixers Based on
NbN Techniques for ALMA Band 10, Applied
Superconductivity Conf. 2006, (Seattle, USA, Aug. 27-Sept.
1).
Takeda, M., Shoji, A., Saito, S., Shan, W., Uzawa, Y., Li, J.,
Shi, S.-C., Wang, Z.: 2007, Measurement of Complex
Dielectric Constant of MgO Substrate in the THz Region, 7thWorkshop on Submm-Wave Receiver Technologies in Eastern
Asia, (Osaka, Japan, Jan 17-19).
Takeda, T.: 2006, Visualizing Particle Simulation Data of
Astronomy, 18th Int. Planetarium Society Conf., (Melbourne,
Australia, July 23-27).
Takeda, Y.: 2006, Perspective for determining surface abundances and physical parameters of Metal-Rich Stars, The
Metal Rich Universe, (La Palma, Canary Island, Spain, June
12-16).
Tamura, M.: 2006, JTPF, TPF Coronagraph Workshop,(Pasadena, California, USA, Sep. 28-29).
Tamura, M.: 2006, JTPF and Planet finding, The 4th Int.
TPF/Darwin Workshop, (Pasadena, California, USA, Nov. 810).
Tamura, T.: 2007, Fabrication of Submicron SIS Junction
Using i-Line Stepper, 7th Workshop on Submm-Wave
Receiver Technologies in Eastern Asia, (Osaka, Japan, Jan
17-19).
Tamura, Y., Nakanishi, K., Kohno, K., Kawabe, R., Okuda,
T.: 2006, A New Submillimeter Diagnostics of Physical
Conditions of ISM in High Redshift Galaxies, Int.
Astronomical Union XXVIth General Assembly, (Prague,
Czech, Aug. 14-25).
Tanaka, K.: 2006, Detailed Distribution of Shocked Molecular
Gas in the l=1.3 deg Complex, Mapping the Galaxy and
Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June 2630).
Tanaka, M.: 2006, RDBMSs' Conformance to Atandard SQL,IVOA interoperability meeting, (Victoria, Canada, May 1419).
Tatsumi, D., the TAMA collaboration: 2006, Status of TAMA,
11th Gravitational Wave Data Analysis Workshop, (Potsdam,
Germany, Dec. 18-21).
Tavrov, A., Yokochi, K., Nsihikawa, J., Kurokawa, T.,
Takeda, M.: 2006, Recent Development of AchromaticInterfero-Coronagraph for Planet-Finder, TPF CoronagraphWorkshop, (Pasadena, California, USA, Sep. 28-29).
Tomisaka, K.: 2006, Contraction of Rotating Magnetized
Clouds and Outflows, Astronomy Dept. Colloquium, (Seoul,
Korea, Oct. 30).
Tomisaka, K., Saigo, K.: 2006, Fragmentation and Evolutionof the First Core, The 2nd East-Asia Numerical Astrophysics
Meeting, (Daejeon, Korea, Nov. 1-3).
Tomono, D.: 2007, Subaru Telescope before and after the
Earthquake, Mauna Kea observatories earthquake workshop,(Kailua-Kona, Hawaii, USA, Mar. 23).
Tosaki, T.: 2006, Dence Molecular Gas Formation Triggeredby Spiral Density Wave, Mapping the Galaxy and Nearby77文献英文 08.3.2 10:34 AM ページ78

Galaxies, (Ishigaki Island, Okinawa, Japan, June 26-30).
Tosaki, T.: 2006, Giant Molecular Association in Spiral Armsof M 31, Mapping the Galaxy and Nearby Galaxies, (Ishigaki
Island, Okinawa, Japan, June 26-30).
Tosaki, T., Shioya, Y., Kuno, N., Nakanishi, K., Hasegawa,T., Matsushita, S., Kohno, K., Miura, R., Tamura, Y.,
Okumura, S. K., Kawabe, R.: 2006, Dense Molecular Gas
Formation Triggered by Spiral Density Wave in M 31,
Triggered Star Formation in a Turbulent ISM, (Prague,
Czech, Aug. 14-18).
Tosaki, T., Shioya, Y., Kuno, N., Hasegwa, T., Nakanishi, K.,
Matsushita, S., Kohno, K.: 2006, Giant Molecular
Association in Spiral Arms of M 31: Evidence for Dense Gas
Formation Via Spiral Shock Associated with Density
Waves?, Mapping the Galaxy and Nearby Galaxies, (Ishigaki
Island, Okinawa, Japan, June 26-30).
Totani, T., Kawai, N., Kosugi, G., Aoki, K., Yamada, T., Iye,
M., Ohta, K., Hattori, T.: 2006, Implications for the Cosmic
Reionization from the Optical Afterglow Spectrum of theGamma-Ray Burst 050904 at z = 6.3, IAU 26th General
Assembly, (Prague, Czech, Aug. 14-25).
Tsuboi, M., Miyazaki, A., Handa, T.: 2006, The Synchrotron
Cut-off Frequency of Relativistic Electrons I the Radio Arc
and Their Acceleration Area, Mapping the Galaxy and
Nearby Galaxies, (Ishigaki Island, Okinawa, Japan, June 2630).
Tsuboi, M., Okumura, S. K., Miyazaki, A.: 2006, Interaction
between SNR Sagittarius A East and 50-km s-1 Molecular
Cloud, Galactic Center Workshop 2006: From the Center ofthe Milky Way to Nearby Low-Luminosity Galactic Nuclei,(Bad Honnef, Germany, Apr. 18-22).
Tsujimoto, T.: 2006, The Origin of the Double Main-Sequencein Omega Centauri, Deconstructing the Local Group, (Aspen,
USA, June 11-July 2).
Tsujimoto, T., Kobayashi, N., Ikeda, Y., Kondo, S., Yasui, C.,
Minami, A., Motohara, K., Gouda, N.: 2006, A Near-Infrared
High-Resolution Spectroscopic Survey of Bulge Stars - JASMINE Prestudy, IAU 26th General Assembly, JointDiscussion 13, Exploiting large surveys for Galactic astronomy, (Prague, Czech, Aug. 22-23).
Tsuneta, S.: 2006, Hinode: A New Solar Observatory in Space- Current Status -, CAWSES Int. Workshop on Space Weather
Modeling, (Yokohama, Japan, Nov. 14-17).
Tsuneta, S.: 2007, First Results from Hinode (Solar-B)
Mission, Int. Conf. on Chanllenges for Solar Cycle 24,(Ahmedabad, India, Jan. 22-25).
Umemoto, T., Mochizuki, N., Shibata, K. M., Roh, D.-G.,
Chung, H.-S.: 2007, Mm Wavelength Methanol Masers
Survey towards Massive Star Forming Regions, IAU Symp.
242, Astrophysical masers and their environments, (Alice
Springs, Australia, Mar. 12-16).
Uraguchi, F., et al.: 2006, The DIMM Station at Subaru
Telescope, SPIE 6267, Ground-based and Airborne
Telescopes, (Orlando, USA, May 24-31).
Ustinov, A. V., Batov, I. E., Jin, X. Y., Shitov, S. V., Koval, Y.,
Müller, P.: 2007, Detection of 0.5 THz Radiation from
Bi2Sr2CaCu2O8 Single Crystals, 18th Int. Symp. on Space
Terahertz Technology, (Caltech, CF, USA, Mar. 21-23).
Usuda, K. S.: 2006, Visualizing the Milky Way Galaxy - Disk

78

Model and Panoramic Model, Engaging the EPO
Community: Best Practices, New Approaches (Astronomical
Society of the Pacific, 118th Annual Meeting), (Baltimore,
Maryland, USA).
Usuda, T.: 2006, SUBARU Telescope: Current Performances& Future Upgrade Plans, SPIE 6267, Ground-based andAirborne Telescopes, (Orlando, USA, May 24-31).
Uzawa, Y.: 2007, Status of Band 10 Development, 7thWorkshop on Submm-Wave Receiver Technologies in Eastern
Asia, (Osaka, Japan, Jan 17-19).
Uzawa, Y., Sugimoto, M., Kimura, K., Nohara, R., Manabe, T.,
Ogawa, H., Fujii, Y., Shan, W.-L., Kaneko, K., Kroug, M.,
Shitov, S.: 2007, Near-Field Beam Measurements ofCorrugated Horns for ALMA band 10, 18th Int. Symp. on
Space Terahertz Technology, (Caltech, CF, USA, Mar. 2123).
Uzawa. Y., Wang, Z., Takeda, M., Kroug, M.: 2006,
Evaluation of Tunneling Barriers in Superconducting NbN
Junctions with Subharmonic Gap Structures, Applied
Superconductivity Conf. 2006, (Seattle, USA, Aug. 27-Sept.
1).
Wada, K.: 2006, Global SFR in Galactic Disks, The 2nd EastAsia Numerical Astrophysics Meeting, (Daejeon, Korea, Nov.
1-3).
Wada, K.: 2006, Modeling the ISM and Feedback - Toward
Numerical Milky Way, CRAL Conf.: Chemodynamics fromfirst stars to local galaxies, (Lyon, France, July 10-14).
Wada, K.: 2006, Numerical Modeling of the ISM in the
Galactic Center and Disks, Mapping the Galaxy and nearby
galaxies, (Ishigaki Island, Okinawa, Japan, June 26-30).
Wang, Y. P., Wang, Y. P., Yamada, T., Tanaka, I., Iye, M.:
2006, Subaru Deep Imaging of the Field of QSO 1508+5714
at z=4.28, IAU 26th General Assembly, (Prague, Czech, Aug.
14-25).
Wang, Z., Takeda, M., Terai, T., Uzawa, Y.: 2006, HighQuality NbN/AIN/NbN Tunnel Junctions Fabricated byReactive
dc-Magnetron
Sputtering,
AppliedSuperconductivity Conf. 2006, (Seattle, USA, Aug. 27-Sept.
1).
Wang, Z., Takeda, M., Uzawa, Y.: 2006, Development of lownoise SIS mixers with NbN technique for ALMA Band 10,
IRMMW-Thz 2006, (Shanghai, China, Sept. 18-22).
Watanabe, J.: 2006, Sendai Astronomical Observatory - Its
Renewal and History as an observatory for general public -,Innovation in Teaching/Learning Astronomy Methods, 26th
meeting of the IAU, Special Session 2, (Prague, Czech, Aug.
17-18).
Watanabe, J.: 2006, Star Week - A Successful Campaign inJapan -, Innovation in Teaching/Learning Astronomy
Methods, 26th meeting of the IAU, Special Session 2, (Prague,
Czech, Aug. 17-18).
Watanabe, J., Ootsubo, T., Honada, M., Sugita, S., Kawakita,
H., Kadono, T., Furusho, R.: 2006, Interpretation of the
Crystalline/Amorphous Silicates Ratio, AOGS 3rd Annual
Meeting, (Singapore, Singapore, July 10-14).
Watanabe, J., Sato, M., Kasuga, T.: 2006, Note on a New
Approach to Clarify Passed Cometary Activities of Parent
Objects of Meteor Showers, AOGS 3rd Annual Meeting,(Singapore, Singapore, July 10-14).

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Watanabe, T.: 2006, Solar and LHD Plasma Diagnostics, 5thInt. Conf. on Atomic and Molecular Data (ICAMDATA),(Meudon, France, Oct. 17).
Watanabe, T.: 2006, Emission Line Imaging Spectroscopy for
Diagnosing of Solar Outer Atmospheres, 16th Int. Toki Conf.,(Gifu, Japan, Dec. 5-8).
Yamada, M., Koyama, H., Omukai, K., Inutsuka, S.: 2006,
Synthetic Observations of Turbulent Flows in Diffuse
Multiphase Interstellar Medium, IAU Symp. 237, (Prague,
Czech, Aug. 14-18).
Yamada, Y., Arimoto, N., Vazdekis, A., Peletier, R. F.: 2006,
Stellar Population Study of Nearby Elliptical Galaxies, FineTuning Stellar Population Models, Lorentz Center (Leiden,
Neitherland).
Yamada, Y., Gouda, N., Yano, T., Kobayashi, Y., Sako, N.,
JASMINE WG: 2006, JASMINE - Data Analysis andSimulation -, 36th COSPAR Scientific Assembly, (Beijing,
China, July 16-23).
Yamada, Y., Gouda, N., Yano, T., Kobayashi, Y., Tsujimoto,T., Suganuma, M., Niwa, Y., Sako, N., Hatsutori, Y.,
Tanaka, T., JASMINE WG: 2006, JASMINE Simulator,
SPIE, Space Telescopes and Instrumentation Ⅰ : Optical,
Infrared, and Millimeter, (Orlando, USA, May 24-31).
Yamada, Y., Gouda, N., Yano, T., Sako, N., Hatsutori, Y.,
Tanaka, T., Yamauchi, Y., JASMINE WG: 2006, JASMINE
Simulator, 26th General Assembly, Joint-Discussion 13,
Exploiting large surveys for Galactic astronomy, (Prague,
Czech, Aug. 22-23).
Yamamoto, M., Toda, M., Higa, Y., Maeda, K., Watanabe, J.:
2006, Recent Development of Meteor Train Studies, AOGS
3rd Annual Meeting, (Singapore, Singapore, July 10-14).
Yamamoto, T., Sakurai, T.: 2006, Inflow Velocity andCoronal Magnetic Field Strength Estimated from the GOES
X-Ray Light Curve, IAU Symp. 233, Solar activity and its
magnetic origin, (Cairo, Egypt, Mar. 31-Apr. 4).
Yamamoto, T., Sakurai, T., Yokoyama, T., Kusano, K.: 2006,
Forecast of the Solar Flare Magnitude from the Photospheric
Magnetic Field Properties, AOGS 3rd Annual Meeting,(Singapore, Singapore, July 10-14).
Yamamoto, T., Sakurai, T., Yokoyama, T., Kusano, K.: 2006,
The Coronal Field Strength and the Magnetic Reconnection
Rate from the GOES X-ray Flux and the Photospheric
Magnetogram, AOGS 3rd Annual Meeting, (Singapore,
Singapore, July 10-14).
Yamamoto, T., Sakurai, T., Yokoyama, T., Kusano, K.,
Notoya, S., Inoue, S.: 2006, Helicity Injections in Various
Regions, 36th COSPAR Scientific Assembly, (Beijing, China,
July 16-23).
Yamazaki, D. G., Ichiki, K., Kajino, T., Mathews, G. J.: 2006,
Primordial Magnetic Field Constrained from CMB
Anisotropies, and its Generation and Evolution before, during
and after the BBN, Int. Symp. on Nuclei in Cosmos IX,(CERN, Genève, Switzerland, June 25-30).
Yamoto, F.: 2006, Two Evolutionary Paths of an Axisymmetric
Gravitational Instability in the Dust Layer of a Protoplanetary
Disk, From Dust to Planetesimals, (Munich, Germany, Sept.
11-15).
Yamoto, F.: 2006, Two Evolutionary Paths of an Axisymmetric
Gravitational Instability in the Dust Layer of a Protoplanetary

Disk, 38th Annual Meeting of the Division for Planetary
Sciences, (Pasadena, California, USA, Oct. 8-13).
Yan, J., Ping, J., Matsumoto, K., Fei, L.: 2006, The Simulationof Lunar Gravity Field Recovery from Delta-VLBI
Observation of Chang'E and SELENE Lunar Orbiters, 36th
COSPAR Scientific Assembly, (Beijing, China, July 16-23).
Yano, T., Gouda, N., Kobayashi, Y., Yamada, Y., JASMINE
Working Group: 2006, JASMINE Project - Instrument
Design and Centroiding Experiment -, 36th COSPAR
Scientific Assembly, (Beijing, China, July 16-23).
Yano, T., Araki, H., Gouda, N., Kobayashi, Y., Tsujimoto,T., Nakajima, T., Kawano, N., Tazawa, S., Yamada, Y.,
Hanada, H., Asari, K., Tsuruta, S.: 2006, CCD Centroiding
Experiment for JASMINE and ILOM, SPIE, Space
Telescopes and Instrumentation I: Optical, Infrared, andMillimeter, (Orlando, USA, May 24-31).
Yano, T., Gouda, N., Yamada, Y.: 2006, New Method for
Astrometric Measurements in Space Mission, JASMINE, IAU
26th General Assembly, Joint-Discussion 13, Exploiting large
surveys for Galactic astronomy, (Prague, Czech, Aug. 22-23).
Yoshida, H.: 2006, Integrability of 2D Homogeneous
Polynomial Potentials, Conf. on Singularities and Differential
Equations, (Tordesillas, Spain, Sept. 4-8).
Yoshida, H.: 2006, Toward a Complete List of Integrable
Potentials: Present Status, Int. Conf. on Chaos and Dynamical
Complexity, (Hsin-Chu, Taiwan, May 24-30).
Yoshida, T.: 2006, Supernova Mixtures Indicating Isotopic
Ratios of Presolar Grains, IAU 26th General Assembly, Joint
Discussion 11 on Pre-Solar Grains as Astrophysical Tools,(Pragu, Czech, Aug. 14-25).
Yoshida, T.: 2007, Light Element Synthesis in Supernovae with
Neutrino Oscillations, Neutrinos in Physics and Astrophysics,(Aspen, USA, Jan. 29-Feb. 3).
Yoshida, T.: 2007, Neutrino Nucleosynthesis with MSW
Effects in Core-Collapse Supernovae, 21st Century COE 6th
Symp. on Neutrino Process and Stellar Evolution, (Tokyo,
Japan, Feb. 7-9).
Yoshida, T., Kajino, T., Yokomakura, H., Kimura, K.,
Takamura, A., Hartmann, D. H.: 2006, Can supernova neutrino nucleosynthesis constrain neutrino oscillation parameters?,
Int. Symp. on Nuclei in Cosmos IX, (CERN, Genève,
Switzerland, June 25-30).

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