ISSN 1346-1192

ANNUAL REPORTOF THENATIONAL ASTRONOMICAL OBSERVATORY
OF JAPAN

Volume 4

Fiscal 2001

Explanation of the cover photograph: A spectrum of water-vapor maser emission from the nucleus of a
type 2 Seyfert galaxy, IC 2560 (optical photograph). In addition
to the known strong features around the systemic velocity (2876
km/s), weaker high-velocity features offset from the systematic
velocity up to ±420 km/s has been newly detected. Analysis has
shown that a super massive black hole sits at the nucleus from analyzing the data (2001; PASJ, 53, 215). The optical image is takenfrom Digitized Sky Survey (UK Schmidt).

Postscript
Editors Publications Commitee
TANIKAWA, Kiyotaka
HONMA, Mareki
IMANISHI, Masatoshi
KUNO, Nario
MURAMATSU, Toshiya
SEKII, TakashiSÔMA Mitsuru
YAMASHITA, Yoshiko
YASUDA, Naoki
Publisher National Astronomical Observatory of Japan
Osawa 2-21-1, Mitaka-shi, Tokyo 181-8588, Japan
TEL: +81-422-34-3600
FAX: +81-422-34-3690
http://www.nao.ac.jp/
Printer Kyoshin Co., Ltd.
1-20-19, Miyamae, Suginami-ku, Tokyo 168-0081, Japan
TEL: +81-3-3331-0950

Subaru IRCS view of binary brown dwarfs HD 130948B and HD 130948C.
With adaptive optics, IRCS delivers images and spectra with diffraction-limited resolution.
In this image, a close binary with a 0.13 arcsecond separation is clearly resolved.

Table of Contents
Preface

Norio KAIFU
Director General
National Astronomical Observatory of JapanⅠ Scientific Highlights April 2001 — March 2002 …………………………

1

Ⅱ Publications, Presentations ………………………………………………… 51
1 ．Refereed Publications …………………………………………………… 51
2 ．Publications of the National Astronomical Observatory of Japan ……… 60
3 ．Report of the National Astronomical Observatory of Japan …………… 60
4 ．Other Publications ……………………………………………………… 60
5 ．Presentations …………………………………………………………… 65

PREFACE
The NAOJ is promoting manifold fields of astronomy andastrophysics such as the optical/IR astronomy, radio astronomy, solar physics, theoretical astronomy/astrophysics, VLBI
astrometry/geodesy, gravitational wave detection by operating
top-level large facilities in each field. Among excellent institutes for astronomy and astrophysics in the world which are
specialized in the individual fields such as optical/IR, radio or
theory, the NAOJ is a unique institute for astronomy and astrophysics as a whole. The role of the NAOJ is also to provide
top-level facilities for university scientists and to represent theJapanese astronomy and astrophysics as an inter-university national research institute.
Under above characteristics and status the NAOJ has been developing new projects such as
the VERA, Subaru, TAMA-300 and ALMA to promote the research and education, and tried torespond to the strong public interest about the world we are living. Here I make a very brief review of our achievements during the financial year 2001, and the details are reported in the following text sections.
The Subaru Telescope, an 8.2m aperture optical/IR telescope has been in excellent condition through the open operation started last year. Five observing instruments among seven werealready opened for the operation. Remaining two instruments and adaptive optics system are to
be in operation from 2002. Refer to the highlight papers in the text for the scientific results fromthe Subaru Telescope.
The construction of a 20m antenna in Ishigaki Island, Okinawa was finished. This is the
4-th and final of dual-beam 20m antennas for the VERA project. The test observations with themax. 2300km baseline VLBI network (connecting the Mizusawa, Kagoshima, Chichi-Jima andIshigaki stations) to measure the distance to radio stars aiming to produce the three-dimensional
map of the whole Galaxy will start next year.
The gravitational wave detector TAMA-300, an advanced collaboration project with the
University of Tokyo and KEK, had succeeded in the long-term operation for the first time in theworld. The sensitivity was also in the highest level. The data reduction and further stabilizationof operation are in progress.
In the Nobeyama Radio Observatory the BEARS, a new 85-115 GHz 25-beam receiver for
the 45m telescope, has been operated with satisfactory performance through the year. The observations of molecular clouds have been made extensively by using the huge mapping capability of the BEARS. The RAINBOW, a combination of the 45m telescope and six 10m antennasof the NMA (Nobeyama Millimeter Array) has been operated successfully as one of the mostsensitive interferometer in the mm-wavelength region. The Nobeyama Radio Heliograph andthe solar magnetograph in Mitaka Campus have actively produced data which provided new understandings of the solar activity.
The progress worthy of special mention in 2002 was the promotion of the collaboration with
universities in radio astronomy. The Hokkaido University, Gifu University, Yamaguchi University and Kagoshima University have started the building-up of a new radio astronomy group by
using the 11m to 32m aperture antennas with VLBI capabilities under the close cooperation withNAOJ. Another remarkable activity was made in the field of public relation and education. The
Public Relation Center has successfully developed a number of excellent tasks like very popular
event “Your Four Days as an Astronomer” for high school students. Also various public activities were made in the local NAOJ facility areas including Hawaii and VERA sites, and the NAOJ
is now acting an important role in the science education for the public and students.
The most important ongoing project of the NAOJ is realization of the ALMA, which is aninternational large mm wave and sub-mm wave interferometer to be constructed in northern
Chile. Japanese participation to the ALMA, especially with its sub-mm wave technology andexperience, is essentially important to this epoch-making big project. The reorganization of allnational universities/institutes to be independent agencies aiming for operation from FY2004 is
another major subject for NAOJ. Intensive discussions are ongoing to create a flexible organization for powerful basic research.

Norio Kaifu
Director General
National Astronomical Observatory of JapanI

Scientific Highlights(2001 Apr. - 2002 Mar.)1 . Development of the Solar-B Spacecraft ………………………………………………………………… TSUNETA et al.
2 . Development of Solar-B Solar Optical Telescope …………………………………………………… SUEMATSU et al.
3 . Development of Image Stabilization System for
Solar Optical Telescope onboard Solar-B satellite…………………………………………………… NAGATA et al.
4 . Completion of VERA Ishigakijima Station ………………………………………………………………… MIYAJI et al.
5 . Interferometric Gravitational Wave Detector TAMA300:
1,000 hours Observation and Recycling Experiment……………………………………………… FUJIMOTO et al.
6 . Eleven-Year Solar Cycle Periodicity in Sky Brightness Observed at Mt. Norikura ………………………… SAKURAI
7 . Near Infrared Adaptive Optics Spectroscopy of Binary Brown Dwarf …………………………………… GOTO et al.
8 . Galaxy Number Counts in the Hubble Deep Field as a Strong Constraint
on a Hierarchical Galaxy Formation Model …………………………………………………… NAGASHIMA et al.
9 . Photoionization effect of the UV background on the colour-magnitude relationof elliptical galaxies …………………………………………………………………………… NAGASHIMA et al.
10. A Solution to the Missing Link in the Press-Schechter Formalism ……………………………………… NAGASHIMA
11. Spectropolarimetric Evidence of Asymmetric Outburst in the Fast Nova V1494 Aquilae …………… KAWABATA et al.
12. High-speed Hα camera for solar flare observations ………………………………………………… HANAOKA et al.
13. A Large-Scale CO Mapping of the Central Region of W51 ………………………………………… OKUMURA et al.
14. Near-Infrared Spectroscopy of the Compact HII Region W51 IRS 2 ………………………………… OKUMURA et al.
15. Acceptance and adaptation of octants and sextants in Japan during the 18th and 19th centuries …………NAKAMURA
NAKAMURA
16. Dense Plasma Torus around the Nucleus of NGC 1052 ………………………………………………… KAMENO et al.
17. Near-IR study of M16 (SIRIUS first light observations) ………………………………………………SUGITANI et al.
18. 2 Millimeter dust around NGC 7538-IRS 1, 2, and 3. I. Unfilled structure of dust ………………… AKABANE et al.
19. Buried AGNs in LINER type ultraluminous infrared galaxies …………………………………………IMANISHI et al.
20. A list of all integrable two-dimensional homogeneous polynomial potentials
with a polynomial integral of order at most four in the momenta ……………………………… NAKAGAWA et al.
21. Submillimeter Imaging Polarimetry of the NGC 7538 Region ………………………………………… MOMOSE et al.
22. The Spin Temperature of NH3 in Comet C/1999S4 (LINEAR) ……………………………………… KAWAKITA et al.
23. Wide-Field TV Observation of the Leonid Meteor Storm in 2001: Main Peak over Japan ………… WATANABE et al.
24. Optical Follow-up of the GRB 010222 Afterglow by Subaru Telescope …………………………… WATANABE et al.
25. Development of a new GPS device for precise timing measurements …………………………………… SÔMA et al.
26. High-beta Disruption in the Solar Atmosphere …………………………………………………………… SHIBASAKI
27. Sunspot Magnetic Fields Observed with a Large-Format Infrared Array ……………………………… SAKURAI et al.
28. Flexible Prism Used as an Image Stabilizer …………………………………………………………… SAKURAI et al.
29. Interpolation of One- and Two-Dimensional Images
with Pixelwise Photon Number Conservation ……………………………………………………… SAKURAI et al.
30. Chromospheric Magnetic Field of Solar Active Regions ………………………………………… CHOUDHARY et al.
31. Radial distribution of molecular gas in galaxies ………………………………………………………NISHIYAMA et al.
32. Discovery of a water megamaser in a starburst galaxy NGC 6240 ………………………………………… NAKAI et al.
33. Spectroscopic Studies of r-Process Elements in Extremely Metal-Poor Stars
with Subaru HDS and Cosmochronometry ……………………………………………………………HONDA et al.

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34. Small Fluctuation of Coronal X-Ray Intensity : Possibility of Nanoflare Heating ………………… KATSUKAWA et al.
35. Lithium isotopic ratio in interstellar media ……………………………………………………… KAWANOMOTO et al.
36. Revision of Ephemeris Yearbook (Rekishoh-Nenpyoh) …………………………………………… FUKUSHIMA et al.
37. When did the Hubble Sequence Appear ? ……………………………………………………………… YAMADA et al.
38. Bicolour Lightcurve of TNO 1996 TO66 with the ESO-VLT ………………………………………… SEKIGUCHI et al.
39. Probing Dark Matter Substructure in Lens Galaxies …………………………………………………………… CHIBA
40. Sensitivity of an imaging space infrared interferometer……………………………………………… NAKAJIMA et al.
41. CCD Photometry of the MUSES-C Mission Target: Asteroid (25143) 1998 SF36 ……………… DERMAWAN et al.

The Mechanical Test Model of the Solar-B spacecraft mounted on the shaking machine of the ISAS environmental test facility.
The healthiness of the structure against the launch condition was confirmed.

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Development of the Solar-B Spacecraft
TSUNETA, Saku, ICHIMOTO, Kiyoshi, SUEMATSU, Yoshinori, SHIMIZU, Toshifumi
HARA, Hirohisa, KANO, Ryohei, NAGATA, Shin’ichi, TAMURA, Tomonori
NAKAGIRI, Masao, NOGUCHI, Motokazu, KATO, Yoshihiro(Solar Physics Division, NAOJ)

WATANABE, Tetsuya, HANAOKA, Yoichiro, SAWA, Masaki(Radio Astronomy Division, NAOJ)

OTSUBO, Masashi(Advanced Technology Center, NAOJ)

KOSUGI, Takeo, YAMADA, Takahiro, SAKAO, Taro
MATSUZAKI, Keiichi, MINESUGI, Kenji, ONISHI, Akira(ISAS)KATSUKAWA, Yukio, KOBAYASHI, Ken, KUBO, Masahito(Tokyo University)

The Solar-B spacecraft, currently under development
toward the launch in summer of 2005, consists of the Solar
Optical Telescope (SOT) to make a precise measurementsof magnetic fields of solar photosphere with a high spatial
resolution, the X-Ray Telescope (XRT) to observe the dynamics of the high temperature corona, and the EUV Imaging
Spectrometer (EIS) to observe plasma motions in transition
region and corona. The aim of the Solar-B is to investigate
the physical coupling between the photosphere (engine) andthe corona (dissipater) to ultimately understand the coronalheating mechanism. The magnetic field maps with 0.2'' resolution, the images of high temperature corona with 1'' resolution, and the precise coronal velocity maps provided by thesetelescopes are all new and unprecedented scientific outcome
are expected.
These advanced instruments are being developed underclose collaboration between Japan (ISAS/NAOJ), the UnitedState (NASA), and the United Kingdom (PPARC). Regarding the SOT, the largest of the three telescopes, the 50cm φ
optical telescope (OTA) is developed by Japan and the Focal
Plane Package (FPP) is developed by NASA. Regarding the
XRT, NASA is in charge of the X-ray optics and Japan is incharge of the X-ray CCD camera and observation control system. EIS is developed mainly by US and UK. In this collaboration, the primary responsibility of NAOJ is the fabricationof the OTA and the X-ray CCD camera. NAOJ, in collaboration with ISAS, is also playing a role in designing and testing
the interface between each instrument and the spacecraft andin developing the Mission Data Processor which is one of the
key components of the Solar-B mission.
After extensive study and design work under the strict

constraints of mass, size, cost, time and environmental conditions, the Mechanical Test Model (MTM) of the spacecraft
was completed in May 2002. The MTM is used to verify
the mechanical validity of the spacecraft and each instrument against the launch condition, and, in case of Solar-B, its
fidelity to the flight model is quite high. Figure 2 shows the
Solar-B MTM mounted on the ISAS vibration test facility.
The cubic box in the bottom is the bus module which contains common electrical devices including the attitude control
system. Mounted on both sides of the bus are the solar array panels, each of which will be expanded to 4.5m in orbit(Figure 1). The cylindrical Optical Bench Unit (OBU) madeof a low expansion CFRP with 1m diameter and 1m height is
attached on the bus module. The OTA is installed inside the
OBU. The FPP, which is a rectangular box, is mounted on
the side of OBU. The XRT and EIS, which are also mounted
on the side of OBU, are so long (−3m) that they extend to thebottom of the spacecraft through the side of the bus module.

Figure 1: The Solar-B spacecraft in orbit3

By using the cylinder-shaped OBU, the 4 scientific instruments were compactly mounted on the spacecraft. It is noted
however that the Solar-B is one of the largest scientific satellite in Japan with its total size of 1.5m × 1.5m × 3.8m.
The status reports of OTA are given in other highlights by
Suematsu and Nagata of this annual report of NAOJ. The status of XRT is briefly described here. The mechanical/thermal
test model of the X-ray CCD camera is shown in Figure 3.
The 2K × 2K back-side illuminated X-ray CCD is cooled
down to −45˚C ~ −70˚C using radiator, and its position can becontrolled in a range of ± 1mm to accommodate any change
of focus of the 3m long telescope and to optimize the focus
position for various fields of views of observation program.
NAOJ has been performing the calibration and evaluation of
the CCD camera using the medium-size vacuum chamber and
X-ray monochromator installed in the Advanced Technology
Center. The extensive activities for fabrication and testing of
the flight CCD camera will continue until its completion in
March 2003. The CCD will then be delivered to the US to be
combined with the X-ray telescope at NASA and after final
testing the XRT will be delivered back to Japan to be installed
to the Solar-B spacecraft in January 2004.
Though the CCD and the grating of EIS are under fabrication in UK and US, it is noted that a significant contribution
from Japanese technology was made to improve their performance in resolution and sensitivity.
The system level mechanical test (2002.5-7) will be followed by the system level thermal vacuum test in October
2002. The integration of the flight OTA will start in April
2003. The integration and optical performance tests of theflight model OTA will be performed in the large clean roomof the environment test facility newly constructed in NAOJ.
After electrical/mechanical interface check starting in January
2004 and the final integration testing, the Solar-B is planned
to be launched in summer of 2005.

Figure 2: The Solar-B Mechanical Test Model mounted on the ISAS
vibration test facility.

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Figure 3: Mechanical/thermal test model of the X-ray CCD camera

Development of Solar-B Solar Optical Telescope
SUEMATSU, Yoshinori, ICHIMOTO, Kiyoshi, SHIMIZU, Toshifumi, NAGATA, Shin’ichi,
TAMURA, Tomonori, TSUNETA, Saku, NOGUCHI, Motokazu, KATO, Yoshihiro, NAKAGIRI, Masao(Division of Solar Physics, NAOJ)

OTSUBO, Masashi(Advanced Technology Center, NAOJ)

HANAOKA, Yoichiro(Division of Radio Astronomy, NAOJ)

KATSUKAWA, Yukio, KOBAYASHI, Ken, KUBO, Masahito(Univ. of Tokyo)

The solar optical telescope (SOT) to be carried aboard
the 22nd ISAS science satellite Solar-B (to be launched in
the summer, 2005) consists of the optical telescope assembly(OTA) made of 50 cm aperture Gregorian telescope and the

focal plane package (FPP) consisting of the filtergraph andspectrograph.
The OTA (Figures 1 and 2) and the FPP (Figure 3) aredesigned and manufactured in Japan and the United States,
respectively, to achieve a near diffraction-limited optical
performance in collaboration with each other. The project isgoing very well thanks to intimate communications between
Japanese and US teams. We have had ten J-US joint design
meetings (about fifty days in total) to work out the sophisticated mechanical, optical and thermal interface since the project started two and half years ago. We have also performed
joint tests for a total of three months.
We here briefl y describe the OTA structure shown in

Figure 1: Layout of the Optical Telescope Assembly (OTA).

Figure 3: Layout of Focal Plane Package (FPP).

Figure 2: OTA integration in clean booth.
5Figure 1. The OTA framework is composed of truss of
CFRP (carbon-fiber reinforced composite material), and isan adhesively bonded structure. The primary mirror (Figure1), which is only 14 kg weight, and the secondary mirror are
made of lightweight ULE like the SUBARU telescope. An
aberration-free collimator lens unit (CLU, Figure 5) is locatedFigure 4: Primary mirror of OTA.

on the secondary focus in order to transfer a collimated beam
to the FPP. A heat dump mirror (HDM, Figure 6), which ismade of aluminum, is located at the primary focus and dumps
most unnecessary solar light to the space. SOT has image
stabilization system (see a highlight article by Nagata et al.
in this volume) and a tip-tilt mirror for this system is locatedinside of the OTA.
An integration of OTA proto model, an alignment of
its optical components and random vibration/shock test
have been carried out with ISAS facility from August, 2001
through April, 2002. We prepared in advance necessary
equipments for the integration and test such as a high surface
accuracy flat mirror of 60 cm diameter (rms wavefront errorof 15 nm), a booth of cleanliness class 100, a tower for the
OTA integration and optical test (Figure 7), a high-speed laser interferometer, a large optical bench, and a six-axes drivestage.
In order to perform the optical test, the OTA proto model
was integrated with actual optical components quite similar
to flight ones except for their wavefront error accuracies; theflight model CFRP truss was used. The proto model primaryand secondary mirrors are also intended as backups for theflight by re-polishing in a contingency case. Proto model
CLU consists of two-group two-lens to give an optimal performance in test wavelength of 632.8 nm (flight model CLU

Figure 5: Flight model of Collimator Lens Unit (CLU).

Figure 6: Secondary mirror and heat dump mirror (HDM) of OTA

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Figure 7: A scene of optical test of OTA

is made of six-group six-lens). The tip-tilt mirror is made of
ULE glass supported and tilt adjusted by three piezo actuatorsfor image stabilization. All the optical components of OTA
are fixed at their best optical performance positions during the
integration and test phase, since the OTA has no adjustment
mechanism on orbit; only focus adjustment is made with a reimaging lens of FPP.
The telescope structure therefore plays a key role in giving the diffraction-limited performance; mounting mechanism of optical components, especially of the primary mirror,
should not degrade their optical qualities and truss should
maintain the separation between the primary and secondary mirror in the accuracy of five microns. It is necessary
to verify by testing that no misalignment of the OTA opticalcomponent is caused by the satellite launch condition.
The alignment of OTA by using interferometer wasverified in the beginning of the test; coma aberration due todecenter and tilt misalignment of secondary mirror and defocus due to its despace misalignment can be made negligibly
small. This first measurement is affected by the deformation
caused by the gravity. We then carried out wavefront error
measurements in both upward (+1G) and downward (−1G)
pointing telescope configuration to estimate a zero gravity
despace position. Based on these measurement, the secondary mirror was adjusted to the zero gravity focus position.
The integration and optical tests were made using the tower(3.2 m high) which is capable to mount the OTA, orienting
it upside down and to set the 60 cm flat mirror at the top or
bottom depending on the OTA orientation. To prevent the
OTA from being contaminated, all these activities were donein class 100 clean rooms by workers wearing clean clothes,hood and gloves for class 100.
In addition to static misalignment, dynamic misalignmentof OTA optics was a more important concern. To check thehealthiness of optics against the satellite launch, the most violent mechanical environment, the random vibration and shock
test simulating the launch condition was performed using the
ISAS facility. By comparing the wavefront errors of OTA
before and after the test, it was demonstrated that the changeof coma and defocus aberration of OTA is within the budget
to achieve the diffraction-limit. This was one of the most important milestones for the flight model.
SOT team of NAOJ is contributing to not only systemlevel test but also component-level test. For example, all thecontaminant doubtful material of OTA is quantitatively tested
for out-gassing using a medium-sized vacuum chamber in the

Advanced Technology Center, NAOJ, because contamination of optical surfaces and resulted degradation of photon
through-put are one of most crucial points for the success of
SOT. NAOJ is performing, using HDM coating samples, athermal cycling test and a heat load test by focusing 1000
times strong solar light on its surface. For the CLU, we performed opto-thermal tests (optical performance test in varied
space thermal condition) and chromatic aberration measurements using a MTF measurement system of NAOJ. A J-US
combination test of image stabilization system (CTM, thecorrelation tracker and tip-tilt mirror package) proto model
was successfully completed in April of 2002 in NAOJ (seeNagata et al.).
Finally, we will perform an opto-thermal test with the
OTA proto model, because the OTA has non-uniform temperature distribution on orbit. For this test, a large vacuum
chamber of 2m diameter and 4.2m tall has been manufactured(Figure 8). The chamber contains two separate shrouds; upper and down side apart, and can control OTA thermal condition similar to that on orbit (−40 degC to 50 degC). The
wavefront error of OTA will be measured in the varied thermal condition of the space to confirm that the thermal deformation and misalignment of OTA optics is within the budget
for the diffraction-limit. This opto-thermal test is scheduledin January of 2003 and then the flight model integration andtest will start in April of 2003.

Figure 8: Vacuum chamber for opto-thermal test of OTA.

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Development of Image Stabilization System for Solar Optical
Telescope onboard Solar-B satellite
NAGATA, Shinichi, SHIMIZU, Toshifumi, ICHIMOTO, Kiyoshi, TSUNETA, Saku
(Solar Physics Division, NAOJ)

MATSUZAKI, Keiichi(ISAS)The primary objective of the Solar Optical Telescope(SOT) onboard Solar-B spacecraft, which is to be launchedin summer of 2005, is to obtain high resolution magnetic
field images of solar surface with the telescope’s diffractionlimit resolution (0.2˝). Since the attitude control system of
the spacecraft cannot satisfy the scientific requirement tostabilize the SOT pointing to its sub-pixel size1 (~ 0.02˝), theSOT incorporates a closed-loop image stabilization system.
This digital servo system consists of correlation tracker, tiptilt mirror2 (figure 1), and tip-tilt mirror controller (figure 2).
The correlation tracker, provided by NASA, takes the solar
granulation images with frequency of 580 Hz and generates
the SOT pointing error signal for tip-tilt mirror control by thecorrelation analysis of the images. The tip-tilt mirror and its
controller that is responsible for the closed-loop control isprovided by NAOJ. A 64 bits CPU, which is newly developed by NASDA for space application, is used for this controller. The closed-loop control is implemented by the software of this controller. Since the main purpose of this system
is to suppress the low frequency disturbance (target cross overfrequency is 14 Hz), the software basically works as integration controller. In addition to this basic function, the software
has the capability to diagnose the system transfer function by
giving reference signal to the system and monitoring the system response to this reference signal. This software also has
the capability to insert three optional filters in the closed-loop
calculation.
The performance of the proto model image stabilization
system was evaluated February-April 2002 and it was shownthat the closed-loop system worked perfectly. We confirmedthat the system satisfied the requirement for jitter reduction (20dB at ~ 1 Hz, cross over frequency is set to 14 Hz), and thecontrol error due to the instrument is as low as ~ 0.0002˝.
The optical configuration of the test is shown in figure
3. The light through the granulation simulator, which can be
The spacecraft pointing is always drifted with a few arcseconds
amplitude due to the reaction of moving component such as momentum wheel, gyro scope, filter wheel and scan mirror of telescope and so on.
2
The lifetime test for commercial PZTs, which is used to actuate thetip-tilt mirror, have been performed since November of 2000.

KOBAYASHI, Ken(Univ. Of Tokyo)

Figure 1: Tip-Tilt mirror

Figure 2: Image stabilization system

18Figure 3: Optical configuration of the test

actuated to generate pointing errors, is reflected by the tiptilt mirror and delivered to the CCD camera. Jitter reduction
performance test, evaluation of diagnostics capability, andevaluation of system control error were performed.
A comparison of system transfer function obtained by the
diagnostic capability and the designed one is shown in figure
4. The measurement curve shown by diamonds agrees wellwith designed curve shown by solid line. The gain curve canbe approximated by software integration controller(|G((ω )| ~k2π /ω )3, and the phase curve can be approximated by the dek2
lay time of digital processors (∠GGω ) ~ τω )4.
In figure 5, an example of jitter reduction performancemeasurement is compared with a model deduced from thesystem transfer function measurement. The measurement isshown by diamonds and the model is shown by solid line.
This comparison was performed several times with varying the parameters of the controller software. The both dataagreed well with each other in all the cases, and we confirmed that diagnostic capability can be used to evaluate andadjust the closed-loop performance in orbit.
The power spectrum of pointing error signal taken byboth servo loop closed and opened are shown in figure 6; thelow frequency disturbance is greatly reduced as expectedfrom the jitter reduction shown in figure 5. In this measurement, the RMS of the pointing error with servo loop closed is
0.0002˝(1σ ).
The proto model phase was successfully closed by thesefruitful test results.
The image stabilization performance in orbit will be ul-

timately evaluated by using the closed-loop characteristics
obtained in this test and the SOT pointing properties measured in the spacecraft mechanical model test scheduled inJuly of 2002. The flight model fabrication will start after thisperformance evaluation. The flight model performance test
is scheduled May-July of 2003 in USA.

Figure 5: Jitter reduction (gain only).

Figure 6: Power spectrum of error signal taken by servo loop closed(solid line) and opened (dotted line); upper panel for X
and lower panel for Y direction.
Figure 4: System transfer function (upper panel for X direction,
lower panel for Y direction).

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k is an integration gainτ is delay time9Completion of VERA Ishigakijima Station
MIYAJI, Takeshi, IWADATE, Kenzaburo, KAMEYA Osamu
HONMA, Mareki, KOBAYASHI, Hideyuki, SASAO, Tetsuo(VERA Promotion Office, NAO)

and VERA Project Team
Following the construction of three stations of VERA
(Mizusawa, Iriki and Ogasawara) approved in the Supplementary Budget in 1999 fiscal year, the establishment of Ishigakijima Station was approved in the Supplementary Budget in2000 fiscal year. The construction started in the summer of2001 and completed in March, 2002.
A station at Ishigakijima is indispensable for VERA(VLBI
Exploration of Radio Astrometry) Project in order to achieve
the measurement goal of 10 µ -arcsecond level astrometric accuracy. The addition of the new station to the preceding three
has almost doubled the maximum baseline length from 1,300
km to 2,300 km and the number of baselines from 3 to 6. The
array enhancements, combined with the phase-compensation
capability of VERA and the triangulation using the Earth’s
Revolution around the Sun (annual parallax method), will enable VERA to realize 100 times improvement in the accuracyof position and distance measurements in astronomy.
In the foundation work at Ishigakijima, a special attention
was paid to increase the strength of the foundation since theland was reclaimed. 16 piles with 1.5 meter diameter wereused compared with 12 in three other stations. In constructing
the 20 m antenna, the experience gained in the construction of
three preceding stations were fully utilized. To avoid possible
delay in the work schedule due to typhoons, a large 200 ton
crane was used for effective construction. The construction
accuracy was measured from midnights to early mornings tominimize the heat effects due to the sunshine in the subtropical island. The novel receiving and recording systems are installed and tested in Ishigakijima where many improvements
were applied based on the experience in three other stations.
The Opening Ceremony of the station was held in Ishigaki City in May 25, 2002, where the City Mayor Mr.Ohama
made a heartful welcome speech for the VERA station. Local
people and amateur astronomers showed a great interest to the
new scientific facility in the island. 280 people attended in
the public astronomy lecture organized by NAO. 1500 people
visited the antenna site in the openhouse held in May 26. 250
people gathered in the star watching event and 150 people
visited the photoexhibition titled ‘Universe viewed by Subaru
Telescope’.
10

Test and calibration observations are now conducted in
Mizusawa, Iriki and Ogasawara stations where initial setups
and performance tests of the telescope system are almost completed. The first VLBI fringe was detected between Mizusawa
and Iriki. Simultaneous tracking of two radio sources was
successfully demonstrated. Test VLBI observations started inthree stations including Ogasawara. Test VLBI observations
with the full four-station array will start within this academic
year. Through the test and calibration observations, we expect
to soon realize the 10 µ -arcsecond level astrometric accuracy.

Figure 1: Top : 20 m antenna under construction with 200 ton crane(Autumn, 2001), bottom: Visitors looking at the moving
telescope in the openhouse held in the day after the Opening Ceremony

Interferometric Gravitational Wave Detector TAMA300:
1,000 hours Observation and Recycling Experiment
FUJIMOTO, Masa-Katsu, KAWAMURA, Seiji, YAMAZAKI, Toshitaka, TAKAHASHI, Ryu-taro
ARAI, Koji, TATSUMI, Daisuke, FUKUSHIMA, Mitsuhiro, ZHU, Zong-Hong
BEYERSDORF, Peter, SATO, Shuichi(Division of Astrometry and Celestial Mechanics, NAOJ)

ANDO, Masaki(University of Tokyo)

TAGOSHI, Hideyuki(Osaka University)

KANDA, Noriyuki(Miyagi University of Education)and the TAMA Collaboration
Data from the observation using the interferometric gravitational wave detector TAMA300 was taken six times from1999 up to now. In the event search using the data of Data
Taking 2, an observational limit to event rate of gravitational
waves due to inspiraling neutron star binaries was obtained
for the first time (H. Tagoshi, et al.: Phys. Rev. D63, (2001)
062001). In August 2000, the world top sensitivity (5 ×
10−21/√√
H
 z in strain) was achieved (M. Ando et al.: Phys. Rev.
Lett. 86, (2001) 3950). Afterwards the sensitivity around 100
Hz was also improved by modifications of the vibration isolation system. S/N to black holes with 10M in distance of 10
kpc was largely improved from 15 to 35 by this improvement.
S/N to neutron stars with 1.4M did not change (~ 35).

of the interferometer makes automatic operation of over 50
control loops succeed. Figure 2 shows integrated observation time. Histogram shows observation time in each shift(8 hours). A line shows total observation time. Observation
time is disturbed at points where histogram falls in due tomainly environmental disturbance like a typhoon and laser
trouble. The result that event rate of inspiraling neutron starbinaries inside Galaxy was less than 0.0095 event/hour (90%C.L.) was obtained from an analysis of the observation data.

Figure 2: Integrated observation time in Data Taking 6. Fall-in on
the 22th August and the 11th September shows typhoon
attacks to Tokyo.
Figure 1: History of the sensitivity improvement in TAMA300. The
sensitivity around 100Hz was improved about 10 times in
2001.

In Data Taking 6 accomplished 2001 summer (50 days),observation time more than 1,000 hours was achieved andpreeminent stability with duty cycle of 86% was obtained. In
this observation, newly developed automatic locking system

We began recycling experiment after Data Taking 6. The
recycling technique makes light power inside the interferometer increase and shot noise level decrease. Therefore more
improvement of the sensitivity is expected. Although controlof the whole interferometer became difficult by introducing
recycling mirror, the operation has been already succeeded in
December 2001. The sensitivity also was recovered almost
the same degree before introduction (improved partially).
11

Eleven-Year Solar Cycle Periodicity
in Sky Brightness Observed at Mt. Norikura
SAKURAI, Takashi(Norikura Solar Observatory, NAOJ)

We analyzed the brightness of the sky observed with acoronagraph at Mt. Norikura in the period of 1951-1997 [1].
The coronagraph is a telescope designed to observe the solar
corona without eclipse, by artificially occulting the sun witha metal disk in the telescope. In the process of measuring
the intensity of coronal emission, the sky background brightness has also been measured in order to subtract it from thecoronal emission. The sky background is due to scattering by
aerosols in the upper atmosphere.
The power spectrum analysis shows that the strongest
signal is from annual variations; generally the sky is brighterin spring because of dust from the China continent. However, we have discovered that the power spectrum also showsa clear eleven-year periodicity of solar activity cycle. The
peaks in the eleven-year component are found in the declining phase of activity, 2-4 years after the sunspot number
maximum. The amplitude of this component is about 20%of the mean. A possible interpretation is that the solar activity (probably the UV radiation) modulates the contents ofaerosols in the upper atmosphere of the earth, thus producing
variations in scattering of sunlight.

Reference[1] Sakurai, T.: 2002, Earth, Planets and Space, 54, 153.

12

Figure 1: (a) The brightness of the sky observed at Mt. Norikura in the period of 1951-1997. The thin line
shows monthly data, and the thick line is a oneyear running mean. (b) The power spectrum of thesky brightness by the maximum entropy method.
The eleven-year peak is indicated by the arrow.

Near Infrared Adaptive Optics Spectroscopyof Binary Brown Dwarf
GOTO, Miwa, KOBAYASHI, Naoto, TERADA, Hiroshi, GAESSLER, W.
KANZAWA, Tomio, TAKAMI, Hideki, TAKATO, Naruhisa
KAMATA, Yukiko, IYE, Masanori, SAINT-JACQUES, D. J.
(NAOJ)TOKUNAGA, A. T., POTTER, D., CUSHING, M.
(University of Hawaii)

We report the first near infrared spectroscopy assisted by
the Subaru adaptive optics (AO) system [1].
HD 130948 is a triple system discovered by [2] in thecourse of an imaging survey of low-mass companions to
nearby young stars. The HD 130948 system consists of abright primary star (VV = 5.9) with a faint companions at a
separation of 2".63. The goal of the present observation is toconfirm the substellarity of the faint binary companions. The
binary companions are separated by only 0".13.
Close binary brown dwarfs are important in terms that the
dynamical mass is obtained without depending on any stellar model. The mass of brown dwarfs has been determinedby comparing the optical properties such as luminosity andspectrum with an evolutional model of low mass stars. If the
dynamical mass of the stars which is independent from optical properties is available, the stellar models are then tested inturn.
Suppose the mass is same, the smaller the radius of theorbit of the system, the shorter the orbital period. To determine the dynamical mass of brown dwarfs in realistic timescale, the separation of the binary companions should be 1-2
AU or smaller. It corresponds to 0".1 to 0".2 in projection at~10pc away from us. The assistance of the adaptive optics
system is integral for the observation from the ground.
We need the spectra of both binary components separately
to compare it with existing photosphere models, which means

Figure 1: Counter clockwise from the upper right: K
K-band (2.2 µ m)
image of HD 130948 without adaptive optics system andwith adaptive optics system. A blow up of faint companions, a spectrogram at around 2.1 µ m.

Figure 2: H
H-(1.48-(1.48 - 1.82 µ m) and K
K-band (1.90 - 2.40 µ m) spectraof HD 130948 B and C. The water vapor absorption isconspicuous at the both ends of the bands, which ensuresthe low mass nature of the stars.

13that the observation needs both high spatial resolution andspectroscopic capabilities. Subaru AO with infrared cameraand spectrograph (IRCS) provides one of a few solutions thatsatisfies the requirements.
We successfully delivered the spectra of both components
HD 130948 B and C with clear separation. The water vapor
absorption features at the both ends of the H
H- and K
K- bands
clearly manifest that low mass nature of the companions.
The absorption strength indicates the effective temperatureof the HD 130948 B and C are about 1900 K. The age ofthe primary HD 130948 A is estimated to be 0.3 to 0.8~Gyrbased on the rotation period, X-ray activity, and possible attribution to a group of young stars Ursa Major Stream. Assuming the coevality of the triple system the mass of HD

14130948 B and C has been derived to be in between 0.040 M
and 0.065 M with the evolutional model of the effective
temperature [3]. The substellarities of the both binary companions are confirmed that they are lighter than the limit of
the sustainable hydrogen burning.
The monitoring observation of the binary brown dwarfs
to determine the orbital is in progress by the collaborators at
University of Hawaii.

References[1] Goto, M., et al.: 2002, ApJ,
ApJ 567, L59.
[2] Potter, D., et al.: 2002, ApJ,
ApJ 567, L133.
[3] Baraffe, I., et al.: 1998, A&A, 337, 403.

Galaxy Number Counts in the Hubble Deep Field as
a Strong Constraint on a Hierarchical Galaxy
Formation Model
NAGASHIMA, Masahiro, TOTANI, Tomonori(Division of Theoretical Astrophysics, NAOJ)GOUDA, Naoteru(Division of Astrometry and Celestial Mechanics, NAOJ)YOSHII, Yuzuru(Institute of Astronomy, University of Tokyo)

We re-analyzed number counts of galaxies using a semianalytic model (SAM) of galaxy formation based on thehierarchical clustering scenario[1]. The main results areshown in Figure 1. We have determined the astrophysicalparameters in the SAM that reproduce observations of nearby
galaxies, and used them to predict the number counts and redshifts of faint galaxies for three cosmological models for (1)the standard cold dark matter (CDM) universe (SCDM; redlines), (2) a low-density flat universe with nonzero cosmological constant (LCDM; green lines), and (3) a low-density
open universe with zero cosmological constant (OCDM; bluelines). The novelty of our SAM analysis is the inclusion of
selection effects arising from the cosmological dimming of
surface brightness of high-redshift galaxies, and also from theabsorption of visible light by internal dust and intergalactic
HI clouds. Contrary to previous SAM analyses which do
not take into account such selection effects, we find, fromcomparison with observed counts and redshifts of faint galaxies in the Hubble Deep Field (HDF), that the standard CDM
universe is not preferred, and a low-density universe eitherwith or without cosmological constant is favorable, as suggested by other recent studies. The importance of the selection effects are also shown in the Figure 1, as the difference
between the thick and thin lines. Moreover, we find that asimple prescription for the time scale of star formation (SF),being proportional to the dynamical time scale of the formation of the galactic disk, is unable to reproduce the observed
number-redshift relation for HDF galaxies, and that the SF
time scale should be nearly independent of redshift, as suggested by other SAM analyses for the formation of quasars
and the evolution of damped Ly-α systems.

Figure 1: N--m relation. The green, blue and red lines denote thepredicted galaxy counts in a Λ-dominated flat Univese(LCDM), an open Universe (OCDM), and the standard
CDM model (SCDM), respectively. The thick and thinlines indicate models with and without the selection effects, respectively.

Reference[1] Nagashima, M., Totani, T., Gouda, N., and Yoshii, Y.: 2001,
Astrophys. J., 557, 505–518.

15

Photoionization effect of the UV background on thecolour-magnitude relation of elliptical galaxies
NAGASHIMA, Masahiro(Division of Theoretical Astrophysics, NAOJ)GOUDA, Naoteru(Division of Astrometry and Celestial Mechanics, NAOJ)

We examined effects of the ultraviolet background radiation (UVB) on the colour-magnitude relation (CMR) of
elliptical galaxies in clusters of galaxies in the hierarchicalclustering scenario by using a semi-analytic model of galaxy
formation [1]. In our model the UVB photoionizes gas indark haloes and suppresses the cooling of the diffuse hot gas
onto galaxy discs. By using a semi-analytic model without
the effect of the UVB, Kauffmann & Charlot [2] found that
the CMR can be reproduced by strong supernova heating
because such supernova feedback suppresses the chemicalenrichment in galaxies especially for small galaxies as shownin Figs. 1a and 1b. We find that the CMR also becomes bluer
by the UVB in a different way from the supernova feedback
as shown in Fig. 1c. Thus there is a degeneracy between the
supernova feedback and the UVB on the CMR.
While the supernova feedback suppresses the chemicalenrichment by a similar mechanism to galactic wind, theUVB suppresses the cooling of the hot gas as schematicallyshown in Fig.2. This fact induces the suppression of the metallicity of the intracluster medium (ICM). In our model wefind that the existence of the UVB is plausible to accountfor the metallicity of the ICM in observations that is nearly
equal to 0.3 times the solar value, and that in this case we canreproduce the CMR and the metallicity of the ICM simultaneously.

References[1] Nagashima, M., and Gouda, N.: 2001, Mon. Not. R. Astr.
Soc., 325, L13–L18.
[2] Kauffmann, G. and Charlot, S.: 1988, Mon. Not. R. Astr. Soc.,
297, L23–L28.

16

Figure 1: Color-magnitude relations. The lines denote the observed
Coma CMRs with and without aperture correction, respectively. The curves indicate the model predictions.

Figure 2: Schematic descriptions of ellipticals in dark haloes.
These two galaxies have the same masses of dark matterand stars. rvir denotes the virial radius of the haloes. The
mass of the reheated, metal-polluted hot gas is β M*. The
right model has weaker supernova feedback than the left
model because of the UVB.

A Solution to the Missing Link in thePress-Schechter Formalism
NAGASHIMA, Masahiro(Division of Theoretical Astrophysics, NAOJ)

The Press-Schechter (PS) formalism for mass functions of
the gravitationally collapsed objects is reanalyzed[1]. It has
been suggested by many authors that the PS mass function
agrees well with the mass function given by N
N-body simulations, while many too simple assumptions are contained in
the formalism. In order to understand why the PS formalism
works well we consider the following three effects on themass function: the filtering effect of the density fluctuation
field, the peak ansatz in which objects collapse around density
maxima, and the spatial correlation of density contrasts within a region of a collapsing halo because objects have non-zero
finite volume. According to the method given by Yano, Nagashima & Gouda (YNG) [2] who used an integral formula
proposed by Jedamzik [3], we resolve the missing link in the
PS formalism, taking into account the three effects. WhileYNG showed that the effect of the spatial correlation alters
the original PS mass function, in this paper, we show that thefiltering effect almost cancels out the effect of the spatial correlation and that the original PS is almost recovered by combining these two effects, particularly in the case of the top-hat
filter. The mass functions in the case of a ΛCDM model are
shown in Fig.1. Our prediction (the dash-dotted curve) wellagrees with N
N-body results (crosses). On the other hand, as
for the peak ansatz, the resultant mass functions are changed
dramatically and not in agreement especially at low-masstails in the cases of the Gaussian and the sharp kk-space filters.
We show that these properties of the mass function can beinterpreted in terms of the kernel probability P(M
M1|M
M2) in the
integral formula qualitatively.

Figure 1: Differential multiplicity functions F(MF(M) with the effect of
the spatial correlation in a ΛCDM model. The solid, thedotted, the dashed and the dash-dotted lines denote F(
F M)
Mfor the PS, the sharp kk-space, the Gaussian and the top-hat
filters. The crosses indicate the mass function given by
Jenkins et al. (2001), which was obtained by fitting theirN-body simulation.
N

References[1] Nagashima, M.: 2001, Astrophys. J., 562, 7–23.
[2] Yano, T. et al.: 1996, Cosmological Constants and the Evolutionof the Universe (Eds. K. Sato et al.), University Academy Press,
p.313.
[3] Jedamzik, K.: 1995, Astrophys. J., 448, 1.

17

Spectropolarimetric Evidence of Asymmetric Outburst
in the Fast Nova V1494 Aquilae
KAWABATA, Koji S.

(Division of Optical and Infrared Astronomy, NAOJ)AKITAYA, Hiroshi, IKEDA, Yuji, ISOGAI, Mizuki, NAKAYAMA, Satoru, SEKI, Munezo(Tohoku University)

KONDOH, Masahiro

KARUBE, Tomokazu, OKAZAKI, Akira(Fukushima University)

HIRATA, Ryuko(Kyoto University)(Gunma University)

MATSUMURA, Masafumi(Kagawa University)

We reported our extended polarimetric observations ofa fast nova from the pre-maximum to transition stages [1].
The observations were made for V1494 Aquilae (= Nova Aql
1999 No.2) at the Dodaira Observatory of NAOJ between
1999 December 2 and 2000 March 29 (UT). (The Dodaira
Observatory was closed on the end of 2000 March and March
29 was the final observation day at the observatory.) We
discovered that the light from the nova had already been intrinsically polarized in the pre-maximum stage and that the
intrinsic polarization took a local maximum at visual maximum light. For the next six days a nearly orthogonal polarization component gradually increased. This component waslater accompanied and finally replaced by rapidly oscillating
components. These observations provide direct evidence thatan asymmetric geometry was present even prior to maximum
brightness. The principal geometry of the wind projected
onto the sky appears nearly constant, at least, from shortly after visual maximum to transition stages, but clumping of theejecta appears to become significant in the later stages. The
nearly orthogonal rotation of the position angle seen aroundthe maximum light could be interpreted in terms of the optical depth effect, as seen in the prolate density distribution
model of the scattering dominated photosphere [2].

References[1] Kawabata, K. S., et al.: 2001, Astrophys. J., 552, 782–786.
[2] Höflich, P.: 1991, Astron. Astrophys., 246, 481–489.

18

HIRAKATA, Nobuyuki(Takeo High School)

Figure 1: Time variations of the continuum and line polarization.
We show (a) visual light curve from VSNET, (b, c) leveland position angle of the observed polarization, respectively, and (d, e) those of the intrinsic polarization. The
open squares and filled circles represent the data averaged
for the line-free continuum areas and for strong emission
lines (Hα , Hβ and OI λ 8446), respectively. In panels(b) and (c), the estimated interstellar component at Hα isshown by horizontal dotted lines. The error bars represent
1σ observational error.

High-speed Hα camera for solar flare observations
HANAOKA, Yoichiro(Division of Radio Astronomy, NAOJ)NOGUCHI, Motokazu, ICHIMOTO, Kiyoshi, SAKURAI, Takashi
The Solar Flare Telescope Team
(Division of Solar Physics, NAOJ)

To resolve individual spikes (elementary bursts) of impulsive solar flares requires a time resolution within 1 sec and a
spatial resolution of about 1 arcsec. However, it is difficult
to realize such high temporal and high spatial resolutions simultaneously with the hard X-ray instruments. On the other
hand, it is easy to obtain one-arcsec resolution images withthe video rate in the Hα flare observations. High-cadence
Hα observations of solar flares are strongly required during
this solar maximum, because we have plenty of hard X-ray
data provided by the Yohkoh satellite and RHESSI. Then,
we have developed a high-speed Hα camera, which is a new
digital imaging system for the Hα imager of the Solar Flare
Telescope at Mitaka, for the high-cadence observations of solar flares.
Figure 1 shows a schematic view of the system. A highspeed digital camera was installed in the Solar Flare Telescope, and data from the camera are processed with a PC.
Generally, observations with high resolutions produce hugeamount of data. It has been difficult to handle such a flood of
data, but the recent advance of the computer technology enables us to handle vast data with a small computer. We constructed a framework of the general purpose real-time dataprocessing system for solar observations, and the high-speed
Hα camera is an application of this system. To install a new
application, for instance a real-time frame selector instead of
the high-speed Hα camera, we just need to replace the image
processing functions, as if to replace a ‘building block’.
In the actual operation of the high-speed Hα camera, images taken in every 30 sec are kept as context data. High-cadence images with a 0.5 sec cadence are recorded in parallel.
After the daily observation, flares are searched automatically,
and the high-cadence data of the time periods of the detected
flares are cut out and recorded on CD-Rs. Quick-look images
and movies, and daily Hα images and movies, lists of the observation time periods and detected flares are also produced
automatically, and they are open on the WWW page of theDivision of Solar Physics, NAOJ. During the period from2001 July through 2002 April, the observation was carried out
on 215 days, and 290 flares were recorded.

We are planning to replace the white-light imager of theFlare Telescope with a similar system, and to introduce a polarimeter system to measure the linear polarization in the Hαline.

Figure 1: Schematic drawing of the high-speed Hα camera system.

Figure 2: Plot of Hα brightness index on 2001 Nov. 24 (lower panel) along with a plot of soft X-ray intensity (upper panel).
Four flares were detected automatically and high-cadence
data of the shadowed periods are recorded. Sample images of the flares are also shown.

19

A Large-Scale CO Mapping of the Central Region of W51
OKUMURA, Shin-ichiro

MIYAWAKI, Ryosuke(Earth Observation Research Center, NASDA)

SORAI, Kazuo(Hokkaido University)(Fukuoka University of Education)

YAMASHITA, Takuya(Subaru Telescope, NAOJ)

HASEGAWA, Tetsuo(ALMA Project Office, NAOJ)

W51 is one of the most luminous star-forming regions in
the Galaxy. During the past two or three decades, G49.5-0.4,
the brightest H II region complex in W51, has been subject todetailed observational studies as an example of massive starforming regions. Near-infrared observations of the entire
region of G49.5-0.4 revealed that the region is separated into
four subgroups according to their ages, and that 17 O stars
in the youngest group were born in the last 0.8 Myr [1]. We
have obtained a high-resolution (16")" 13CO ((JJ = 1−0) map of")
the entire region of G49.5-0.4 to determine the relationshipbetween the morphological and kinematical features of themolecular clouds and the massive star-formation activity [2].
Observations in the 13CO ((JJ = 1−0) line were made withthe 45 m telescope at Nobeyama Radio Observatory. We
mapped an area of about 15'.3 × 16'.7 centered near W51 IRS
2, with a 17"" grid spacing.
Figure 1 shows position-velocity maps for 13CO cut along
three different axes. Here, four discrete molecular clouds
were identified toward G49.5-0.4, as shown on the figure. We
also found the peculiar morphological feature of each cloud[2]. They are too complicated for us to describe their evolution.
We think that the 60 km s−1 cloud was sandwiched between the 56 km s−1 cloud and the HV stream, resulting in a“pileup”of the molecular clouds and such a peculiar morphological feature. An abundance of massive stars in W51 IRS 1
also seems to have resulted from the “pileup.”

References[1] Okumura, S., Mori, A., Nishihara, E., Watanabe, E., &Yamashita, T.: 2000, Astrophys. J., 543, 799.
[2] Okumura, S., Miyawaki, R., Sorai, K., Yamashita, T., &Hasegawa, T.: 2001, PASJ,
PASJ 53, 793.

20

Figure 1: Position-velocity map for 13CO cut along (a) b=−00°22'0,(b) l=49°29'5, and (c) α 1950=19h21m24s. The pluses andthe cross indicate the positions of W51 IRS 2 (W51d) andW51b (see [1] and references therein), respectively, andthe shaded areas show the positions of W51 IRS 1 (W51e).
The labels in the figures show each cloud system identified here.

Near-Infrared Spectroscopy of the Compact HII Region
W51 IRS 2
OKUMURA, Shin-ichiro

MORI, Atsushi, WATANABE, Etsuji(Earth Observation Research Center, NASDA)(Okayama Astrophysical Observatory, NAOJ)NISHIHARA, Eiji

YAMASHITA, Takuya(Gunma Astronomical Observatory)

Massive stars are born in giant molecular clouds and form
HII regions around them. Young HII regions are in a state of
rapid expansion, therefore, compact/ultracompact HII regions
represent very early stages in the lives of massive stars. They
provide information on the process of massive-star formationin the clouds in which they form. Most of them are luminous
in the infrared and radio wavelength, whereas masked in thevisual by extinction. It means that they must be studied in theinfrared or longer wavelength.
Medium-resolution (R ∼ 460) spectra of the compact HII
regions W51 IRS 2 EAST (hereafter IRS 2E) and W51 IRS 2
WEST (hereafter IRS 2W) have been obtained in the K window, using a near-infrared camera and spectrograph, OASIS[1]. Brγ , HeI, [FeIII], molecular hydrogen (H2) lines, and an
unidentified line at 2.288 µ m were detected [2].
We have measured three [FeIII] transitions and compared
the line ratios with the model calculations. The observed line
ratios are consistent with the values predicted for ne ∼ 105−106
cm−3. From the observed line ratio of [FeIII] 2.22 µ m to Brγemission, we also derived an average gas phase abundance oflog (Fe++/H+)=−6.3.
We have detected emission in 7 transitions (IRS 2E) and5 transitions (IRS 2W) of H2. The rotational and vibrational
excitation temperatures, and the ortho-to-para ratios of H2
were calculated from the observed line ratios. Our results indicate that the excitation of H2 in both IRS 2E and IRS 2W isdominated by fluorescence, rather than shocks.
The unidentified line at 2.288 ± 0.001 µ m was detectedwith ∼ 2% of the intensity of Brγ in both IRS 2E and IRS
2W. There is a possibility that the line is identified as the H2
3−2 S(2) line at 2.287 µ m. However, in IRS 2E, the intensity of the 2.288 µ m line is comparable to that of the H2 1−0
S(1) line, and furthermore in IRS 2W, it is three times larger
than that of the 1−0 S(1) line. The observed intensity ratios
are hard to be explained by any of the H2-radiation models.
Therefore, we came to the conclusion that this emission is not(Subaru Telescope, NAOJ)

due to H2 and it remains unidentified.

Figure 1: Spectrum of W51 IRS 2E showing bright hydrogen andhelium recombination lines (upper) and many other weaker lines (lower).

References[1] Okumura, S., Nishihara, E., Watanabe, E., Mori, A., Kataza, H.,& Yamashita, T.: 2000, PASJ,
PASJ 52, 931.
[2] Okumura, S., Mori, A., Watanabe, E., Nishihara, E., & Yamashita, T.: 2001, Astron. J., 121, 2089.

21

Acceptance and adaptation of octants and sextants in Japan
during the 18th and 19th centuries
NAKAMURA, Tsuko(Division of Optical and Infrared Astronomy, NAOJ)

This work overviews the introduction, acceptance andadaptation of octants and sextants in Japan during the 18thand 19th centuries. Octants first appear in the Japanese literature in the 1770s. In 1783 Motoki Ryoei, a well-known
interpreter and scholar, first translated a Dutch book on octants (1749) by Cornelis Douwes. From that date, octants
continued to attract wide interest from Japanese professional
and amateur astronomers and land surveyors, and a considerable number of books on octants and sextants were published
up to the 1860s. In this study we made clear that C. Douwes
played an important role in translating into Dutch the eminent book “Astronomie” by the French astronomer J.J.F. de
Lalande, through which the Japanese recognized the decisive
superiority of the Western astronomy over the traditional oneof Chinese origin. We also found out that, around 1806, an
octant was made for the first time by Michikata Kume, thelow-ranking vassal of a Daimyo lord in Shikoku. Owing to
the strict seclusion policy adopted by the Tokugawa shogunate during the Edo period, the Japanese adapted octants as aconvenient instrument for land surveying rather than for navigation, and even unique range finders were also invented as amodification. It was not until after the mid-1850s that octants
were used for marine navigation.

Fig. 1: Sextant designed for land-surveying (from “Rokubungi Ryochi Tebikiso” published in 1852 by Murata Sajuro). Notethat there are no sun-glasses.

Reference[1] Nakamura, T.: 2002, J. Astron. History and Heritage, 5, in press.

22

Fig. 2: Range-finder called “Shakaku Kangi” (from “Rokubungi
Ryochi Tebikiso”).

Dense Plasma Torus around the Nucleus of NGC 1052
KAMENO, Seiji, INOUE, Makoto(Division of Radio Astronomy, NAOJ)

SAWADA-SATOH, Satoko, SHEN, Zhi-Qiang, WAJIMA, Kiyoaki*(The Institute of Space and Astronautical Science)

Reference[1] Kameno, S., Sawada-Satoh, S., Inoue, M., Shen, Z.-Q., and
Wajima, K.: 2001, Publ. Astron. Soc. Japan, 53, 169–178.
*: Present position: NAOJ
1: The VLBA is a facility of the National Radio Astronomy Observatory in U.S.A.

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Figure 1: Trichromatic radio image of NGC 1052. Images at 15.4,
8.4, and 2.3 GHz are drawn in blue, green, and red channels, respectively. The western receding jet shows blue
color, which indicates absorption at lower frequencies.

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Some galaxies host Active Galactic Nuclei (AGNs) whichemit tremendous power of ∼ 1035 − 1041 W. The origin of thepower is considered to consist of a massive black hole withaccreting matter onto it. Here, we introduce radio observations unveiling ‘fuel reserver’ associated with an AGN in
NGC 1052 at the distance of 60 million light year.
Figure 1 shows the trichromatic radio image of NGC
1052 obtained with the VLBA1. Twin jets emanating fromthe nucleus are symmetric at 15.4 GHz, while the receding jet
is fainter than the approaching one at 2.3 GHz as drawn by
blue color. Spectral analysis indicates that free-free absorption (FFA) is working towards the receding jet.
FFA is a radiative transfer process that cold dense plasma
diminishes radio emission. Its opacity indicates electron density, electron temperature, and path length of the absorbing
plasma.
Figure 2a illustrates the distribution of the FFA opacity
calculated from the trichromatic images. The opacity along
the jet (figure 2b) rapidly decreases towards the approaching jet, while it covers ∼ 2 light year towards the recedingjet. The asymmetric opacity profile is suggestive of a dense
plasma torus perpendicular to the jet (figure 2c), which can bea ‘fuel reserver’ of AGN. We also found diffuse ambient absorber surrounding the torus, drawn by green curve in figure2b.
It is remarkable that the spherically symmetric distribution coexists with the torus. The latter should be supportedby the centrifugal force by rotation around the nucleus, while
the former is supported by the thermal pressure. Our results
suggest transition from the radial accretion to rotational accretion.

�����������

������������
�������

��������������
�����������
������������

Figure 2: (a): A grayscale distribution of the free-free absorption
opacity. (b): The opacity profile along the jet. It peaks at
the nucleus and tails towards the receding jet, but rapidly
decreases towards approaching jet. (c): A schematic diagram of NGC 1052. A plasma torus perpendicular to thejet is the free-free absorber, which covers the receding jet
but does not the approaching one. That is why the opacity
distribution is asymmetric.

23

Near-IR study of M16 (SIRIUS first light observations)
SUGITANI, Koji

(Insitute of Natural Sciences, Nagoya City University)

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

NAKAJIMA, Yasushi, NAGASHIMA, Chie, NAGAYAMA, Takahiro, NAGATA, Tesuya, SATO, Shuji(Department of Astrophysics, Nagoya University)

PICKLES, Andrew J.

NAKAYA Hidehiko(Institute for Astronomy, University of Hawaii)(Subaru Telescope, NAOJ)FUKUDA, Naoya

OGURA, Katsuo(Department of Physics, Chiba University)(Kokugakuin University)

SIRIUS (Simultaneous three-color InfraRed Imager
for Unbiased Surveys) has been constructed under the collaboration between Nagoya University, NAOJ, Nagoya City
University, and others [1]. We have performed its first lightobservations in August and October, 2000, on the Universityof Hawaii 2.2 m telescope. Here we present JHKs imaging
study of M16 that were obtained with SIRIUS.
In contrast to optical images, the infrared images showthat the Eagle Nebulas pillars have head-tail structures, withthe heads faced toward the central part of the star cluster
NGC 6611 and the tails trailed toward the opposite side
(Fig. 1). We have found a number of previously unreported
young stellar object (YSO) candidates associated with thesehead-tail pillars [2]. In particular, the youngest YSOs arelocated at the tips of the pillars or globules, facing toward thecentral part of NGC 6611. Some are associated with nearinfrared jets or cometary reflection nebulae, with indicationsof a circumstellar disk. This YSO distribution and the cloud
structures suggest that the most recent star formation is taking
place following the interaction with UV light from the OBstars in NGC 6611.
This image was also used for the paper of NMA observation of M16 [3].

References[1] Nagashima, C., et al.: 1999, Star Formation 1999, ed. T.
Nakamoto (Nobeyama: NRO), 397, or
http://www.z.phys.nagoya-u.ac.jp/~sirius[2] Sugitani, K., Tamura, M., Nakajima, Y., Nagashima, C.,
Nagayama, T., Nakaya, H., Pickles, A.J., Nagata, T., Sato, S.,
Fukuda, N., Ogura, K.: 2002, Astrophysical Journal, 565, L25.
[3] Fukuda, N, Hanawa, T., Sugitani, K.: 2002, Astrophysical Journal, 568, L127.

24

Figure 1: JHKs three-color composite image of M16 (J: blue; H:
green; Ks: red) obtained by SIRIUS, which was mounted
on the UH 2.2 m telescope. North is up, and east is tothe left.

2 Millimeter Dust around NGC 7538-IRS 1, 2, and 3. I.
Unifilled structure of dust
AKABANE, Kenji*, MATSUO, Hiroshi, KUNO, Nario(Nobeyama Radio Observatory, NAOJ)

SUGITANI, Koji

(Institute of Natural Science, Nagoya City University)and of the total intensity of the wing parts of the CO(
CO(JJ=1−0)
J=1−0)
line emission of the region (figure 1)[2].
Table 1: A gray body fitting result
Parameter
Tdust(K)(1)2rc (pc)(2)β (3)Ω0 (sr)(4)Ωe (sr)(5)η (6)Ae (= R2Ωe m2)(7)

42
~0.5
2.0
2.6 × 10-8
1.08 × 10-80.42
8.03 × 1031

(1) Temperature of the dust grain.
(2) Full size of the distributed dust clumps.
(3) Absorption index of dust grains.
(4) Solid angle of the dust clumps.
(5) Total of net solid angle of the dust emission area.
(6) Filling factor of the dust clumps.
(7) Total of net projective area of the dust emission.
5

10

References

300

100 50 25

10S(1-e- ν )Be

Td= 42 K

2.2m(max)=2.6 10-8sr[1] Akabane, K., Matsuo, H., Kuno, N., and Sugitani, K.: 2001,
PASJ 53, 821.
PASJ,[2] Kameya, O., Hasegawa, T., Hirano, N., Takakubo, K., and Seki,
M.: 1989, ApJ,
ApJ 339, 222.

: IRAS DATA
: Werner et al.(1979): Wynn-Williams et al.(1974)(IRS 1+2+3)

=1.0

4

10

22

: Chini et al.(1986)

3e(min)=1.08 10-8sr

1023Sν (Jy)

=0.42
(

)

2

24

10

Wm-2Hz-1

A 2mm continuum mapping observation around NGC
7538-IRS1, 2, and 3 was made by the Nobeyama Bolometer
Array (NOBA) with a spatial resolution of 12". An extended
source of ~ 32"" × 44" (∆α × ∆δ ), having a hardly resolved
central core structure, was observed [1]. The core gives
flux density of 3.1Jy ± 1Jy and is clearly identified with thatfrom the compact free-free emission region. A smooth andextended source (figure 1) gives an integrated flux density of
5Jy ± 1.5Jy, and an intensity spectrum of ν 3 ~ ν 3.5 in the millimeter wave region. The fitting of a gray body function tothe observational data shows that an absorption index β , of 1.8~ 2.0, filling factor η , of 0.3 ~ 0.5, and the dust temperature,
Td of 34K ~ 45K are of reasonable parameters for this 2mm
extended dust (figure 2, table 1). Astronomical silicate grains
were examined for the dust model. The total mass and luminosity were obtained as Md = 0.85 × 102 M and Ld = 2.2 ×
105 L , respectively. The extent of 2mm dust emission partly
coincides with those of the 100µ m map, of the 57µ m map,

(1)
(2)

10
(3)

1

*Professor Emeritus, Tokyo Astronomical Obseravtory, Universityof Tokyo-1

10

H II free-free emisison(IRS 1+2+3)

8000K Te(4)
3 2

Figure 1: Overlap of the distribution of the both wing parts of
CO(JJ=1−0)
CO(J=1−0) line (dashed line)[2] on the present result of
2mm dust (full line)[1].

25

Akabane et al.

1110(1) Werner et al. (1979)(2) Chini et al. (1986)(3) This work

1 (mm)

26

4200K Te

(4) Akabane et al. (1992)

12

10

13

10

14

10

f (Hz)

Figure 2: Spectral feature of the sources in the region of NGC
7538(N). Reported mm, sub-mm, far-IR, and mid-IR
data of the region are plotted with the referred black bodyemission profiles[1].

25Buried AGNs in LINER type ultraluminous infrared galaxies
IMANISHI, Masatoshi(Division of Optical and Infrared Astronomy, NAOJ)

DUDLEY, Chris C.

(Naval Research Laboratory)

Ultraluminous infrared galaxies (ULIRGs) radiate most of
their quasar-like luminosities (> 1012L ) as infrared dust emission. Since the cosmic submillimeter background emission,
which reflects the total amount of the cosmic activity hidden
by dust, is dominated by discrete sources, similar to ULIRGs,
ULIRGs have been used to trace the star formation rate, dust
content, and metallicity in the early universe. However, themost important question of whether ULIRGs are powered
predominantly by starburst activity or an AGN buried in a
thick dust shell is energetically required remains unanswered.
In order to detect the putative buried AGNs and properly
evaluate their energetic importance in ULIRGs, it is essential
to observe at wavelengths where dust extinction is low. At 3
−4 µ m, dust extinction is as low as that at 7−8 µ m [4], andwe can quantitatively distinguish between starbursts andburied AGNs, by using the 3.3 µ m PAH emission and 3.4µ m carbonaceous dust absorption (Figure 1). Recent detailed
studies have shown that the bulk of the infrared luminosities
of ULIRGs originate in compact (< a few 100 pc) nuclear
regions and not extended regions [6]. Thus, ground-based slit
spectroscopy is better suited than space-based large aperture
spectroscopy to find evidence for the putative buried AGNs at
the nuclei of ULIRGs, by minimizing the contamination fromextended emission.
Theoretically, buried AGNs produce LINER-type optical
spectra because an X-ray dissociation region dominated byemission from neutral and singly-ionized species develops
around them [5]. We thus performed 3−4 µ m spectroscopyof three bright ULIRGs classified optically as LINERs, andfound strong evidence for energetically important buried
AGNs in two out of the three observed LINER ULIRGs (IRAS08572+3915 and UGC 5101; see Figure 1). Based on thecomparison of the optical depth of the 3.4 µ m carbonaceousand 9.7 µ m silicate dust absorption, it was also suggested that
dust has a strong temperature gradient [1], which favors thepresence of a compact energy source, that is, an energeticallyimportance buried AGN. Our result contradicts the widelyheld view that LINER ULIRGs are starburst powered. We
plan to extend this study to fainter LINER ULIRGs to clarify more unambiguously the energetic importance of buried
AGNs in LINER ULIRGs in general.
26

MALONEY, Philip R.
(University of Colorado)

Figure 1: (a) A 3−4 µ m spectrum of a starburst powered galaxy(NGC 253) Since the equivalent width of the 3.3 µ m PAH
emission is, by definition, robust to dust extinction, strong
3.3 µ m PAH emission should be always seen regardless ofdust extinction of starbursts. (b) A LINER ULIRG powered by a buried AGN ((AV ~ 150 mag), with undetectablestarburst activity (IRAS 08572+3915). It shows a strong
3.4 µ m carbonaceous dust absorption feature, with nodetectable 3.3 µ m PAH emission. (c) A LINER ULIRG
powered both by an energetically important buried AGN
and detectable starburst activity (UGC 5101). The solidline is the adopted continuum level. It shows both the 3.4µ m carbonaceous dust absorption and the 3.3 µ m PAH
emission, but the equivalent width of the PAH emission
is significantly lower than in starburst galaxies. Based on
the optical depth of the 3.4 µ m dust absorption after subtracting the contribution from starbursts to the observed
3−4 µ m fluxes, we can estimate dust extinction toward theburied AGN ((AAV > 100 mag in this source), and found thatthe dereddened dust emission luminosity produced by theburied AGN can account for >70% of the infrared luminosity of UGC 5101. Adopted from [2] and [3].

References[1] Imanishi, M.: 2000, MNRAS, 319, 331.
[2] Imanishi, M., and Dudley, C. C.: 2000, ApJ,
ApJ 545, 701.
[3] Imanishi, M., Dudley, C. C., and Maloney, P. R.: 2001, ApJ,
ApJ 558,
L93.
[4] Lutz et al.: 1996, A & A, 315, L269.
[5] Maloney, P. R., Hollenbach, D. J., and Tielens, A. G. G. M. :1996, ApJ,
ApJ 466, 561.
[6] Soifer et al.: 2000, AJ,
AJ 119, 509.

A list of all integrable two-dimensional homogeneouspolynomial potentials with a polynomial integral oforder at most four in the momenta
NAKAGAWA, Katsuya(Graduate University for Advanced Studies/NAOJ)

A Hamiltonian system with two degrees of freedom is integrable if the system has a first integral which is independentof the Hamiltonian. The purpose of this study is to investigate the conditions for which a Hamiltonian system with a
two-dimensional homogeneous polynomial potential, definedby
H = –1 ( px2 + py2 ) + V(
V(x,y),
2(1)

possesses an additional polynomial first integral. The homogeneity of potentials is assumed from the following two reasons:• The integrability of a non-homogeneous potential depends
on the integrability of each of its lowest-degree part andhighest-degree part, which means that a study of integrability for homogeneous potentials is the basis of considering
integrability for non-homogeneous potentials.
• The system with a homogeneous potential is invariant under a scale transformation, which leads to the weightedhomogeneity of first integrals. As a result, we can simplify
the form of first integrals.
Let a polynomial Φ ((x, y, px , py ) be a first integral of thesystem. Then, the Poisson bracket of Φ and H vanishes identically, which gives an identity for x, y, px ,py . Then, we havesimultaneous algebraic equations for the coefficients of thepotential and the first integral.
By solving these simultaneous algebraic equations, we
can findk
V = r k = ((xx2 + y2)k/2(kk = even)(2)with an additional polynomial first integral {\em linear} inthe momenta, and
k+1
k
k+1
 r + x  k+1
r−
V = –1   + (−1)k x  

r  2
2

V = Ax k + By k

YOSHIDA, Haruo(Division of Astrometry and Celestial Mechanics, NAOJ)

momenta. The potentials (2), (3), and (4) are separable inpolar, parabolic, and Cartesian coordinates, respectively.
In the early 1980s, the following three potentials were discovered with an additional polynomial first integral which isgenuinely quartic in the momenta.
3 xy2
V = x3 + ––16

(5)

1 xy2 + √
–—
3 i y3V = x3 + ––
2
18

(6)

3 x2 y2 + ––1 y4
V = x4 + ––
4
8

(7)

According to Hietarinta (1983), these three potentials are
the only ones that admit an additional polynomial first integral genuinely cubic or quartic in the momenta if the degreeof homogeneous potentials is {\em five or less}.
In this paper [1], the case for homogeneous potentials ofan arbitrary degree is investigated. As a result, the following
theorem is obtained.
Theorem ([1]) If the degree of the homogeneous potential is
five or more, then the system can not have an additional polynomial first integral which is genuinely cubic or quartic in
the momenta.
This theorem, together with the result of Hietarinta (1983),
brings a list of all integrable two-dimensional homogeneouspolynomial potentials with an additional polynomial first integral of order at most four in the momenta:• A first integral linear in the momenta: (2)• A first integral quadratic in the momenta: (3), (4)• A first integral cubic in the momenta: —• A first integral quartic in the momenta: (5), (6), (7)

(3)
(4)

with an additional polynomial first integral quadratic in the

References[1] Nakagawa, K. and Yoshida, H.: 2001, J. Phys. A: Math. Gen.,34, 8611–8630.

27

Submillimeter Imaging Polarimetry of the NGC 7538 Region
MOMOSE, Munetake(Institute of Astrophysics and Planetary Sciences, Ibaraki University)

TAMURA, Motohide

KAMEYA, Osamu(Division of Optical and Infrared Astronomy,NAOJ) (Division of Earth Rotation, NAOJ)

CHRYSOSTOMOU, Antonio, HOUGH, Jim H.

(Department of Physical Sciences, University of Hertfordshire)

Imaging polarimetry of the 850µ m continuum emission
in the NGC 7538 region was carried out using the SCUBA
Polarimeter. The polarization map is interpreted in termsof thermal radiation by magnetically aligned dust grains.
Two prominent cores associated with IRS 1 and IRS 11,
IRS 1(SMM) and IRS 11(SMM), are found in the surface
brightness map. Although these cores look similar in surface
brightness, their polarization shows striking differences. In
IRS 11(SMM), the polarization vectors are extremely wellordered, and the degrees of polarization are quite high withan average of ~3.9%. In IRS 1(SMM), on the other hand, thedirections of polarization vectors are locally disturbed, andthe degrees of polarization are much lower (1.6% in average) than those of IRS 11(SMM). These differences suggestthat small scale fluctuations of the magnetic field are more
prominent in IRS 1(SMM). This can be interpreted in termsof the difference in evolutionary stage of the cores. Inside
IRS 1(SMM), which seems to be at a later evolutionary stage
than IRS 11(SMM), substructures such as subclumps or a

GREAVES, Jane S.

(Joint Astronomy Centre)

MORINO, Jun-Ichi(Subaru Telescope, NAOJ)

cluster of infrared sources have already formed. Small scale
fluctuations in the magnetic field could have developed during the formation of these substructures. The distribution ofmagnetic field directions derived from our polarization map
agrees well with those of molecular outflows associated with
IRS 1(SMM) and IRS 11(SMM). Comparisons of energy
densities between the magnetic field and the outflows showthat the magnetic field probably plays an important role inguiding the directions of the outflows.
This work [1] was supported in part by the Grant in-aid
for Scientific Research of Ministry of Education, Science,Sports and Culture, and by the Japan Society of the Promotion of Science.
References[1] Momose et al.: 2001, Astrophys. J., 555, 855-862.
[2] Kameya et al. in Proc. of the 7th Manchester Astronomical Conference on “Molecular Clouds” ed. R. James & T. Millar (Manchester: UK): 1990, 111-112.

Figure 1: (a) Polarization E vectors of the 850µ m continuum emissions (green lines) superposed on the surface brightness map (gray scale).
The length of each line is proportional to the polarization degree. (b) Magnetic field directions derived from the polarization vectorsin (a) (black and violet lines) superposed on the distribution of CO(
CO(JJJ=3−2)=3−2) high-velocity outflows [2] (contours). The black lines
indicate field directions inside the regions where the flux density is higher than 10 % of the IRS 1(SMM) peak while the violet lines
indicate those outside the regions. The blue and red contours show the distribution of the CO(
CO(JJJ=3−2)=3−2) emissions integrated over VLSR
= −74 to −64 km s−1 and VLSR = −54 to −44 km s−1, respectively.

28

The Spin Temperature of NH3 in Comet C/1999S4 (LINEAR)KAWAKITA, Hideyo(Gunma Astronomical Observatory)

WATANABE, Jun-ichi(Public Information Office, NAOJ)

ANDO, Hiroyasu, FUSE, Tetsuharu, OKITA, Kiichi, USUDA, Tomonori(Subaru Telescope, NAOJ)

AOKI, Wako, HONDA, Satoshi, KAJINO, Toshitaka, NOGUCHI, Kunio, KAWANOMOTO, Satoshi(Division of Optical and Infrared Astronomy, NAOJ)IZUMIURA, Hideyuki, WATANABE, Etsuji, YOSHIDA, Michitoshi(Okayama Astrophysical Observatory, NAOJ)

SATO, Bun'ei(Okayama Astrophysical Observatory, NAOJ, Department of Astronomy, School of Science, University of Tokyo)

KAMBE, Eiji

SADAKANE, Kozo

TAKADA-HIDAI, Masahide

TAKEDA, Yoichi(Department of Earth and Ocean Sciences, National Defense Academy) (Astronomical Institute, Osaka Kyoiku University)(Liberal Arts Education Center, Tokai University)(Komazawa University)

A high dispersion spectrum of Comet C/1999 S4 (LINEAR) was obtained in the optical region using the high dispersion spectrograph (HDS) on the Subaru telescope when
the comet was 0.863 astronomical units (AU) from the Sun
before its disintegration. We obtained high signal-to-noise
ratio emission lines of the cometary NH2 bands from which
an ortho-to-para ratio (OPR) of 3.33±0.07 was derived on
the basis of a fluorescence excitation model. Assuming thatcometary NH 2 mainly originates from ammonia throughphotodissociation, the derived OPR of NH2 molecules shouldreflect that of ammonia, which provides information on theenvironment of molecular formation or condensation andof the thermal history of cometary ices. It can be safely assumed that the OPR of ammonia in comets was unchanged in
the nucleus. If the OPR equilibrated to the temperature of icy
dust mantle in the solar nebula, the derived OPR suggests thetemperature of about 28 K. This may indicate a formation region of the cometary ammonia ice between the orbit of Saturnand that of Uranus in the solar nebula [1].

Reference[1] Kawakita, H., Watanabe, J., et al.: 2001, Science, 294, 1089.

Figure 1: Spectra of NH2 Ã (0, 9, 0) and Ã (0, 7, 0) bands incomet C/1999 S4 (LINEAR) and the synthetic spectrum
based on the fluorescence equilibrium calculation.

29

Wide-Field TV Observation of the Leonid Meteor Storm
in 2001: Main Peak over JapanWATANABE, Jun-ichi(Public Relations Center, NAOJ)

SEKIGUCHI, Tomohiko(Division of Radio Astronomy, NAOJ)SHIKURA, Masato(Departmernt of Physics, Science University of Tokyo)

NAITO, Seiichiro(Department of Astronomy, School of Science, The University of Tokyo)

ABE, Shinsuke(The Institute of Space and Aeronautical Science)

The world-wide campaign of the Leonid meteor shower
performed until 2000 resulted in great success. One of theimportant advances in meteor science is on the structure of
the spatial distribution of meteoroids in the meteor stream,
which consists of several narrow dust trails. Each trail wasformed by meteoroids ejected at a particular return of theparent comet. Based on this concept, several researchers
performed a detailed calculation, which resulted in great success for reproducing the observed time profile of the Leonids
activity.
According to these so-called "dust trail" theories, theLeonid meteor shower was expected to show a strong display
between 17h 00m and 18h 30m UT in 2001 November 18 by
two dense dust trails of 1699 and 1866. These predictions
suggested that Japan would be one of the best observationalsite.
As same as our observations in 1998[1] and 1999[2], we
carried out a wide-field TV observation at Iwaki city, Fukushima prefecture, from 17h17m UT through 20h20m UT
on 2001 November 18[3]. We used a lens with the shortest
focal length ((ff = 3.8 mm, F0.8, HG3808AFCS-HSP, CBC
Co.). The combination of the back-up camera with this lensgiving a wide field of view of 80˚.6 × 65˚.0, along with alimiting magnitude of 3.5. We detected 869 Leonid meteors,along with 32 non-Leonids. A broad main-peak of the activity
was recognized at around 18h25m UT, when the peak influx
rate of meteoroids was 1.4 × 10−5 km−2 s−1 (mag ≤ +3). The
activity of this main peak was comparable to that of a storm
observed in 1999 over Europe.

30

Figure 1: Time variation of the number of Leonid meteors detectedin our TV observation on 2001 November 18. The dashdotted line is the hourly rate of the number of meteors
observed in a 15 min interval, and the solid line is thenumber after a correction for the radiant-point elevation.
The solid curve is the elevation of the radiant point.

References[1] Watanabe, J., Abe, S., Fukushima, H., Kinoshita, D.: 1999,
Pub. Astron. Soc. Japan, 51, L11–L14.
[2] Watanabe, J., Takahashi Y., Sasaki A., Abe, S., Kinoshita, D.,
Shiki, S.: 2000, Pub. Astron. Soc. Japan, 52, L21–L24.
[3] Watanabe, J., Sekiguchi, T., Shikura, M., Naito, S., Abe, S.:
2002, Pub. Astron. Soc. Japan, 54, L23–L26.

Optical Follow-up of the GRB 010222 Afterglow
by Subaru Telescope
WATANABE, Jun-ichi(Public Relations Center, NAOJ)KINOSHITA, Daisuke(Graduate University for Advanced Studies/NAOJ)

KOMIYAMA, Yutaka, FUSE, Tetsuharu(Subaru Telescope, NAOJ)

URATA, Yuji

(Departmernt of Physics, Science University of Tokyo)

YOSHIDA, Fumi

(Graduate School of Science and Technology, Kobe University)

Gamma Ray Bursters (GRBs) are thought to be the mostviolent phenomena in the universe. Follow-up observations
at various wavelength are necessary to reveal the nature of
GRBs. However, the difficulty of such a follow-up still remains mainly concerning the unexpected nature of the timeand position of GRBs. Therefore, some coordinated cooperations should be necessary for the follow-up of the GRBs by
many researchers including those in the other field.
When we were performing a deep survey observation
for the Edgeworth-Kuiper belt objects on 2001 February 21
using the Suprime-Cam of the Subaru telescope at MaunaKea, we received an alert concerning the appearance ofGamma Ray Bursts (GRB 010222), which appeared on Feb.
22, 07:23:30 U.T. The message also stated that this GRB
010222 was a very bright GRB, possibly the brightest everobserved by BeppoSAX [1]. We decided to dedicate a partof our telescope time to observe the optical afterglow of GRB
010222[2]. The obtained R-band magnitude was 18.59 ± 0.04
at February 22.51 UT, 18.99 ± 0.04 at February 22.65 UT,
and 21.76 ± 0.03 at February 25.64 UT. The light curve madefrom all data reported so far shows the decay of the brightness with a broken power law, of which the indices are −0.92± 0.01 before and −1.27 ± 0.01 after the break. The breakpoint of the light curve is 0.73 ± 0.02 d after the burst, whichis the earliest example ever observed.

Figure 1: Time variation of the brightness of GRB 010222. Timeis counted by day from 22.308 UT. The open circles are
our data, while others are data taken by GCN circulars(GCN967 A. Henden et al., GCN 970 K. Z. Stanek et al.,GCN 973 P. A. Price et al., GCN 975 J. P. U. Fynbo et al.,GCN 983 K. Z. Stanek et al., GCN 985 N. Masetti et al.,GCN 990 A. Oksanen et al., GCN 991 K. Z. Stanek & E.
Falco, GCN 992 G. Valentini et al., GCN 998 & 1000 C.
Veillet, GCN 1002 S. Holland et al.). The light curve wasfitted by a power law together with a break at 0.73 d after
the burst.

References[1] Piro, L.: 2001, GCN Circ., 959.
[2] Watanabe, J., Kinoshita, D., Komiyama, Y., Fuse, T., Urata, Y.,
Yoshida, F.: 2001, Pub. Astron. Soc. Japan, 53, L27–L31.

31

Development of a new GPS device
for precise timing measurements
SÔMA, Mitsuru(Division of Astrometry and Celestial Mechanics, NAOJ)

HAYAMIZU, Tsutomu(Sendai Space Hall),

GESHIRO, Hiroyuki(Oishikogen Astronomical Observatory)

The Japanese shortwave JJY time signals were shut down
on 2001 March 31st. Instead the longwave time signals are
now emitted at 40 and 60 kHz, and inexpensive clocks andwatches controlled by those signals are on the market. However according to our measurements those radio-controlled
clocks have typically delays of 0.1s to 0.3s, and therefore
they cannot be used for precise timing observations [1].
The longwave JJY time signals have only a carrier waveof 40 kHz or 60 kHz and by changing the length of the carrier
signal of each second they provide binary codes of the date,time, etc. In the case of the longwave WWVB time signals
the binary codes are provided by different reduction percentage of the amplitude of the carrier. Both of JJY and WWVB
have no audio component, and we understand that most of
the longwave time signals in the world are of the same kinds.
Therefore, in order to make the signals audible, it is needed
to use the CW mode of the receivers and a filter of about 500
Hz, which can cause a delay of about several tens of milliseconds. This fact demonstrates that it is very hard to get a
precise pip sound at each second like the shortwave time signals.
As seen above there was no simple way of using the
longwave time signals for precise timing measurements. Accordingly we designed equipment, called the GHS clock,that can be used with inexpensive GPS receivers to produce
both an LED flash and a pip sound at the beginning of eachsecond [2][3]. GHS stands for Geshiro-Hayamizu-Sôma,
which comes from the names of the authors of the equipment.
According to the GPS receiver manual, this device has an accuracy better than 500 nano-seconds, and our tests show thatit usually has an accuracy better than 200 nano-seconds. A
brief description of the GHS clock is also given in [4].
The GHS clock provides both a shortwave JJY like pip
sound and an LED flash at each second, so that it can be used
32

by those who have used the shortwave JJY time signals and it
can also be used by video observers who want to get precise
timing measurements of astronomical phenomena.
The users can make their own GHS clocks according totheir elaborate plans. Fig. 1 shows an example of a microcomputer-installed GHS clock, which can display the date,the time, the geodetic coordinates of the station, the true local
solar time, the local sidereal time, and the hour angle of Polaris on the liquid crystal screen.

Figure 1: Microcomputer-installed GHS clock

References[1] Sôma, M., Zhu, Z.: 2000, ATF 2000 Proceedings, Communications Research Laboratory, Japan, 302–304.
[2] Hayamizu, T., Geshiro, H., and Sôma, M.: 2000, The Astronomical Herald
Herald, 93, 720–727 (in Japanese).
[3] Hayamizu, T., Sôma, M., Geshiro, H., and Hashiguchi, T.: 2001,
Report Nat. Astron. Obs. Japan, 5, 73–79 (in Japanese).
[4] Nugent, R.: 2000, Occultation Newsletter, 8 (2), 3–5.

High-beta Disruption in the Solar Atmosphere
SHIBASAKI, Kiyoto(Division of Radio Astronomy, NAOJ)

The outer layers of X-ray loops in solar flares are known
to be more active: they are hotter than the lower loops andabove-the-loop-top hard X-ray sources are formed there.
These phenomena are interpreted as the result of the reconnection above the loop, which convert magnetic energy into
thermal and non-thermal energy of plasma. However, little
direct evidence for the reconnection has been presented sofar. This paper interprets the activity in the outer layer offlaring loops on a different scenario. Coronal loops filledwith hot and dense plasma (high beta) or with fast plasma
flow, surrounded by the low-beta corona, are unstable at theirouter boundary where the curvature is convex outward andthe density gradient is inward. The centrifugal force acting
upward on the plasma in the loop can exceed that of gravity.
This condition is favorable for localized interchange instabil-

ity called “ballooning instability” and the plasma in the loop
is ejected when the instability has developed into non-linear
phase (“high-beta disruption”). This is a natural consequenceof the high-beta (and/or the high velocity) plasma confinedin a curved coronal loop. The high-beta disruption has many
elements common to solar flares. In this paper, importance ofthe high-beta plasma is stressed, which is a neglected part ofthe solar activity so far.

Reference[1] Shibasaki, K.: 2001, Astrophys. J., 557, 326.

33

Sunspot Magnetic Fields Observedwith a Large-Format Infrared Array
SAKURAI, Takashi(Solar Physics Division, NAOJ)YANAGISAWA, Kenshi(Okayama Astrophysical Observatory, NAOJ)

KOBIKI, Toshihiko(Norikura Solar Observatory, NAOJ)

KASAHARA, Shouichi(Faculty of Science and Technology, Meisei University)

NAKAKUBO, Kayoko(Suginami Science Center, Tokyo)

Magnetic fields on the sun are usually measured by the
Zeeman effect of spectral lines. The sensitivity of magnetic
field measurement depends on the width of spectral lines andthe magnitude of the Zeeman splitting. The former increases
linearly in wavelength, while the latter increases in proportion
to the square of the wavelength. For example, in the H-bandHregion (1.5-1.8 µ m) in the infrared, we can achieve a threetimes higher sensitivity compared to the visible wavelengths
near 5000 Å.
We have carried out spectro-polarimetric observationsof sunspots by using a PtSi near-infrared camera (KONIC)of Kiso Observatory, The University of Tokyo, in November
1999. The detector has a format of 1040 × 1040 pixels. The
camera was attached to a spectrograph of the Domeless Solar
Telescope at Hida Observatory, Kyoto University. Because
the quantum efficiency of the PtSi detector is low (about 2%),the exposure time was a few seconds with a dispersion of 1.4
Å/mm.
We observed the absorption lines of Fe I at 15648.5 Å(Landè factor gL = 3) and derived the distribution of themagnetic field strengths and inclination angles across the sunspots. Figure 1 shows completely split Zeeman components
from a sunspot whose field strength was 2400 Gauss.

Reference[1] Sakurai, T., et al.: 2001, Publ. Astron. Soc. Japan, 53, 923.

34

Figure 1: The spectra of a sunspot (NOAA region 8747, 1999
November 3). The spectrum at the top panel has been divided by the intensity integrated over the wavelength, sothat the sunspot does not show up dark, but the location of
the spot is readily inferred by the large Zeeman splitting.
The bottom panel is a profile of the upper panel throughthe umbra. The tick marks shown at the Fe I 15648.5 Å ((ggL= 3) line on the left indicate a Zeeman splitting of each 1
kG. The line on the right is Fe I 15652.9 Å ((ggL = 1.53).

Flexible Prism Used as an Image Stabilizer
SAKURAI, Takashi(Solar Physics Division, NAOJ)NOGUCHI, Motokazu, SHINODA, Kazuya, TANAKA, Nobuyuki(Norikura Solar Observatory, NAOJ)

The image motion due to atmospheric turbulence (seeing)or vibration of a telescope degrades the quality of observed
images. An image stabilizer made of a small ‘tip-tilt’ mirror
is often used to compensate for the image motion. An inconvenient aspect of the tip-tilt mirror is that it bends the optical
path. Unless it is planned from the beginning, the existing
optical system has to be modified considerably to incorporate
the tip-tilt mirror.
We have developed a new image-stabilizing scheme byusing a flexible prism [1]. This kind of prism is now widelyused as an anti-vibration scheme in hand-held video cameras.
An advantage of this scheme is that we simply put the prism
into the existing optical path to correct for the image motion.
The prism we use as an image stabilizer is manufactured
by Canon (the registered brand name is ‘vari-angle prism’).
Canon produces a vibration-stabilized binocular equippedwith this prism. The aperture is 40 mm, and it responds tofrequencies up to 20 Hz.
Figure 1 shows the prism. The prism is made of twoplates of glass whose peripheries are connected by a bellows.
In the volume sealed by two glass plates and the bellows is
contained a liquid, so that the glass plates can be tilted. The
tilt axes of the two glass plates are oriented 90˚ from eachother, so that by properly tilting both glass plates, the lightbeam can be deflected to any direction within a few degrees.
The tilt of the prism is driven by two solenoid coils.
Figure 2 shows the performance of the prism tested on
the Solar Flare Telescope at Mitaka. Although the response
speed of 20 Hz is not fast enough to fully compensate for theseeing effect, it is effective in removing low frequency vibration of the telescope due to winds. The prisms have beenequipped on the Solar Flare Telescope since 1995.

Figure 1: The prism. The aperture is 40 mm.

Figure 2: Positions of the solar image from the telescopes without(left) and with (right) the prism, observed simultaneously.
The image motion was suppressed to less than 1˝ by theprism.

Reference[1] Sakurai, T., et al.: 2001, Solar Phys., 205, 201.

35

Interpolation of One- and Two-Dimensional Images
with Pixelwise Photon Number Conservation
SAKURAI, Takashi, SHIN, Junho(Graduate University for Advanced Studies/NAOJ)

The interpolation of one- and two-dimensional images is
considered. The usual linear or cubic-spline interpolations
try to connect given data points. On the other hand, image
data give area integrals of the radiation intensity (i.e. photon
counts) over pixels. Our problem in one-dimensional case is
to find an interpolating function y(x( ) which, after integration(x
over pixels, gives the prescribed photon counts.
We adopted the variational principle in which the linear andcubic-spline interpolations, respectively, minimize the energyof tension and bending. When the constraint of prescribedphoton counts is added by using the Lagrange’s multiplier,
we obtain the quadratic and fourth-order polynomials, respectively, as extensions of linear and cubic-spline interpolations.
A similar technique has been developed for two-dimensional
data. These methods were tested on some simple examples
and showed satisfactory results [1].

Reference[1] Sakurai, T., and Shin, J.: 2001, Publ. Astron. Soc. Japan, 53, 361.

36Figure 1: The dotted curves represent the original data, and the step
functions indicate the sampled data with an image detector. If one uses a simple cubic-spline interpolation (left),the difference between the original function and the interpolated curve is large. The quadratic (middle) and fourthorder (right) interpolations recover the observed photon
counts (represented by step functions) exactly. The difference between the original function and the interpolated
curves is small.

Chromospheric Magnetic Field of Solar Active Regions
CHOUDHARY, Debi Prasad(Udaipur Solar Observatory, India)

SAKURAI, Takashi(Solar Physics Division, NAOJ)

The three-dimensional structure of magnetic field of 137
solar active regions is studied by comparing the observed andcomputed chromospheric field. The data used are magnetograms of the photosphere and the chromosphere obtained at
NSO Kitt Peak. Chromospheric magnetograms are obtainedby observing the Ca II 8542 Å line, which is formed 800 km
above the photosphere. We computed the potential magnetic
field at this height by using the observed photospheric fieldas the boundary condition, and compared it with the observed
chromospheric field.
In the low field range, within ± 300 G, most of the observed field is close to the potential field. For field values
greater than ± 500 G, we frequently found large deviations
from the potential field. The long-lived active regions, whichmake multiple disk passages, show marked non-potentiality
during their initial phase. During the decaying phase they
converge to potential field configuration.
The deviation of the observed chromospheric field fromthe computed potential field extrapolated from the photosphere can be a good indicator for flare productivity of the region. This property can be useful in the framework of space
weather forecast and flare prediction.

Figure 1: The scatter plot of the photospheric (abscissa) and chromospheric (ordinate) magnetic field strengths in active
region NOAA 8821 on 12 January 2000. The black and red
dots are the observed and computed chromospheric fields,
respectively.

Reference[1] Choudhary, D. P., Sakurai, T., and Venkatakrishnan, P.: 2001,
Astrophys. J., 560, 439.

37

Radial distribution of molecular gas in galaxies
NISHIYAMA, Kota, NAKAI, Naomasa, KUNO, Nario(Division of Radio Astronomy, NAOJ)

We have studied the distribution and dynamics of molecular gas in galaxies by observing CO emission mainly along
the major and minor axes of 28 nearby spiral galaxies withthe 45-m telescope of the Nobeyama Radio Observatory. The
observations showed that the surface density of molecular gas
indicates an exponential distribution in the region of the flat
(differential) rotation curve for all the galaxies. This could
be because the radial distribution is determined by gas inflow
due to the viscosity of molecular clouds. The surface densityof molecular gas in barred galaxies also shows a characteristic distribution in the region of the bar, suggesting gas inflow
along the bar by the bar potential and perpendicular to thebar by viscosity. Such a transfer of molecular gas increases
the gas density in the central region, probably causing theevolution of the rotation curve, which is determined by themass distribution, on the time scale of the galaxy age. We
compared the radial distribution of the surface density of HI
with that of H2, and found same scale length of the exponential distribution in the Virgo galaxies and a much larger scale
length in field galaxies for HI. This could be due to a difference in the viscosity coefficient of the HI gas.

References[1] Nishiyama, K., and Nakai, N.: 2001, PASJ,
PASJ 53, 713.
[2] Nishiyama, K., Nakai, N., and Kuno, N.: 2001, PASJ,
PASJ 53, 757.

38

Figure 1: Radial distributions of the total gas (H2 + HI) of molecularand atomic gas in non-Virgo galaxies (upper) and Virgogalaxies (lower). The blue and red lines indicate the H2and HI-dominated regions, respectively.

Discovery of a water megamaser
in a starburst galaxy NGC 6240
NAKAI, Naomasa(Division of Radio Astronomy, NAOJ)

SATO, Nahoko(NAOJ/Hokkaido University)

We detected a water-vapor maser emission in a prototypical ultraluminous FIR galaxy with an AGN, NGC 6240. The
flux density of the detected maser line was SS=96 mJy at a distance of 100 Mpc, which is typical for water megamaser. The
maser line was redshifted by 204 km/s relative to the systemic
velocity of the galaxy, while no systemic velocity feature was
detected. The previous observed upper limits were at a level
lower than the present flux density, indicating that the water

YAMAUCHI, Aya(NAOJ/Kyushu University)

maser in NGC 6240 flared up by more than a factor of 5 in2001.
References[1] Braatz, J. A., Wilson, A. S., and Henkel, C.: 1996, ApJS, 106, 51.
[2] Claussen, M. J., and Lo, K.-Y.: 1986, ApJ,
ApJ 308, 592.
[3] Henkel, C. et al.:1984, A&A, 141, L1.
[4] Nakai, N., Sato, N., and Yamauchi, A.: 2002, PASJ,
PASJ 54, L27.

Figure 1: Water-vapor maser spectrum of NGC 6240 measured with the 45-m telescope of the Nobeyama Radio Observatory.
The arrow indicates the systemic velocity of the galaxy.

Figure 2: Peak flux densities of the water-vapor maser emission from NGC 6240 measured until 2001. [1] [2] [3] [4]The unfilled circle indicates a possible detection in 1984 September [3] and the filled circle the present result. The upper limits are 3 rms.

39

Spectroscopic Studies of r-Process Elements in Extremely
Metal-Poor Stars with Subaru HDS and Cosmochronometry
HONDA, Satoshi, AOKI, Wako, ANDO, Hiroyasu, NOGUCHI, Kunio(Division Optical and Infrared Astronomy, NAOJ)

KAJINO, Toshitaka(Theoretical Astrophysics Division, NAOJ)

We obtained high resolution ((R = 50,000 ~ 90,000), highquality (S/N = 50 ~ 400) spectra of 22 metal-poor stars for
precise abundance studies with High Dispersion Spectrograph(HDS) fabricated for the Subaru Telescope.
We found that Mg, Si, Ca, and Ti show overabundances
compared with Fe, and the abundances of iron-peak elements
show small dispersion. Compared with the abundances ofthese elements, those of neutron-capture elements show large
dispersion as found by previous studies. The dispersion canbe interpreted as a result of incomplete mixing of the interstellar medium at the beginning of the Galaxy formation.
The Ba to Eu ratios in metal-poor stars observed in our
program are nearly equal to that of the solar system r-processcomponent. This result proves that these elements are primarily synthesized by r-process. The abundance patterns of
the heavy neutron-capture elements (56 ≤ Z ≤ 69) in sevenobjects with excesses of the neutron-capture elements are
similar to that of the solar system r-process component.
However, the abundance patterns of neutron-capture elements(56 ≤ Z ≤ 69) in two of them show significant deviation fromthat of the solar system r-process component, which can not
be explained only by the uncertainty of the analysis. This
result suggests that s-process nucleosynthesis contributs tothe production of neutron-capture elements in these objects,
or small variation exists in the abundance pattern of elements
produced by the r-process in the range of 56 ≤ Z ≤ 69. On
the other hand, the abundance ratios of light neutron-capture
elements (38 ≤ Z ≤ 46) to heavier ones (56 ≤ Z ≤ 69) show alarge dispersion. This result supports previous suggestions
that the light neutron-capture elements have been produced in40

the different sites from those for heavy ones.
The abundance ratio of the radio-active element Th (ZZ=90) to stable one (e.g., Eu) in very metal-poor stars has beenused as a cosmochronomter in some previous works. Th isdetected in seven stars in our sample. The Th/Eu abundance
ratios ([Th/Eu]) distribute from −0.30 to −0.67. These values correspond to the ages of only a few or zero Gyrs, when
we assume the initial Th/Eu abundance ratio is the same asthat of the solar system. These are too short as the ages ofvery metal-poor stars, which are believed to be formed in theearly Galaxy. This result means that the universality of theabundance pattern of the neutron-capture elements can not be
extended to Th (ZZ = 90) by using the solar system r-processcomponent. Th/Eu is not a good chronometer for metal-poorstars.

Figure 1: Scaled abundances in our objects compared with the solar
system r-process compornent.

Small Fluctuation of Coronal X-Ray Intensity :Possibility of Nanoflare Heating
KATSUKAWA, Yukio(University of Tokyo/NAOJ)

Small flare (“nanoflare”) is one of the possible mechanisms to heat the solar corona, in which many energeticallysmall transient events continuously occur and heat the corona.
A simple method to probe the nanoflare heating scenario iscounting of transient events such as flares and microflares observed in X-rays and EUV. Energy of each event and occurrence rate give total heat input into the corona by such events.
Many works have been performed until now, and showed thatevents which can be identified as discrete ones (energy ranges
from 1024 to 1033 erg) do not supply enough energy to heat
the corona. Thus, it is important to investigate whether muchsmaller energy events occur more frequently. However, suchtiny events may be unable to be identified as discrete events,
and new approaches are required.
In this work, we suggest a new but simple approach toanalyze time variation of the corona. We extract persistentcomponent in time profiles of X-ray intensity, and calculatemean intensity. Then, we make histograms about deviationfrom the mean intensity. Fluctuation of the X-ray intensity
can be characterized quantitatively by the width of the histograms. If the histograms are broader than noise distribution,
it means that X-ray intensity fluctuates and tiny events are occurring in the corona.
We use images of an active region obtained by Yohkoh
Soft X-ray Telescope (SXT)(Figure 1) in this analysis. The
histograms mentioned above are made for different intensity
levels (Figure 2). The histograms are found to consist of two
components; Gaussian-like distribution around the center,
which corresponds to random fluctuation around the mean
intensity, and wing component, which corresponds to systematic time variation of X-ray intensity. Since we are hereinterested in small fluctuation around the mean intensity, we
extract the central Gaussian-like component, and measure
the width of the histograms. Of course, noises of SXT cause
false fluctuation. We evaluate all noise sources accurately,
and compare the observed histogram width with the predicted
noise level.
In dark regions (Figure 2[a]), the fluctuation of X-ray in-

TSUNETA, Saku

(Solar Physics Division, NAOJ)

tensity is almost due to the noise. On the other hand, the histogram in bright regions (Figure 2[b]) is found to be broader
than the predicted noise distribution. This means that somefluctuating sources exist in the solar corona. We attributethe observed small fluctuation to the signature of nanoflares.
We also estimate the energy of nanoflares from the observed
fluctuation of X-ray intensity. The estimated energy is about
1020 erg, and is much smaller than the energy of theoretically
predicted nanoflares (1024 erg).

Figure 1: Soft X-ray image of an active region obtained by
Yohkoh (left), and sample light-curves of the X-ray intensity (right).

Figure 2: Histograms of the X-ray intensity. (a) is for dark regions,and (b) is for bright regions. The dashed curves show thepredicted noise distribution.

Reference[1] Katsukawa, Y., and Tsuneta, S.: 2001, ApJ,
ApJ 557, 343.
41

Lithium isotopic ratio in interstellar media
KAWANOMOTO, Satoshi, ANDO, Hiroyasu(Division of Optical and Infrared Astronomy, NAOJ)SUZUKI, Ken, Takeru(University of Tokyo/Division of Theoretical Astrophysics, NAOJ)

KAJINO, Toshitaka(Division of Theoretical Astrophysics, NAOJ)

Although most of metals in the universe are synthesizedby nuclear reactions in the interior of stars, the light elements
like Lithium are synthesized by Big-Bang nucleosynthesis,
spallation reactions in interstellar media, nova nucleosynthesis, and supernova nucleosynthesis. Light elements aredestroyed easily inside stars. Therefore Lithium is the mostimportant element for studies of the Big-Bang theory, theGalactic chemical evolution, and structure of stars. It should
be noted that there are two stable isotopes 7Li and 6Li withdifferent characters. 7Li is synthesized by the Big-Bang nucleosynthesis, but 6Li is rarely created in Big-Bang. Becauseof this difference, the isotopic ratio of Litnium varies depending on the location and time. We tried to observe interstellar
absorption lines in order to derive the isotopic ratio.

Figure 1: Sample spectrum of HD169454 Li I and K I.

42

In the early observations of Subaru-HDS (High Dispersion Spectrograph), we obtained some spectra of interstellar
absorption lines including λ =6708Å Lithium lines as a test
observation for high spectral dispersion and high signal-tonoise ratio. From these data and additional data obtained at
Okayama Astrophysical Observatory, we derived the lithium
isotopic ratio for directions of three stars, χ 2−Ori, HD169454,
HD250290. A sample spectrum is shown in Figure 1. Distances of these stars are about 1.5kpc. We derived the lithium
isotopic ratio for these stars.
On the basis of our results together with the data of 7Li/6Li
so far reported for the local ISMs in the solar neighborhood,
we attempted to determine the primordial 7Li abundance byusing the GCE model, taking into account its galactocentric
distance dependence. In Figure 2, we show the galactocentric
distance dependence of 7Li/6Li. Using these data, we obtained the upper limit of primordial lithium abundance, 7Li/H< 8 × 10−10. This is the first result of primordial lithium abundance determined without using observations of population II
stars.

Figure 2: Plot of 7Li/6Li vs. galactocentric distance of backgroundstars with best fit model calculation. Our new data (filled
circle), previously reported data (open circle), and a model
calculation (solid line) with error region (shaded area) are
shown.

Revision of Ephemeris Yearbook (Rekishoh-Nenpyoh)
FUKUSHIMA, Toshio, NAKAI, Hiroshi, ITO, Setsuko(Public Relations Center, Ephemeris Computation Office)

The Ephemeris Computation Office of the Public Relations Center, NAOJ, has conducted the computation of aJapanese civil almanac named Ephemeris Yearbook, or Rekishoh-Nenpyoh in Japanese. The Yearbook contains the dateof vernal and autmunal equinoxes, the apparent positions of
the Sun, the Moon, and major planets, the information on thesolar and lunar eclipses and planetary phenomena, and otherephemeris issues. This work is to comply with the preparation of ephmerides, one of the legal missions charged to theobservatory.
Since the last major revision on 1985, the advent of observational techniques and the rapid increase of observational
data both in quality and in quantity have spurred the creationof better lunar/planetary ephemerides as well as the latest
nutation theories. Also it has been well acknowledged that
the Tokyo Datum, the basic set of Japanese geodetic systemused since the Meiji era, has non-negligible difference fromthe so-called world geodetic systems thanks to the GPS andother precision measurement techniques in space geodesy.
Then the Japanese Government recently replaced the Datum
by a new one based on a recent ITRF by modifying the lawof surveying, which automatically requires the adopted values of latitude and longitude of some representative positions
listed in the Ephemeris Yearbook. Accounting these situation
and requirements, we have updated the basic theories of theEphemeris Yearbook from the year of 2003. The major revi-

Figure 1a: DE405−DE200 (Sun)Figure 1b: DE405−DE200 (Pluto)

43sions are as follows.
1. Revision of Lunar/Planetary Ephemeris
As for the position and velocity of the Sun, the Moon, andmajor planets, we replaced the current basis, DE200/LE200
of NASA/JPL, by its latest version, DE405/LE405 (Standish
1998). The accuracy of the latter is estimated as small as 1
mas for the apparent position of inner planets. At the sametime, the fundamental reference frame of the Yearbook waschanged from the classic one, that based on the mean equinox
and equator at J2000.0, to the International Celestial Reference Frame, the IAU official reference frame defined by theset of positions of quasars. Also the system of astronomical

constants has been changed to that adopted in DE405/LE405,
which is quite close to the IAU 2000 Best Estimates of Astronomical Constants. This change introduced some small
differences as shown in Figs. 1a and 1b. The figures illustrate
the differences in the right ascension, the declination, and thegeocentric distance of the Sun and Pluto between DE405 andDE200.
2. Revision of Nutation Theory
As for the nutation theory, we replaced the IAU 1980
theory to SF2001 (Shirai and Fukushima 2001). The latter
was created by fitting to the VLBI observations of the Earthpole offsets in the last 20 years and includes a correction to
the IAU 1976 precession formula. Fig.2 shows the differenceof the IAU 1980 nutation theory and SF2001. The difference of SF2001 from the other latest nutation theories such as
IAU2000A are small as less than 1.5mas in longitude and 0.6
mas in obliquity for the forthcoming 20 years.
3. Revision of Geodetic System
To be conformal with the modification of the laws of
the surveying and the hydrographic duties adopted by theCongress in June, 2001, and enforced on April 1st, 2002, werevised the data of geodetic system such as the radius and theflattening factor of the Earth and the longitude and latitude ofmany landmarks in Japan.
4. New Form of Expression
In order to enable to obtain more precise values of the nutations and the equation of equinox, we changed their tabulation stepsize from 10 days to 4 days.

References[1] Ephemeris Yearbook (2003): 2002, NAOJ.
NAOJ[2] Shirai, T., and Fukushima, T.: 2001, AJ,
AJ 121, 3270–3283.
[3] Standish, E.M.: 1998, JPL Planetary and Lunar Ephemerides,
IOM 312. F-98-048.

Figure 2: SF2001−IAU1980

44

When did the Hubble Sequence Appear ?
YAMADA, Toru

(Division of Optical and Infrared Astronomy, NAOJ)

We are conducting observational study to reveal overall
history of structure formation in the universe. In this year we
worked on the Subaru deep NIR data as well as HST archived
data of the Hubble Deep Field North [1][2].
First, with the HST NICMOS deep imaging data, we construct a volume-limited complete sample of galaxies up to z =2 with M
Mv < −20 and investigated their evolution. We foundthat (i) there are about 100 galaxies with M
Mv < −20 and z < 2
in HDF-N, (ii) the commoving density of bulge-dominatedgalaxies rapidly decrease above z = 1, and (iii) rest-opticalflux of disk galaxies at z > 1.5 is completely dominated by theyoung stars formed in on-going star formation. The Hubble
sequence clearly appears up to z = 1 but conspicuously
changes above the redshift.
We then conducted extremely deep NIR imaging with
Subaru to study the rest-frame optical properties of the galaxies at z > 2. We found that many galaxies at z > 2 in HDF-N (i)have no clear morphological sequence, (ii) have stellar mass
significantly smaller than the typical L* galaxies at z = 0, and(iii) rest-optical flux is dominated by young stars.
In HDF-N, massive galaxies which form the Hubble sequence have not been formed yet and they appeared as they
are around z ~ 1. Using the upcoming data taken for the
Subaru Observatory project, we will study how these are general trend in the universe.

KAJISAWA, Masaru(NAOJ / Tohoku University)

Figure 1: A complete sample of bulge-dominated galaxies at z < 2

Figure 2: A complete sample of disk-dominated galaxies at z < 2

Figure 3: (left) Rest-UV morphology of a galaxy at z = 3.4 with
HST. (right) Rest-optical morphology of the galaxy with
CISCO

References[1] Kajisawa M. and Yamada T.: 2001, PASJ.,
PASJ 58, 833.
[2] Yamada T. and Kajisawa M.: 2001, in “Mass of Galaxies at Low
and High Redshift” in press.

Figure 4: Observed stellar mass distribution of galaxies at z > 2

45

Bicolour Lightcurve of TNO 1996 TO66 with the ESO-VLTSEKIGUCHI, Tomohiko

BOEHNHARDT, Hermann(Division of Radio Astronomy, NAOJ)(Eouropean Southern Observatory)

HAINAUT, O. R.

DELAHODDE, C. E.

(Eouropean Southern Observatory)(Institut d'Astrophysique de Marseille)

Abstract
We performed high resolution imaging of 1996 TO66 in
V and R band to verify and monitor the lightcurve change,
to address a colour change over a rotation and to search
for a cometary activity. No activity was detected at the 29
mag/sq.arcsec level with 5400s integration time with the
ESO-VLT. Combining the data in Nov. and Dec. 1999, we
obtained a complete rotation period coverage. The lightcurve was a single-peaked, with an amplitude of 0.21 mag in
R. The (VV − R) colour displays the inhomogeneity of TNO
surface. TNO’s patchy surface may be caused the intensitychange of water absorption feature in near-IR spectra. Theseobservations can be the starting points for a challenging workof surface mapping of TNOs.
Summary
The main results of this study are the following:• 1996 TO66 is one of the largest TNO. The derived diameter is 600−700 km assuming 0.04 albedo.
• Our data are consistent with the 6.25 hr rotation period.
• No resolved coma was detected down to 29 mag/sq.arcsec
on a 5400s composite R exposure.
• The (V−R) colour of 1996 TO66 has neutral colour overa rotation in general but a small bump around the rotation
phase of 0.4 may indicate a change in the colour gradientof the surface material. This supports the inhomogeneous
surface material and reflectivity as reported by Brown et al.
(1999) and Hainaut et al. (2000).
These results come to the starting points for a work of
surface mapping of TNOs as Pluto.

Figure 1: The R-band images of 1996 TO66 in November, 1999,
with an effective integration time of 5400s. 1996 TO66 in
the center and the star appear trailed because the images
have been shifted to cancel out the motion of the TNO.
51” × 51”.

References[1] Hainaut, O. R., Delahodde, C. E., Boehnhardt, H. et al.: 2000,
Astron. & Astrophys., 356, 1076.
[2] Brown, R. H., Cruikshank, D. P. & Pendleton, Y.: 1999, Astrophys. J., 519, L101.

46

Figure 2: Phased lightcurve of 1996 TO66 in V and R-band foldedwith 6.25 h period.

Probing Dark Matter Substructure in Lens Galaxies
CHIBA, Masashi(Division of Astrometry and Celestial Mechanics, NAOJ)

The cold dark matter (CDM) scenario for structure formation in the universe has been quite successful in explaining awide variety of observational results, including characteristic
fluctuations of the cosmic microwave background and largescale structure of galaxies on scales larger than ~ 1 Mpc. The
currently best world model, which accords with the results ofmany cosmological observations, consists of approximately
30 % CDM and 70 % vacuum energy or quintessence. However, the recent advent of high-resolution N
N-body simulations
on CDM-based structure formation has enabled to highlightvarious discrepancies with existing observations on scales
smaller than ~ 1 Mpc. One of the most serious issues is that
CDM models predict the existence of several hundred clumps
or “subhalos” in a galaxy-sized halo, in sharp contrast to theobserved number of about dozen Milky Way satellites.
To assess the existence of such numerous CDM subhalos
in a galaxy-sized halo, we investigate their effects on theevents of strong lensing. Lens galaxies are represented bya smooth ellipsoid in an external shear field and additional
CDM subhalos taken from Monte Carlo realizations whichaccord with recent N
N-body results. We also consider otherpossible perturbers, globular clusters and luminous dwarf
satellites, for comparison. We then apply the models to theparticular lens systems with four images, B1422 + 231 and
PG1115 + 080, for which smooth lens models are unable toreproduce both the positions of the images and their radio
flux ratios or dust-free optical flux ratios simultaneously. We
show that the perturbations by both globular clusters anddwarf satellites are too small to change the flux ratios, whereas CDM subhalos are most likely perturbers to reproduce theobserved flux ratios in a statistically significant manner (Figure 1). This result suggests to us the presence of numerous
subhalos in lens galaxies, which is consistent with the resultsof cosmological N
N-body simulations.

Figure 1: The probability distributions of the flux ratios for B1422 +
231 (left panels, in units of flux B) and for PG1115 + 080(right panels, in units of flux A1). Upper panels show thecases of globular clusters (dashed lines) and dwarf satellites (solid lines) as perturbers, whereas lower panels show
the case of CDM subhalos. Solid bars denote the observed flux ratios of A/B and r ≡ (A+B+C(A+B+C)/(
A+B+C)/(|A|+|B|+|C|)for B1422 + 231 and A2/A1 for PG1115 + 080.

Reference[1] Chiba, M.: 2002, Astrophys. J., 565, 17-23.

47

Sensitivity of an imaging space infrared interferometer
NAKAJIMA, Tadashi(Division of Optical and Infrared Astronomy, NAOJ)

MATSUHARA, Hideo(ISAS)

Early in the 21st century space infrared observatories
such as ASTRO-F, SIRTF, FIRST, and SPICA are planned to
study the formation of planets, stars, and galaxies. The improvement in sensitivity is so great that the source-detection
limits of these space observatories are expected to be set bysource confusion, especially in the far infrared. To improvefurther the source detection limits, individual sources need
to be resolved by an infrared interferometer. Therefore it isimportant to quantify the sensitivity of a space infrared interferometer for the purpose of aperture synthesis imaging.
Following the observatories, space infrared interferometers such as TPF and Darwin are considered, with an emphasis on the detection of terrestrial planets around nearby stars.
TPF and Darwin will consist of several radiation cooled
apertures and will be capable of synthesis imaging as well
as planet detection by nulling interferometry. The detection
limits of these interferometers for general purpose imaging
are of great interest. Among many applications of synthesis
imaging with space infrared interferometer, we are interested
particularly in deep galaxy count by which the history ofgalaxy formation can be studied. We discuss how a TPF likeinterferometer operated in the far infrared can improve thenumber count data of high-redshift galaxies.
We first formulate the signal-to-noise ratios of infrared
images obtained by aperture synthesis in the presence ofsource shot noise, background shot noise, and detector readnoise. We consider the case in which n beams are combined
pairwise at n(n−1)/2 detectors and the case in which all the nbeams are combined at a single detector.
We obtain the detection limits of separated spacecraft interferometers such as the TPF and Darwin in the presence of48

the natural thermal background as functions of wavelength.
The comparison of a TPF-like interferometer with NGST,
SPICA, and FIRST reveals that at λ > 100 µ m, an interferometer is more sensitive than SPICA or FIRST. This is true with
only radiation cooling of the apertures.

Figure 1: Comparison with monolithic observatories. The sensitivity of an interferometer composed of four 3.5-m aperturesis plotted for telescope temperatures of 5, 10, 20, and
40 K with an emissivity of 5%. The maximum baseline
length is assumed to be 100 m. The dashed curves denotethe sensitivities of NGST, SPICA, and FIRST that are
given for comparison.

Reference[1] Nakajima, T., and Matsuhara, H.: 2001, Applied Optics, 40, 514.

CCD Photometry of the MUSES-C Mission Target:
Asteroid (25143) 1998 SF36
DERMAWAN, Budi

(School of Science, Univ. of Tokyo)

NAKAMURA, Tsuko, FUKUSHIMA, Hideo, SATO, Hideo, YOSHIDA, Fumi
(Division of Optical and Infrared Astronomy, NAOJ)

SATO, Yusuke(Graduate School of Education, Tokyo Gakugei Univ.)

We conducted extensive photometric observations using
0.5-m telescope equipped with CCD camera of 1152 × 770
pixels at NAO-Mitaka from 2001 February 15 until March 19,
covering phase angle (α ) of 20.7˚−36.5˚, to obtain the physical properties of Near-Earth Asteroid (25143) 1998 SF36.
The asteroid is now planned as the target for the Japanese
MUSES-C sample return mission, so that detailed knowledgeof physical characteristics of this asteroid is very essential forthe success of this mission. Photometric data ((III-band)-band) weresuccessfully taken for 13 nights, while colorimetric observation was attempted on March 18 using BVRI bands.
We revealed several physical properties such as asteroid's
colors, rotation period, phase curve, and lightcurves. We obtained the asteroid's colors (without solar colors substraction):
(B−V
(B−V
B−V)) = 0.902 ± 0.042, (V−R) = 0.475 ± 0.039, and (V−I)
V−I) =
V−I
0.725 ± 0.012. This implies that the type of this asteroid isclose to the S-type, though it does not seem to be a typical
S-type, judging from its location of the color diagram shownin figure 1. In order to find the rotation period of this asteroid, we employed the Phase Dispersion Minimization technique and the Fourier-transform method. A resulting spin period of this asteroid is found to be 12.13 ± 0.02 hr. We also
calculated the asteroid absolute magnitude ((HH)) and the slope
H(G) for the two-parameter magnitude system derived from theasteroid’s phase curve. We thus obtained H = 18.61 ± 0.18, G= 0.29 ± 0.14, and the estimated albedo is to be 0.29−0.08+0.09 . We
suggest that this albedo may be higher than that for the typical S-type asteroids. After employing the phase-angle dependence on the light-curve, we could eventually make a composite light-curve by applying the Fourier analysis method
shown in figure 2 for α = 20.8˚. We made clear that the peak~ 0.49 mag,to-peak amplitude at zero phase angle A (0˚) −which implies that the minimum ratio of the longest and intermediate axes is 1.6.
Reference[1] Dermawan, B., Nakamura, T., Fukushima, H., Sato, H., Yoshida,F., Sato, Y. : 2002, Publ. Astron. Soc. Japan, 54, in press.

Figure 1: Obtained asteroid colors (marked with error bars) in color
diagrams (V−I)
V−I) vs (V−R)) on the upper panel and ((B−V
V−I
B−V)) vs
B−V
(V−R) on the lower one. The letters denote the asteroid's
type. The asteroid data are taken from the Eight-Colors
Asteroid Survey (ECAS).

Figure 2: Composite light-curve of the asteroid at α = 20.8˚. The
observed data points are given with error bars and folded
into the rotational phase with the period of 12.13 hr basedon 2001 February 15.56588.
49

II Publications, Presentations
1. Refereed Publications
Akabane, K., Matsuo, H., Kuno, N., Sugitani, K.: 2001, 2Millimeter Dust around NGC 7538-IRS 1, 2 and 3. I.
Unfilled Structure of Dust Cloud, Publ. Astron. Soc. Japan, 53, 821‑832. (NROR. 545)
Akiyama, M., Ueda, Y., and Ohta, K.: 2002, A Candidate ofa Type 2 Quasi-stellar Object at z=0.9: Large X-Ray Absorption with a Strong Broad Hα Emission Line, Astrophys.
J., 567, 42‑49.
Ando, M., Arai, K., Takahashi, R., Heinzel, G., Kawamura,S., Tatsumi, D., Kanda, N., Tagoshi, H., Araya, A., Asada,
H., Aso, Y., Barton, M. A., Fujimoto, M. K., Fukushima,M., Futamase, T., Hayama, K., Horikoshi, G., Ishizuka,
H., Kamikubota, N., Kawabe, K., Kawashima, N.,
Kobayashi, Y., Kojima, Y., Kondo, K., Kozai, Y., Kuroda,K., Matsuda, N., Mio, N., Miura, K., Miyakawa, O.,
Miyama, S. M., Miyoki, S., Moriwaki, S., Musha, M.,
Nagano, S., Nakagawa, K., Nakamura, T., Nakao, K.,
Numata, K., Ogawa, Y., Ohashi, M., Ohishi, N., Okutomi,
S., Oohara, K., Otsuka, S., Saito, Y., Sasaki, M., Sato, S.,
Sekiya, A., Shibata, M., Somiya, K., Suzuki, T., Takamori,A., Tanaka, T., Taniguchi, S., Telada, S., Tochikubo, K.,
Tomaru, T., Tsubono, K., Tsuda, N., Uchiyama, T., Ueda,
A., Ueda, K., Waseda, K., Watanabe, Y., Yakura, H.,
Yamamoto, K., Yamazaki, T.: 2001, Stable Operation of
a 300-m Laser Interferometer with Sufficient Sensitivity
to Detect Gravitational-Wave Events within Our Galaxy,Phys. Rev. Lett., 86, 3950‑3954.
Aoki, W., Norris, J. E., Ryan, S. G., Beers, T. C., and Ando,H.: 2002, The Chemical Composition of Carbon-rich,
Very Metal Poor Stars: A New Class of Mildly Carbon
Rich Objects without Excess of Neutron-Capture Elements, Astrophys. J., 567, 1166.
Aoki, W., Ryan, S. G., Norris, J. E., Beers, T. C., Ando, H.,
Iwamoto, N., Kajino, T., Mathews, G. J., and Fujimoto,
M. Y.: 2001, Neutron Capture Elements in s-Process-Rich,
Very Metal-Poor Stars, Astrophys. J., 561, 346.
Aoyama, Y. and Naito, I.: 2001, Atmospheric excitation of
the Chandler wobble, 1983‑1998, J. Geophys. Res., 106,8941‑8954.
Arai, K., and the TAMA collaboration: 2002, Sensing andcontrols for power-recycling of TAMA300, Class. Quantum Grav., 19, 1843.
Asai, A., Shimojo, M., Isobe, H., Morimoto, T., Yokoyama,T., Shibasaki, K., and Nakajima, H.: 2001, Periodic
Acceleration of Electrons in the 1998 November 10 Solar
Flare, Astrophys. J. Lett., 562, L103‑L106.
Aurass, H., Shibasaki, K., Reiner, M., and Karlicky, M.:
2002, Microwave Detection of Shock and Associated Electron Beam Formation, Astrophys. J., 567, 610‑621.
Baba, H., Sadakane, K., Norimoto, Y., Ayani, K., Ioroi, M.,
Matsumoto, K., Nogami, D., Makita, M., and Kato, T.:
2002, Spiral Structure in WZ Sagittae around the 2001
Outburst Maximum, Publ. Astron. Soc. Japan, 54, L7‑

L10.
Baba, H., Sadakane, K., Norimoto, Y., Nogami, D.,
Matsumoto, K., Makita, M., and Kato, T.: 2001, WZ
SAGITTAE, IAUC, 7678.
Baba, H., Sadakane,K., and Norimoto,Y.: 2001, WZ
SAGITTAE, IAUC, 7672.
Bekki, K., and Chiba, M.: 2001, Formation of the Galactic
Stellar Halo I. Structure and Kinematics, Astrophys. J.,
558, 666‑686.
Bekki, K., and Chiba, M.: 2002, Formation of Galactic Disk
Globular Clusters in Early Dissipative Minor Merging,Astrophys. J., 566, 245‑251.
Boehnhardt, H., Tozzi, G. P., Birkle, K., Hainaut, O.,
Sekiguchi, T., Vair, M., Watanabe, J., Rupprecht, G.,
and The FORS Instrument Team: 2001, Visible and nearIR observations of transneptunian objects. Results from
ESO and Calar Alto Telescopes, Astron. Astrophys., 378,
653‑667.
Carter, D., Mobasher, B., Bridges, T. J., Poggianti, B. M.,
Komiyama, Y., Kashikawa, N., Doi, M., Iye, M.,
Okamura, S., Sekiguchi, M., Shimasaku, K., Yagi, M.,
Yasuda, N.: 2002, A Photometric and Spectroscopic Studyof Dwarf and Giant Galaxies in the ComaCluster. V. Dependence of the Spectroscopic Properties on Location in
the Cluster, Astrophys. J., 567, 772.
Chernov, G. P., Fu, Q. J., Lao, D. B., and Hanaoka, Y.:
2001, Ion-Sound Model of Microwave Spikes with Fast
Shocks in the Reconnection Region, Solar Physics, 201,
153‑180.
Chiba, M.: 2002, Probing Dark Matter Substructure in Lens
Galaxies, Astrophys. J., 565, 17‑23.
Deguchi, S., Fujii, T., Matsumoto, S., Nakashima, J., andWood, P. R.: 2001, Near-Infrared Observations of IRAS
Sources with SiO Masers at the Inner Galactic Bulge,
Publ. Astron. Soc. Japan, 53, 293‑304.
Deguchi, S., Fujii, T., Miyoshi, M., and Nakashima, J.:
2002, Observation of SiO Maser Sources within a Few
Parsec from the Galactic Center, Publ. Astron. Soc. Japan,
54, 61‑71. (NROR. 548).
Deguchi, S., Nakashima, J., and Balasubramanyam, R.:
2001, SiO Maser Survey of Southern IRAS Sources, Publ.
Astron. Soc. Japan, 53, 305‑314.
‥
Dickens, J. E., Irvine, W. M., Nummelin, A., Mollendal,
H.,
Saito, S., Thorwirth, S., Hjalmarson, Astrophys., andOhishi, M.: 2001, Searches for New Interstellar Molecules, including a Tentative Detection of Aziridine and apossible Detection of Propenal, Spectrochimica Acta, PartA, 57, 643‑660.
Doi, M., Furusawa, H., Nakata, F., Ouchi, M., Yasuda, N.,
Miyazaki, S., Kashikawa, N., Komiyama, Y., Ohyama,Y., Yagi, M., Aoki, K., Hook, I., Perlmutter, S., Aldering,G.: 2001, Supernovae 2001cq, 2001cr, 2001cs, 2001ct,
2001cu, 2001cv, 2001cw, IAUC, 7649.
Ebisuzaki, T., Makino, J., Tsuru, T. G., Funato, Y., Zwart, S.
P., Hut, P., McMillan, S., Matsushita, S., Matsumoto, H.,
51

and Kawabe, R.: 2001, Missing Link Found? the "Runaway" Path to Supermassive Black Holes, Astrophys. J.
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Enoki, M., Takahara, F., and Fujita, Y.: 2001, Effects ofFormation Epoch Distribution on X-Ray Luminosity andTemperature Functions of Galaxy Clusters, Astrophys. J.,
556, 77‑86.
Enomoto, R., Hara, S., Asahara, A., Bicknell, G. V., Edwards,
P. G., Gunji, S., Hara, T., Jimbo, J., Kajino, F., Katagiri,
H., Kataoka, J., Kawachi, A., Kifune, T., Kubo, H.,
Kushida, J., Matsubara, Y., Mizumoto, Y., Mori, M.,
Moriya, M., Muraishi, H., Muraki, Y., Naito,T., Nakase,T., Nishijima, K., Okumura, K., Patterson, J. R.,
Sakurazawa, K., Swaby, D. L., Takano, K., Tanimori, T.,
Tamura, T., Tsuchiya, K., Uruma, K., Yanagita, S.,
Yoshida, T., Yoshikoshi, T., Yuki, A.: 2002, Design studyof CANGAROO-III, stereoscopic imaging atmospheric
Cherenkov telescopes for sub-TeV γ -ray detection,
Astropart. Phys., 16, 235‑244.
Famiano, M., Vandegriff, J., Boyd, R. N., Kajino, T., and2
3
7
Osmer, P.: 2001, Production of H, He and Li fromInteractions between Jets and Clouds, Astrophys. J. Lett.,
547, L21‑L24.
Fujita, Y., and Sarazin, C. L.: 2001, Nonthermal Emission
from Accreting and Merging Clusters of Galaxies,
Astrophys. J., 563, 660‑672.
Fujita, Y.: 2001, Ram-Pressure Stripping of Galaxies in
High-Redshift Clusters and the Influence of Intracluster
Medium Heating, Astrophys. J., 550, 612‑621.
Fukushima, H.: 2001, Comet C/2000 WM-1 (LINEAR),
IAUC, 7764, 3.
Furusho, T., Yamasaki, N. Y., Ohashi, T., Shibata, R., andEzawa, H.: 2001, Temperature Map of the Perseus Cluster of Galaxies Observed with ASCA, Astrophys. J. Lett.,
561, L165‑L169.
Furusho, T., Yamasaki, N., Ohashi, T., Shibata, R., Kagei,T., Ishisaki, Y., Kikuchi, K., Ezawa, H., and Ikebe, Y.:
2001, ASCA Temperature Maps of Three Clusters of
Galaxies: Abell 1060, AWM 7, and the Centaurus Cluster, Publ. Astron. Soc. Japan, 53, 421‑432.
Furuya, R. S., Kitamura, Y., Wootten, H. A., Claussen, M. J.,
and Kawabe, R.: 2001, Water Mass Survey towards LowMass Young Stellar Objects in the Northern Sky: Observational Constraints on Maser Excitation Conditions,Astrophys. J. Lett., 559, L143‑L147. (NROR. 542)
Fynbo, J. U., Gorosabel, J., Dall, T. H., Hjorth, J., Pedersen,‥
H., Andersen, M. I., Moller,P., Holland, S., Smail, I.,
Kobayashi, N., Rol, E., Vreeswijk, P., Burud, I., Jensen,
B. L., Thomsen, B., Henden, A., Vrba, F., Canzian, B.,
Castro Cero'n, J. M., Castro-Tirado, A. J., Cline, T., Goto,
M., Greiner, J., Hanski, M. T., Hurley, K., Lund, N.,‥Pursimo, T., Ostensen, R., Solheim, J., Tanvir, N., andTerada, H.: 2001, The optical afterglow and host galaxyof GRB 000926, Astron. Astrophys., 373, 796‑804.
Goto, M., Kobayashi, N., Terada, H., Gaessler, W.,
Kanzawa, T., Takami, H., Takato, N., Hayano, Y.,
Kamata, Y., Iye, M., Saint-Jacques, D. J., Tokunaga,
A. T., Potter, D., Cushing, M.: 2002, Near-Infrared Adaptive OpticsSpectroscopy of Binary Brown Dwarfs HD
52130948B and HD 130948C, Astrophys. J. Lett., 567, L59‑
L62.
Gouda, N., Tsujimoto, T., Kobayashi, Y., Nakajima, T.,
Yasuda, N., Matsuhara, H.: 2002, Japanese Astrometry
Satellite Mission for Infrared Exploration, Astrophycs andSpace Science, 280, 89‑94.
Grechnev, V. V., and Nakajima, H.: 2002, An Impulsive
Solar Flare Accompanied by a Cusplike Structure in SoftX-Rays, Astrophys. J., 566, 539‑554.
Hagiwara, Y., Diamond, P. J., Nakai, N., and Kawabe, R.:
2001, VLBI Study of Water Maser Emission in the Seyfert 2 Galaxy NGC 5793. I. Imaging Blueshifted Emission and the Parsec-Scale Jet, Astrophys. J., 560, 119‑126.
Hagiwara, Y., Henkel, C., Menten, K. M., and Nakai, N.:
2001, Water Maser Emission from the Active Nucleus in
M51, Astrophys. J. Lett., 560, L37‑L40.
Hanaoka, Y., and Sakurai, T.: 2001, Determination of theMagnetic Loop Configuration of a Solar Flare, Earth,Planets, and Space, 53, 593‑596.
Hayakawa, T., Cambresy, L., Onishi, T., Mizuno, A., andFukui, Y.: 2001, Column Density and Extinction in the
Chamaeleon II-III Dark-Cloud Complex, Publ. Astron.
Soc. Japan, 53, 1109‑1118.
Heki, K. and Miyazaki, S.: 2001, Plate convergence andlong term crustal deformation in central Japan, Geophys.
Res. Lett., 28, 2313‑2316.
Heki, K.: 2001, Seasonal modulation of interseismic strain
build-up in Northeastern Japan driven by snow loads,
Science, 293, 89‑92.
Hirano, N., and Taniguchi, Y.: 2001, Submillimeter CO
Emission from Shock-Heated Gas in the L1157 Outflow,
Astrophys. J. Lett., 550, L219‑L222.
Honma, M. and Kurayama, T.: 2002, Astrometricmicrolensing of distant sources caused by stars in the Galaxy, Astrophys. J., 568, 717‑725.
Honma, M.: 2001, Detecting Galactic MACHOs with VERA
through Astrometric Microlensing of Distant Radio
Sources, Publ. Astron. Soc. Japan, 53, 233‑241.
Hudson, H. S., Kosugi, T., Nitta, N. V., and Shimojo, M.:
2001, Hard X-Radiation from a Fast Coronal Ejection,
Astrophys. J. Lett., 561, L211‑L214.
Ikeda, M., Ohishi, M., Nummelin, A., Dickens, J. E.,
Bergman, P., Hjalmarson, Å., and Irvine, W. M.: 2001,
Survey Observations of c-C2H4O and CH3CHO toward
Massive Star-Forming Regions, Astrophys. J., 560, 792‑
805.
Imai, H., Deguchi, S., and Sasao, T.: 2002, Microstructureof Water Masers in W3 IRS5, Astrophys. J., 567, 971‑979.
(NROR. 549).
Imai, H., Ishihara, Y., Kameya, O., and Nakai, N.: 2001,
Water Maser Survey in the Andromeda Galaxy, Publ.
Astron. Soc. Japan, 53, 489‑493. (NROR. 536).
Imai, H., Miyoshi, M., Ukita, N., Morimoto, M., Iwata, T.,
Takaba, H., Kameno, S., Matsumoto, K., Fujisawa, K.,
and Kawaguchi, N.: 2001, Snapshot VLBI Observationsof SiO v=1 and v=2 (J=1-0) Maser Sources, Publ. Astron.
Soc. Japan, 53, 259‑273.
Imanishi, M., Dudley, C. C., and Maloney, P. R.: 2001,
Strong Evidence for a Buried Active Galactic Nucleus in

UGC 5101: Implications for LINER-type Ultraluminous
Infrared Galaxies, Astrophys. J. Lett., 558, L93‑L96.
Imanishi, M.: 2001, Thermal Infrared 3-5 Micron Colors of
Obscured and Unobscured Active Galactic Nuclei, Astron.
J., 121, 1927‑1935.
Inoue, K. T.: 2001, Are Compact Hyperbolic Models
Observationally Ruled Out ?, Progress of Theoretical
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Inoue, K. T.: 2001, COBE Constraints on a Compact Toroidal Low-density Universe, Classical and Quantum Gravity, 18, 1967‑1978.
Ishihara, Y., Nakai, N., Iyomoto, N., Makishima, K., Diamond, P., and Hall, P.: 2001, Water-Vapor Maser Emission from the Seyfert 2 Galaxy IC 2560: Evidence for a
Super-Massive Black Hole, Publ. Astron. Soc. Japan, 53,
215‑225. (NROR. 538).
Ishii, M., Nagata, T., Sato, S., Yao, Y., Jiang, Z., andNakaya, H.: 2001, K-Band Spectroscopy of Luminous
Young Stellar Objects, Astron. J., 121, 3191‑3206.
Ishitsuka, Jose K., Imai, H., Omodaka, T., Ueno, M.,
Kameya, O., Sasao, T., Morimoto, M., Miyaji, T.,
Nakajima, J., and Watanabe, T.: 2001, VLBI Monitoring
Observations of Water Masers around the Semi-Regular
Variable Star R Crateris, Publ. Astron. Soc. Japan, 53,
1231‑1238. (NROR. 550).
Isobe, H., Yokoyama, T., Shimojo, M., Morimoto, T.,
Kozu, H., Eto, S., Narukage, N., and Shibata, K.: 2002,
Reconnection Rate in the Decay Phase of a Long Duration Event Flare on 1997 May 12, Astrophys. J., 566, 528‑
538.
Ita, Y., Deguchi, S., Fujii, T., Kameya, O., Miyoshi, M.,
Nakada, Y., Nakashima, J., and Parthasarathy, M.: 2001,
SiO Maser Survey of AGB Stars in the North Galactic
Cap, Astron. Astrophys., 376, 112‑123.
Ito, T. and Miyama, S. M.: 2001, An Estimation of Upper
Limit Masses of υ Andromedae Planets, Astrophys. J.,
552, 372‑379.
Itoh, Y., Tamura, M., Suto, H., Hayashi, S. S., Murakawa,
K., Oasa, Y., Nakajima, Y., Kaifu, N., Kosugi, G., Usuda,
T. and Doi, Y.: 2001, Near-Infrared Observations of S
255-2: The Heart of a Massive YSO Cluster, Publ. Astron.
Soc. Japan, 53, 495‑500.
Iwata, I., Ohta, K., Nakanishi, K., Kohno, K., andMcMahon, R. G.: 2001, CO (J=6-5) Observations of the
Quasar SDSS 1044-0125 at z = 5.8, Publ. Astron. Soc.
Japan, 53, 871‑873.
Iyomoto, N., Fukazawa, Y., Nakai, N., and Ishihara, Y.:
2001, BeppoSAX Observation of NGC 3079, Astrophys.
J. Lett., 561, L69‑L72.
Jiang, Z., Yao, Y., Yang, J., Ishii, M., Nagata, T., Nakaya,
H., and Sato, S.: 2001, K'-Band Polarimetric Imaging of
S187 IR and S233, Astron. J., 122, 313‑321.
Kajisawa, M., Yamada, T.: 2001,When Did the Hubble
Sequence Appear?: Morphology, Color, and NumberDensity Evolution of the Galaxies in the Hubble Deep
Field North, Publ. Astron. Soc. Japan, 53, 833.
Kameno, S., Sawada-Satoh, S., Inoue, M., Shen, Z.-Q., and
Wajima, K.: 2001, The Dense Plasma Torus around the
Nucleus of an Active Galaxy NGC 1052, Publ. Astron.

Soc. Japan, 53, 169‑178.
Kato, T., Baba, H., and Nogami, D.: 2002, IR Com: Deeply
Eclipsing Dwarf Nova Below the Period Gap -A Twin of
HT Cas?, Publ. Astron. Soc. Japan, 54, 79‑85.
Kato, T., Nogami, D., and Baba, H.: 2001, Outburst Photometry of FX Cep, Inf. Bull. Variable Stars, 5103.
Kato, T., Nogami, D., and Baba, H.: 2001, Photometry of
UZ Tau, Inf. Bull. Variable Stars, 5121.
Kato, T., Nogami, D., and Baba, H.: 2001, The 1996-1997
fading of V651 Mon, the binary central star of the planetary nebula NGC 2346, Publ. Astron. Soc. Japan, 53,
901‑903.
Kato, T., Nogami, D., Baba, H., and Masuda, S.: 2001,
Outburst cycle of V363 Lyr, Inf. Bull. Variable Stars,
5118.
Katsukawa, Y., and Tsuneta, S.: 2001, Small Fluctuation ofCoronal X-ray Intensity and a Signature of Nanoflares,
Astrophys. J., 557, 343‑350.
Kawabata, K. S., Akitaya, H., Hirakata, N., Hirata, R.,
Ikeda, Y., Isogai, M., Karube, T., Kondoh, M., Matsumura,M., Nakayama, S., Okazaki, A., and Seki, M.: 2001,
Spectropolarimetric Evidence of Asymmetric Outburst in
the Fast Nova V1494 Aquilae, Astrophys. J., 552, 782‑
786.
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Shibata, K., and Yokoyama, T.: 2001, First Results on theOrigin of Universal Correlation Between Flare Temperature and Emission Measure for Solar and Stellar Flares,
Adv, Space Res., 26, 1753‑1757.
Shimasaku, K., Fukugita, M., Doi, M., Hamabe, M., Ichikawa,T., Okamura, S., Sekiguchi, M., Yasuda, N., Brinkmann,
J., Csabai, I., Ichikawa, S., Ivezic, Z., Kunszt, P. Z.,
Schneider, D. P., Szokoly, G. P., Watanabe, M., and York,D. G.: 2001, Statistical Properties of Bright Galaxies in
the Sloan Digital Sky Survey Photometric System, Astron.
J., 122, 1238‑1250.
Shimojo, M., Kurokawa, H., and Yoshimura, K.: 2002,
Dynamical Features and Evolutional Characteristics ofBrightening Coronal Loops, Solar Physics, 206, 133‑142.
Shimojo, M., Shibata, K., Yokoyama, T., and Hori, K.:
2001, One-Dimensional and Pseudo-Two-Dimensional
Hydrodynamic Simulations of Solar X-Ray Jets, Astrophys.
J., 550, 1051‑1063.
Shirai, T., and Fukushima, T.: 2001, Detection of Excitations of Free Core Nutation of the Earth and their Concurrence with Huge Earthquakes, Geophys. Res. Lett., 28,3553.
Shirasaki, Y., Kakimoto, F., Ogio, S., Gironda, N., Takeda,
M., Kaneko, T., Yoshii, H., Baba, T., Sano, S., Nishi, K.,
Tajima, N., Yamada, Y., Shimoda, S., Nakatani, H., Gotoh,
E., Murakami, K., Toyoda, Y., Matsubara, Y., Mizumoto,Y., Velasquez, W., Velarde, A., Miranda, P.: 2001, Chemical composition of primary cosmic rays with energies
15
16.5
from 10 to 10 eV, Astroparticle Physics, 15, 357‑381.
Singh, J., Sakurai, T., and Ichimoto, K.: 2001, On the
Disappearance of H-Alpha Filaments and Soft X-Ray
Enhancements as Seen from Yohkoh, Bull. Astron. Soc.
India, 29, 193‑202.

Sorai, K., Hasegawa, T., Booth, R. S., Rubio, M., Morino,
J.-I., Bronfman, L., Handa, T., Hayashi, M., Nyman, L.Å ., Oka, T., Sakamoto, S., Seta, M., and Usuda, K. S.:
2001, The CO J=2-1/J=1-0 Ratio in the Large Magellanic
Cloud, Astrophys. J., 551, 794‑802.
Stoughton, C., Lupton, R. H., Bernardi, M., Blanton, M. R.,
Burles, S., Castander, F. J., Connolly, A. J., Eisenstein,
D. J., Frieman, J. A., Hennessy, G. S., Hindsley, R. B.,
Ivezic, Z., Kent, S., Kunszt, P. Z., Lee, B. C., Meiksin,A., Munn, J. A., Newberg, H. J., Nichol, R. C., Nicinski,T., Pier, J. R., Richards, G. T., Richmond, M. W., Schlegel,
D. J., Smith, J. A., Strauss, M. A., SubbaRao, M., Szalay,
A. S., Thakar, A. R., Tucker, D. L., Vanden, B., Daniel,
E, Yanny, B., Adelman, J. K., Anderson, J. E. Jr., Anderson, S. F., Annis, J., Bahcall, N. A., Bakken, J. A.,
Bartelmann, M., Bastian, S., Bauer, A., Berman, E., B‥
ohringer, H., Boroski, W. N., Bracker, S., Briegel, C.,
Briggs, J. W., Brinkmann, J., Brunner, R., Carey, L., Carr,
M. A., Chen, B., Christian, D., Colestock, P. L., Crocker,
J. H., Csabai, I., Czarapata, P. C., Dalcanton, J., Davidsen,
A. F., Davis, J. E., Dehnen, W., Dodelson, S., Doi, M.,
Dombeck, T., Donahue, M., Ellman, N., Elms, B. R.,
Evans, M. L., Eyer, L., Fan, X., Federwitz, G. R., Friedman, S., Fukugita, M., Gal, R., Gillespie, B., Glazebrook,K., Gray, J., Grebel, E. K., Greenawalt, B., Greene, G.,
Gunn, J. E., de Haas, E., Haiman, Z., Haldeman, M., Hall,
P. B., Hamabe, M., Hansen, B., Harris, F. H., Harris, H.,
Harvanek, M., Hawley, S. L., Hayes, J. J. E., Heckman,
T. M., Helmi, A., Henden, A., Hogan, C. J., Hogg, D. W.,
Holmgren, D. J., Holtzman, J., Huang, C.-H., Hull, C.,
Ichikawa, S., Ichikawa, T., Johnston, D. E., Kauffmann,G., Kim, R. S. J., Kimball, T., Kinney, E., Klaene, M.,
Kleinman, S. J., Klypin, A., Knapp, G. R., Korienek, J.,
Krolik, J., Kron, R. G., Krzesinski, J., Lamb, D. Q., Leger,
R. F., Limmongkol, S., Lindenmeyer, C., Long, D. C.,
Loomis, C., Loveday, J., MacKinnon, B., Mannery, E. J.,
Mantsch, P. M., Margon, B., McGehee, P., McKay, T.
A., McLean, B., Menou, K., Merelli, A., Mo, H. J., Monet,D. G., Nakamura, O., Narayanan, V. K., Nash, T., Neilsen,
E. H. Jr., Newman, P. R., Nitta, A., Odenkirchen, M.,
Okada, N., Okamura, S., Ostriker, J. P.,Owen, R., Pauls,A. G., Peoples, J., Peterson, R. S., Petravick, D., Pope,
A., Pordes, R., Postman, M., Prosapio, A., Quinn, T. R.,
Rechenmacher, R., Rivetta, C. H., Rix, H.-W., Rockosi, C.
M., Rosner, R., Ruthmansdorfer, K., Sandford, D.,
Schneider, D. P., Scranton, R., Sekiguchi, M., Sergey, G.,
Sheth, R., Shimasaku, K., Smee, S., Snedden, S. A.,
Stebbins, A., Stubbs, C., Szapudi, I., Szkody, P., Szokoly,
G. P., Tabachnik, S., Tsvetanov, Z., Uomoto, A., Vogeley,
M. S., Voges, W., Waddell, P., Walterbos, R., Wang, S.i., Watanabe, M., Weinberg, D. H., White, R. L., White,
S. D. M., Wilhite, B., Wolfe, D., Yasuda, N., York, D. G.;
Zehavi, I., Zheng, W.: 2002, Sloan Digital Sky Survey:
Early Data Release, Astron. J., 123, 485‑548.
Sugitani, K., Tamura, M., Nakajima, Y., Nagashima, C.,
Nagayama, T., Nakaya, H., Pickles, A. J., Nagata, T.,
Sato, S., Fukuda, N., and Ogura, K.: 2002 Near-Infrared
Study of M16: Star Formation in the Elephant Trunks,
Astrophys. J. Lett., 565, L25‑L28.
57

Sumiyoshi, K., Terasawa, M., Mathews, G. J., Kajino, T.,
Yamada, S., and Suzuki, H.: 2001, R-process in Prompt
Supernova Explosions revisited, Astrophys. J., 562, 880‑
886.
Sumiyoshi, K., Terasawa, M., Suzuki, H., Yamada, S.,
Toki, H., Mathews, G. J., and Kajino, T.: 2001, Relativistic simulations of supernovae and the r-process; A new
relativistic EOS and nuclear reaction network, Nucl. Phys.
A, 688, 478‑480.
Takaba, H., Iwata, T., Miyaji, T., and Deguchi, S.: 2001,
Kashima 34-m Water Maser Survey of Late-Type Stars,
Publ. Astron. Soc. Japan, 53, 517‑533. (NROR. 540).
Takada, M.: 2001, Lensing-induced Non-Gaussian Signatures in the Cosmic Microwave Background, Astrophys.
J., 558, 29‑41.
Takahashi, R., Arai, K. and the TAMA collaboration:
2002, Improvement of the vibration isolation system for
TAMA300, Class. Quantum Grav., 19, 1599‑1604.
Takakuwa, S., Kawaguchi, K., Mikami, H., and Saito, M.:
2001, The Ortho-to-Para Ratio and the Chemical Properties of C3H2 in Dark Cloud Cores, Publ. Astron. Soc.
Japan, 53, 251‑257. (NROR. 537).
Takami, M., Chrysostomou, A., Bailey, J., Gledhill, T. M.,
Tamura, M., and Terada, H.: 2002, He I 1.083 µm
Emission and Absorption in DG Tauri: Line Excitationsin the Jet, Hot Wind, and Accretion Flow, Astrophys. J.
Lett., 568, L53‑L56.
Takami, M., Usuda, T., Sugai, H., Suto, H., Pyo, T.-S.,
Takeyama, N., Aoki, T., Mizutani, K., and Tanaka, M.:
2002, [Fe II] 1.257 µm and He I 1.083 µm Emission in theCentral Region of the Orion Nebula: H II Region, HH
Flows, Jets, and Proplyds, Astrophys. J., 566, 910‑924.
Takeda, Y., Sato, B., Kambe, E., Aoki, W., Honda, S.,
Kawanomoto, S., Masuda, S., Izumiura, H., Watanabe,E., Koyano, H., Maehara, H., Norimoto, Y., Okada, T.,
Shimizu, Y., Uraguchi, F., Yanagisawa, K., Yoshida,M., Miyama, S. M., and Ando, H.: 2002, PhotosphericAbundances of Volatile and Refractory Elements in PlanetHarboring Stars, Publ. Astron. Soc. Japan, 53, 1211‑
1221.
Takeda, Y., Sato, B., Kambe, E., Watanabe, E., Miyazaki,
H., Wada, S., Ando, H., Masuda, S., Izumiura, H.,
Koyano, H., Maehara, H., Norimoto, Y., Okada, T.,
Shimizu, Y., Uraguchi, F., Yanagisawa, K., Yoshida,M., Okada, N., Kawanomoto, S. and Miyama, S. M.:
2001, Iodine-Cell Spectroscopy at Okayama Astrophysical Observatory: First Results, Publ. Astron. Soc. Japan,
54, 113‑120.
Takeuchi, T. T., Kawabe, R., Kohno, K., Nakanishi, K.,
Ishii, T. T., Hirashita, H., and Yoshikawa, K.: 2001, Impact of Future Submillimeter and Millimeter Large Facilities on the Studies of Galaxy Formation and Evolution,
Publ. Astron. Soc. Pacific, 113, 586‑606.
Tamura, M.: 2001 Exoplanet Photometry and Spectroscopy with HII/L2, ISAS Report, SP14, 3‑9.
Tamura, N., Ohta, K., Maihara, T., Iwamuro, F., Motohara,K., Takata, T., and Iye, M.: 2001, NIR Narrow- andBroad-Band Study of the SSA 22 Field, Publ. Astron. Soc.
Japan, 53, 653‑662.
58

Taniguchi, Y., Ohyama, Y., Murayama, T., Yoshida, M.,
Kashikawa, N., Iye, M., Aoki, K., Sasaki, T., Kosugi,G., Takata, T., Saito, Y., Kawabata, K. S., Sekiguchi,
K., Okita, K., Shimizu, Y., Inata, M., Ebizuka, N.,
Ozawa, T., Yadomaru, Y., Taguchi, H., Shioya, Y.,
Nishiura, S., Sudou, H., Nagao, T., Noda, S., Kakazu, Y.,
Ajiki, M., Fujita, S., and Kobayashi, R.: 2001, A ShockInduced Pair of Superbubbles in the High-Redshift Powerful Radio Galaxy MRC 0406‑244, Astrophys. J. Lett.,
559, L9‑L12.
Tanikawa, K. and Yamaguchi, Y.: 2002, Dynamical ordering of symmetric non-Birkhoff periodic points in reversible monotone twist mappings, Chaos, 12, 33‑41.
Tanuma, S., Yokoyama, T., Kudoh, T., and Shibata, K.:
2001, Two-Dimensional Magnetohydrodynamic Numerical Simulations of Magnetic Reconnection Triggered bya Supernova Shock in the Interstellar Medium: Generation of X-Ray Gas in the Galaxy, Astrophys. J., 551, 312‑
332.
Terada, H., Imanishi, M., Goto, M., and Maihara, T.: 2001,
Detection of the unusual 3.5 µm feature in the Herbig Be
star MWC 297, Astron. Astrophys., 377, 994‑998.
Terasawa, M., Sumiyoshi, K., Kajino, T., Tanihata, I., andMathews, G. J.: 2001, New Nuclear Reaction Flow towards R-Process Nucleosynthesis in Supernovae: A Critical Role of the Light Neutron-Rich Nuclei, Astrophys. J.,
562, 470‑479.
Terasawa, M., Sumiyoshi, K., Kajino, T., Tanihata, I.,
Mathews, G. J., and Langanke, K.: 2001, New Reaction
Flow of r-Process Nucleosynthesis in Supernovae, Nucl.
Phys. A, 688, 581‑583.
Tomono, D., Doi, Y., Usuda, T., and Nishimura, T.: 2001,
Mid-Infrared Spectral Energy Distribution of NGC 1068with 0".1 Spatial Resolution, Astrophys. J., 557, 637‑645.
Totani, T. and Inoue, S.: 2002, Preheating in the universe
suppressing high energy gamma rays from structure formation, Astropart. Phys., 17, 79‑85.
Totani, T., and Takeuchi, T.: 2002, A Bridge from Opticalto Infrared Galaxies: Explaining Local Properties andPredicting Galaxy Counts and the Cosmic Background
Radiation, Astrophys. J., 570, 470‑491.
Totani, T., Yoshii, T., Iwamuro, F., Maihara, T. andMotohara, K.: 2001, Hyper Extremely Red Objects in the
Subaru Deep Field: Evidence for Primordial Elliptical
Galaxies in the Dusty Starburst Phase, Astrophys. J. Lett.,
558, L87‑L91.
Totani, T., Yoshii, T., Iwamuro, F., Maihara, T., andMotohara, K.: 2001, Near-Infrared Faint Galaxies in the
Subaru Deep Field: Comparing the Theory with Observations for Galaxy Counts, Colors, and Size Distributions to
K ~ 24.5, Astrophys. J., 559, 592‑605.
Tsuboi, Y., Koyama, K., Hamaguchi, K., Tatematsu, K.,
Sekimoto, Y., Bally, J., and Reipurth, B.: 2001, Discovery of X-Rays from Class 0 Protostar Candidates in OMC3, Astrophys. J., 554, 734‑741.
Tsujimoto, M., Koyama, K., Tsuboi, Y., Goto, M., andKobayashi, N.: 2002, X-Ray Properties of Young Stellar
Objects in OMC-2 and OMC-3 from the Chandra X-Ray
Observatory, Astrophys. J., 566, 974‑981.

Tsujimoto, T., and Shigeyama, T.: 2001, SN 1987A Revisited as a Major Production Site for r-Process Elements,
Astrophys. J. Lett., 561, L97‑L100.
Tsujimoto, T., Shigeyama, T. and Yoshii, Y.: 2002, Chemical Evolution of Odd Elements in an Inhomogeneous Early
Galaxy, Astrophys. J., 565, 1011‑1016.
Tutui, Y., Sofue, Y., Honma, M., Ichikawa, T.,
Wakamatsu, K.: 2001, Hubble Constant at Intermediate
Redshift Using the CO-Line Tully-Fisher Relation, Publ.
Astron. Soc. Japan, 53, 701‑712.
Umehara, H. and Tanikawa, K.: 2001, Improvement of
triple-encounter criterion, Publ. Astron. Soc. Japan, 53,
693‑697.
Vazdekis, A., Kuntschner, H., Davies, R. L., Arimoto, N.,
and Peletier, R.: 2001, On the Origin of the Color-Magnitude Relation in the Virgo Cluster, Astrophys. J. Lett., 551,
L127‑L130.
Vazdekis, A., Salaris, M., Arimoto, N., and Rose, J. A.:
2001, 47 Tucanae: The Spectroscopic versus Color-Magnitude Diagram Age Discrepancy, Astrophys. J., 549,
274‑280.
Wada, K., and Koda, J.: 2002, Multi-Phase Gas Dynamics
in a Weak Barred Potential, Pub. Astron, Soc. Japan, 53,
1163‑1170.
Wada, K., and Norman, C.: 2002, Obscuring Material around
Seyfert Nuclei with Starbursts, Astrophys. J. Lett., 566,
L21‑24.
Wada, K.: 2001, The Three-dimensional Structure of a
Massive Gas Disk in the Galactic Central Region,
Astrophys. J. Lett., 559, L41‑44.
Wanajo, S., Kajino, T., Mathews, G. J., and Otsuki, K.:
2001, The r-process in netrino-driven winds from nascentcompact neutron stars of core-collapse supernovae,
Astrophys. J., 554, 578‑586.
Wang, H., Yan, Y., and Sakurai, T.: 2001, Topology ofMagnetic Field and Coronal Heating in Solar Active Regions, Solar Phys., 201, 323‑336.
Wang, Z., Chakrabarty, D., Roche, P., Charles, P. A.,
Kuulkers, E., Shahbaz, T., Simpson, C., Forbes, D. D. A.,
and Helsdon, S. F.: 2001, The Optical Counterpart of theAccreting Millisecond Pulsar SAX J1808.4-3658 in Outburst: Constraints on the Binary Inclination, Astrophys. J.
Lett., 563, L61‑L64.
Watanabe, J., Kinoshita, D., Komiyama, Y., Fuse, T.,
Urata, Y., and Yoshida, F.: 2001, Optical Follow-up of
the GRB 010222 Afterglow by Subaru Telescope, Publ.
Astron. Soc. Japan, 53, L27‑L31.
Watanabe, M., Yasuda, N., Itoh, N., Ichikawa, T., andYanagisawa, K.: 2001, Surface Photometric Calibrationof the Infrared Tully-Fisher Relation Using Cepheid-based
Distances of Galaxies, Astrophys. J., 555, 215‑231.
Watanabe, T., Sterling, A. C., Hudson, H. S., and Harra, L.
K.: 2001, Energetics an Active Region Observed from
Helium-Like Sulphur Lines, Solar Phys., 201, 71‑91.
Wu, K., Cropper, M., Ramsay, G., and Sekiguchi, K.: 2002,
An electrically powered binary star?, Monthly Notices Roy.
Astron. soc., 331, 221‑227.
Yagi, M., Kashikawa, N., Sekiguchi, M., Doi, M., Yasuda,N., Shimasaku, K., and Okamura, S.: 2002, Luminosity

Functions of 10 Nearby Clusters of Galaxies. I. Data,
Astron. J., 123, 66.
Yagi, M., Kashikawa, N., Sekiguchi, M., Doi, M., Yasuda,N., Shimasaku, K., Okamura, S.: 2002, Luminosity Functions of 10 Nearby Clusters of Galaxies. II. Analysis of
the Luminosity Funciton, Astron. J., 123, 87.
Yahiro, M., Mathews, G. J., Ichiki, K., Kajino, T., andOrito, M.: 2002, Constraints on Cosmic Quintessence andquintessential inflation, Phys. Rev. D, 65, 063502‑063510.
Yamada, M., Fujita, Y.: 2001, The Heating of Intracluster
Gas by the Jet Activities of Active Galactic Nuclei: is the"Preheating" Schenario Realistic?, Astrophys. J. Lett., 553,
L145‑L148.
Yamada, T., Motohara, K., Iwamuro, F., Maihara, T.,
Kajisawa, M., Tanaka, I., Kodama, T., Terada, H.,
Goto, M., Tanabe, H., Taguchi, T., Hata, R., Takata, T.,
Sekiguchi, K., Iye, M., Sasaki, T., Usuda, T., Kosugi,G., and Simpson, C.: 2001, Subaru Deep Near-Infrared
Imaging of the Field of a Possible Proto-Cluster Near theRadio Galaxy 53W002 at z=2.4, Publ. Astron. Soc. Japan,
53, 1119‑1131.
Yamaguchi, Y. and Tanikawa, K.: 2001, Dynamical ordering of Non-Birkhoff periodic orbits in a forced pendulum, Prog. Theor. Phys., 106, 1097‑1114.
Yamaguchi, Y. and Tanikawa, K.: 2001, Non-symmetrical
non-Birkhoff period 2 orbits in the Standard mapping,
Prog. Theor. Phys., 106, 691‑696.
Yamamoto, S., Maezawa, H., Ikeda, M., Ito, T., Oka, T.,
Saito, G., Iwata, M., Kamegai, K., Sakai, T., Sekimoto,Y., Tatematsu, K., Noguchi, T., Shi, S. C., Arikawa, Y.,
Aso, Y., Miyazawa, K., Saito, S., Fujiwara, H., Ohishi,
M., Ozeki, H., and Inatani, J.: 2001, Observations of the CI
3
3
P2‑ P1 Line toward the Orion Kleinmann-Low Region,
Astrophys. J. Lett., 547, L165‑L169.
Yasuda, N., Fukugita, M., Narayanan, V. K., Lupton, R. H.,
Strateva, I., Strauss, M. A., Ivezic, Z., Kim, R. S. J., Hogg,
D. W., Weinberg, D. H., Shimasaku, K., Loveday, J.,
Annis, J., Bahcall, N. A., Blanton, M., Brinkmann, J.,
Brunner, R. J., Connolly, A. J., Csabai, I., Doi, M., Hamabe,M., Ichikawa, S., Ichikawa, T., Johnston, D. E., Knapp,
G. R., Kunszt, P. Z., Lamb, D. Q., McKay, T. A., Munn,
J. A., Nichol, R. C., Okamura, S., Schneider, D. P., Szokoly,
G. P., Vogeley, M. S., Watanabe, M., and York, D. G.:
2001, Galaxy Number Counts from the Sloan Digital Sky
Survey Commissioning Data, Astron. J., 122, 1104-1124.
Yokogawa, S., Kitamura, Y., Momose, M., Asaki, Y.,
Tamura, M., Ida, S., and Kawabe, R.: 2001 Millimeter
continuum image of the circumstellar disk around the
young star Haro 6-5B, Astrophys. J. Lett., 552, L59‑L62.
(NROR. 541).
Yoshida, F., Nakamura, T., Fuse, T., Komiyama, Y.,
Yagi, M., Miyazaki, S., Okamura, S., Ouchi, M., andMiyazaki, M.: 2001, First Subaru Observations of Subkm Main-Belt Asteroids, Publ. Astron. Soc. Japan, 53,
L13‑L16.
Yoshida, H.: 2001, Non-existence of the modified first
integral by symplectic integration methods, Phys. Lett. A,
282, 276‑283.
Yoshida, M., Yagi, M., Okamura, S., Aoki, K., Ohyama,
59

Y., Komiyama, Y., Yasuda, N., Iye, M., Kashikawa, N.,
Doi, M., Furusawa, H., Hamabe, M., Kimura, M.,
Miyazaki, M., Miyazaki, S., Nakata, F., Ouchi, M.,
Sekiguchi, M., Shimasaku, K., and Ohtani, H.: 2002, Discovery of a Very Extended Emission-Line Region aroundthe Seyfert 2 Galaxy NGC 4388, Astrophys. J., 567, 118‑
129.
Yoshii, H., Morizawa, A., Kakimoto, F., Ogio, S., Tsunesada,Y., Tokunou, H., Harada, D., Burgoa, O., Tajima, N.,
Shimoda, Y. Yamada, S., Nishi, K., Nakatani, H., Gotoh,
E., Shirasaki, Y., Miranda, P., Velarde, A., Kaneko, T.,
Murakami, K., Toyoda, Y., Matsubara, Y., Mizumoto,Y.: 2001, Present experiment of BASJE group at Mt.
Chacaltaya, Il Nuovo Cimento C, 024, 507.
Yoshii, Y., Minezaki, T., Aoki, T., Enya, K., Doi, M.,
Motohara, K., Kobayashi, Y., Suganuma, M., Tomita,
H., Peterson, B. A.: 2002, Supernova 2002ap in M74,
IAUC, 7826, 1.
You, J., Li, H., Fan, Z., and Sakurai, T.: 2001, MultiWavelength Observation of the 3N/X3.3 Flare of 28 November 1998, Solar Phys., 203, 107‑117.
Zhu, Z.-H., Fujimoto, M.-K., and Tatsumi, D.: 2001,
Determining the cosmic equation of state by using future
gravitational wave detectors, Astron. Astrophys., 372, 377‑
380.

2. Publications of the National Astronomical
Observatory of Japan
There is no paper in this category.

3. Report of the National Astronomical
Observatory of Japan (in Japanese)＾
Hayamizu, T., Soma,
M., Geshiro, H., and Hashiguchi, T.:
2001,Development of a New Device for Precise Timing,
Rep. Nat. Astron. Obs. Japan, 5, 73‑79.
Nakamura, K., Miyata, T., and Kataza, H.: 2001, Development of Control Software System for Cooled Mid-Infrared Camera and Spectrometer on the Subaru Telescope,
Rep. Nat. Astron. Obs. Japan, 5, 81‑90.
＾
Soma,
M.: 2001, On the Effects of Dip and Refraction in
Calculating the Times of Sunrise and Sunset, Rep. Nat.
Astoron. Obs. Japan, 5, 91‑95.
Shinoda, K., Ichimoto, K., Fukuda, T., and Shin, J.: 2001,
A Universal Polarimeter Using Liquid Crystal Variable
Retarders at the Norikura Solar Observatory, Rep. Nat.
Astron. Obs. Japan, 5, 97‑106.
Iwashita, H., Torii, Y., Kubo, K., Matsuda, K.: 2001,
Endurance Tests of Silver Coated Morrors, Rep. Nat.
Astron. Obs. Japan, 5, 107‑115.
Ishizaki, H., Ichikawa, N., and Morikawa, H.: 2002, A
Logic of the Run-Out Measurement, Rep. Nat. Astron.
Obs. Japan, 5, 117‑129.
Fukushima, H.: 2002, Image Processing of the Solar Corona Wide-Field and High-Resolution Images of the Solar Corona at the Total Solar Eclipse in Africa on June 21,
2001, Rep. Nat. Astron. Obs. Japan, 5, 131‑144.
＾
Kawbata, K. -A., Tanikawa, K., and Soma,
M.: 2002,

60

Reliability of Astronomical Records in the Nihongi, Rep.
Nat. Astron. Obs. Japan, 5, 145‑159.

4. Other Publications
Ariyoshi, S., Matsuo, H., Takeda, M., Noguchi, T.: 2001,
Design of Submillimeter-wave Camera with Superconducting Direct Detectors, Proc. of the 12th International
Symp. on Space Terahertz Technology, 183‑192.
Beers, T. C., and Chiba, M.: 2001, Galaxy Formation One
Star at a Time: New Information From the Kinematics ofField Stars in the Galaxy, Astrophysical Ages and Times
Scales, eds. T. Hippel, C. Simpson, and N. Manset, ASP
Conf. Ser., 245, 149.
Buzzi, L., Aletti, A., Asami, A., Asher, D. J. Fuse, T.,
Hashimoto, N., Ibrahim, A. I., Isobe, S., Nishiyama, K.,
Oshima, Y., Terazono, J., Umehara, H., Urata, T.,
Yoshikawa, M., Kadota, K., Stevens, B., Sanchez, S.,
Rodriguez, J., Kojima, T., Holvorcem, P. R., Schwartz,
M., and Marsden, B. G.: 2002, COMET C/20, Minor
Planet Electronic Circ., 2002‑F39.
Chiba, M., and Nath, B. B.: 2002, On the Origin of Metallicity
in Lyman-alpha Forest Systems, Proc. IAU Symp. 187,
"Cosmic Chemical Evolution", eds. K. Nomoto, and J. W.
Truran, 187, 123‑127.
Davidsson, B., Karlsson, O., Lagerkvist, C.-I., Oja, T., Warell,J., Hahn, G., Mottola, S., Galad, A., Gajdos, S., Haver,R., Anzellini, F., Asami, A., Asher, D. J., Fuse, T.,
Hashimoto, N., Ibrahim, A. I., Isobe, S., Nishiyama, K.,
Oshima, Y., Terazono, J., Umehara, H., Urata, T.,
Yoshikawa, M., Ezaki, Y., Akahori, A., Maeno, H.,
Kadota, K., Nakamura, A., Abe, H., Seki, T., Sanchez, S.,
Takamizawa, K., Mas, A., Schwartz, M., Holvorcem, P.
R., Medkeff, J., and Marsden, B. G.: 2002, COMET C/20,
Minor Planet Electronic Circ., 2002‑F23.
Deguchi, S.: 2001, Stellar Velocity Field in the Bar of the
Galaxy Revealed from SiO Maser Observations, Proc. of
the international spring meeting of "Dynamics of Star
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Just, R. Spurzem, and R. Wielen, ASP Conf. Ser., 228,
404‑406.
Dermawan, B., Nakamura, T., Yoshida, F., Fukushima,
H., Sato, H., and Sato, Y.: 2001, Mitaka photometricobservations of MUSES-C mission target 1998 SF36,
34th Lunar and Planetary Sympo., 95‑98.
Fujita, Y.: 2001, Heating of X-Ray Hot Gas in Groups by
Blast Waves, New Century of X-ray Astronomy, 444-445.
Furusho, T., Yamasaki, N. Y., Ohashi, T., Shibata, R., Kagei,T., Ishisaki, Y., Kikuchi, K., Ezawa, H., and Ikebe, Y.:
2001, ASCA Temperature Maps of Four Clusters of Galaxies: Abell 1060, AWM7, the Centaurus Cluster, and thePerseus Cluster, Proc. of "New Century of X-Ray Astronomy", eds. H. Inoue and H. Kunieda, ASP Conf. Ser.,
251, 446‑447.
Fuse, T., Kinoshita, D., Yamamoto, N., Watanabe, J.:
2001, Outer Solar System Survey, Astrophysical Ages andTimes Scales, Astronomical Society of the Pacific, eds. T.
von Hippel, C. Simpson, and N. Manset, ASP Conf. Ser.,245, 135.

Gaessler, W., Takami, H., Takato, N., Hayano, Y.,
Kamata, Y., Saint-Jacques, D., Minowa, Y., Iye, M.:
2002, First results from the Subaru AO system, Proc. SPIE,
Adaptive Optics Systems and Technology II, eds. Robert
K. Tyson; Domenico Bonaccini; Michael C. Roggemann,
4494, 30‑40.
Giambersio, A. M., Postel, J. B., Pozzoli, V., Ligustri, R.,
Asami, A., Asher, D. J., Fuse, T., Hashimoto, N., Ibrahim,
A.I., Isobe, S., Nishiyama, K., Oshima, Y., Terazono, J.,
Umehara, H., Urata, T., Yoshikawa, M., Ezaki, Y.,
Akahori, A., Suzuki, M., Kadota, K., Seki, T., Sugie, A.,
Broughton, J., Rodriguez, J., Sanchez, S., Payer, T.,
Yamanishi, M., Miyamoto, A., Aimoto, M., Oribe, T.,
Nakano, S., and Marsden, B. G.: 2002, COMET C/20,
Minor Planet Electronic Circ., 2002‑C111.
Goto, M., Kobayashi, N., Terada, H., Takato, N., Gaessler,
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Hanaoka, Y.: 2001, Magnetic Field Structure of the CME
Source Region, Proc. of IAU Symp. 203, "Recent Insights
into the Physics of the Sun and Heliosphere: Highlightsfrom SOHO and other Space Missions", eds. P. Brekke, B.
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Hirabayashi, H., Edwards, P. G., Murata, Y., Inoue, M.,
Kobayashi, H., and Kameno, S.: 2001, A Next Generation Space VLBI Mission, Proc. of "New Century of XRay Astronomy", eds. H. Inoue and H. Kunieda, ASP
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Hirabayashi, H., Murata, Y., Edwards, P. G., Murphy, D.
W., Inoue, M., Kobayashi, H., and Kameno, S.: 2001,
Current Status of the VSOP-2 Mission, Proc. of the IAU
Symp. 205, "Galaxies and their constituents at the highest
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Honma, M.: 2001, Studying the Milky Way Galaxy with
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Honma, M.: 2001, VERA -Science (invited), 2001 AsiaPacific Radio Science Conf., 243.
Horiuchi, S., Kameno, S., and Ohishi, M.: 2001, Developing a Wavelet CLEAN Algorithm for Radio-Interferometer Imaging, Proc. of a meeting "Astronomical Data
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Hough, J. H., Bailey, J. A., Chrysostomou, A., Gledhill, T.
M., Lucas, P. W., Tamura, M., Clark, S., Yates, J., andMenard, F.: 2001 Circular Polarisation in Star-Forming
Regions: Possible Implications for Homochirality, Adv.
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Ikeda, M., Nishiyama, K., Ohishi, M., and Tatematsu, K.:
2001, Development of Radio Astronomical Data Reduction Software NEWSTAR, Proc. of a meeting "Astronomical Data Analysis Software and Systems X", eds. F.
R. Harnden Jr., F. A. Primini, and H. E. Payne, ASP Conf.
Ser., 238, 522‑524.

Imanishi, M.: 2001, 3‑4 µm Spectroscopy of Seyfert 2
Nuclei to Quantitatively Assess the Energetic Importanceof Nuclear Starbursts, Bull. AAS, 199, 5007.
Ishitsuka, J. K., Wada, T., Ieda, F., Tokimasa, N., Kuroda,T., Morimoto, M., Miyaji, T., Omodaka, T., Ueno, M.,
Hasegawa, W., Narusawa, S., and Waki, Y.: 2001, A Near
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P. Chen, C. Lemme, and B. Paczynski, ASP Conf. Ser.,
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Isobe, S., Asami, A., Asher, D.J., Fuse, T., Hashimoto, N.,
Nakano, S., Nishiyama, K., Ohshima, Y., Terazono, J.,
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Bisei Spaceguard Center for Detection of Near-Earth Asteroids and Space Debris, Conf. Proc. of the Airforce Maui
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Iwamoto, N., Kajino, T., and Aoki, W.: 2001, Nucleosynthesis of Heavy Elements in the First Generation Stars,
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Izumiura, H., Deguchi, S., Tajitsu, A., Parthasarathy, M.,
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Izumiura, H., Noguchi, K., Aoki, W., and HDS Developing Group: 2001, Violet Spectra of Silicate Carbon Stars,
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Kajino, T. and Orito, M.: 2001, Neutrinos from the BigBang, Supernovae and the Sun. Proc. 2nd Int. Workshop
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Kajino, T., Orito, M., Ichiki, K., Kawanomoto, S., Ando,
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Kajino, T., Orito, M., Mathews, G. J., and Boyd, R. N.:
2001, Lepton Asymmetric Universe: New Limits from
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Kajino, T.: 2001, Recent Progress in Cosmology and Nuclear
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Kawano, N., Hanada, H., Iwata, T., and Tsubokawa, T.:
2001, Japanese lunar explorer "SELENE" and geodetic
observations of the Moon, Astronomy and geodesy in new
millenium, 157‑160.
Kinoshita, D., Watanabe, J., Fuse, T., Pittichova, J., Meech,
K. J., Ash, S., Yamamoto, N., Buie, M. W., Wasserman,
L. H., Chiang, E., Jordan, A. B., Millis, R. L., Elliot, J. L.,
Kern, S. D., Trilling, D. E., Clancy, K. D., and Marsden,
B. G.: 2002, 2001 DU108, Minor Planet Electronic Circ.,
2002‑F27.
61

Kinoshita, D., Watanabe, J., Fuse, T., Yamamoto, N. andMarsden, B. G.: 2002, 2001 DS108, Minor Planet Electronic Circ., 2002‑D10.
Kinoshita, D., Watanabe, J., Fuse, T., Yamamoto, N., andMarsden, B. G.: 2001, 2001 DM108, Minor Planet Electronic Circ., 2001‑V26.
Kinoshita, D., Watanabe, J., Fuse, T., Yamamoto, N., andMarsden, B. G.: 2001, 2001 DO108, Minor Planet Electronic Circ., 2001‑V30.
Kinoshita, D., Watanabe, J., Fuse, T., Yamamoto, N., andMarsden, B. G.: 2001, 2001 DQ108, Minor Planet Electronic Circ., 2001‑X26.
Kinoshita, D., Watanabe, J., Fuse, T., Yamamoto, N., andMarsden, B. G.: 2001, 2001 DR106, Minor Planet Electronic Circ., 2001‑J33.
Kinoshita, D., Watanabe, J., Fuse, T., Yamamoto, N.,
Yoshida, F., Trujillo, C. A., Brown, M. E., Helin, E. F.,
Pravdo, S., Lawrence, K., Hicks, M., and Marsden, B. G.:
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Kinoshita, H., and Nakai, H.: 2001, Stability Mechanism of
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Koda, J., and Wada, K.: 2001, Probability of Overestimating Central Galactic Mass Using Rotation Curves, The
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Kohno, K., Matsushita, S., Vila-Vilaro, B., Okumura, S.
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Kiloparsec of Starbursts and AGN: The La Palma Connection", eds. J. H. Knapen, J. E. Beckman, I. Shlosman,and T. J. Mahoney, ASP Conf. Ser., 249, 672.
Koike, C., Shibai, H., Tanabe, T., Suto, H., Sogawa, H.,
Kaito, C., Ando, Y., and Fukada, M.: 2002, The opticalproperties of carbon and graphite depend on crystal structure and temperature, IAU Symp., 187, 227.
Kokubo, E., and Ida, S.: 2001, Lunar Formation from a
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Korchagin, V., Tsuchiya, T. and Miyama, S. M.: 2001,
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K., Oshima, Y., Terazono, J., Umehara, H., Urata, T.,
Yoshikawa, M., Ezaki, Y., Maeno, H., Suzuki, M. Kadota,
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Sorai, K.: 2001, Dense Molecular Gas in Early-Type
Galaxies, Proc. of "The Central Kiloparsec of Starbursts
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Kuno, N., Nishiyama, K., Nakai, N., Sorai, K., Vila-Vilaro,B., and Handa, T.: 2001, Distribution and Kinematics ofMolecular Gas in NGC 3504, Proc. of "Galaxy Disks and
Disk Galaxies", eds. J. G. Funes, S. J., and E. M. Corsini,
ASP Conf. Ser., 230, 379‑380.
Lites, B. W., Socas-Navarro, H., Skumanich, A., and Shimizu,
T.: 2001, Converging Flows in the Penumbra of a DeltaSunspot, Magnetic Fields across the Hertzsprung-Russell
Diagram, eds. G. Mathys, S. K. Solanki, and D. T.
Wickramasinghe, ASP Conf. Ser., 248, 143.
Loiubtchenko, S. Yu., Popov, M. V., Hirabayashi, H., andKobayashi, H.: 2001, Original Major L-Band Interference Received by the HALCA Space Radio Telescope,Proc. of IAU Symp. on "Preserving the astronomical sky",eds. R. J. Cohen and W. T. Sullivan, III, 196, 335‑340.
Majumdar, S., Nath, B. B., Chiba, M.: 2001, Galactic Winds
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Malhotra, R., Holman, M. and Ito,T.: 2001, Chaos andStability of the Solar System, Publ. Natl. Acad. Sci., 98,
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Manteca, J., Naves, N. R., Campas, M., Asami, A., Asher, D.
J., Fuse, T., Hashimoto, N., Ibrahim, A. I., Isobe, S.,
Nishiyama, K., Oshima, Y., Terazono, J., Umehara, H.,
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H., Wakuda, S., Rodriguez, J., Sanchez, S., Durig, D. T.,
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Masaki, Y., and Kinoshita, H.: 2001, For Construction of
Analytical Expressions of Nereid's Motion Perturbed by
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Mech., eds. E. Kokubo, T. Itoh, and H. Arakida, 189‑216.
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Matsumoto, H., Tsuru, T. G., Matsushita, S., Harashima, T.,
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M82, Proc. of "New Century of X-Ray Astronomy", eds. H.
Inoue and H. Kunieda, ASP Conf. Ser., 251, 60‑63.
Matsuo, H., Ariyoshi, S., Takeda, M., Noguchi, T.: 2001,
SIS Photon Detectors for Submillimeter-wave Observations, Proc. of the 12th International Symp. on Space
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Matsushita, S., Kawabe, R., Matsumoto, H., Tsuru, T. G.,
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M82: Superbubble, Starburst, and Massive Black Hole,Proc. of "The Central Kiloparsec of Starbursts and AGN:
The La Palma Connection", eds. J. H. Knapen, J. E.
Beckman, I. Shlosman, and T. J. Mahoney, ASP Conf.
Ser., 249, 711‑714.

Miyata, T., Kataza, H., Okamoto, Y., Sako, S., Takubo, S.,
Onaka, T., and Yamashita, T.: 2001, Spatially Resolved
Spectra of the Red Rectangle in the N-band, ASP Conf.
Ser., 265.
Miyazaki, A., and Tsuboi, M.: 2001, Mass Spectrum of thegalactic Center Molecular Clouds, Proc. of the IAU Symp.
205, "Galaxies and their constituents at the highest angular resolutions", eds. R. T. Schilizzi, S. N. Vogel, F.
Paresce, and M. S. Elvis, 356‑357.
Miyazaki, S.: 2001, Weak Lensing Observation using
Suprime-Cam, RESCUE International Symp., 217. (invited)
Nagashima, M., Totani, T., Gouda, N., and Yoshii, Y.:
2001, Galaxy Number Counts in a Hierarchical Galaxy
Model, The Physics of Galaxy Formation, 283‑288.
Nagayama, T., Nagashima, C., Nakajima, Y., Zenno, T.,
Nagata, T., Sato, S., Tamura, M., Nakaya, H., andSugitani, K.: 2001, SIRIUS - Simultaneous three-color
InfraRed Imager for Unbiased Surveys, ASP Conf. Ser.,
232, 389‑391.
Nakajima, Y., Nagashima, C., Nagayama, T., Nagata, T.,
Kato, D., Kurita, M., Kawai, T., Sato, S., Tamura, M.,
Nakaya, H., and Sugitani, K.: 2001, A Deep Near Infrared
Survey of Selected Regions of the Southern Sky withSIRIUS, ASP Conf. Ser., 232, 455‑457.
Nonaka, K., Sawabe, M., Isobe, S., Hashimoto, N., Yokota,
T., and Kameyama, M.: 2001, Overview of BSGC observation system and NASDA orbit determination system,
Conf. Proc. of the Airforce Maui Observatory Systems,
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Nonaka, K., Sawabe, M., Yokota, T., Isobe, S., Hashimoto,N., and Kameyama, M.: 2001, Some results of GEO spacedebris observation and orbital Determination under Experimental Operation, Proc. of the Third European Conf.
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Ohta, K., and Akiyama, M.: 2002 GRB02033 NIR observation at KPNO, GRB Circular Network, 1320, 1.
Ohtani, H., Hattori, T., Miyazaki, S., Iye, M., Komiyama,Y., Sasaki, T., Kosugi, G., and Subaru team.: 2001, HyperFine Feature of Dust Distribution in the Central Region of
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Ohyama, Y., Hamana, T., Kashikawa, N., Chiba, M., andFutamase, T.: 2001, Subaru Spectroscopy of the Gravitational Lens HST 14176+5226: Implications for a Large
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Ohyama, Y., Yoshida, M., Kawabata, K. S., Saito, Y.,
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Iye, M., Ogasawara, R., Takata, T., Sekiguchi, K.,
Yamada, T., Kobayashi, N., Watanabe, J., Totani, T.,
Yoshida, A., Kawai, N., Urata, Y., Tamagawa, T., Torii,
K., Noumaru, J., Komiyama, Y., Aoki, W., and Motohara,
K.: 2002, GRB020305: Subaru optical observations, GRB
Circular Network, 1271, 1.
Okiura, M., Kohno, K., Okumura, S. K., Shibatsuka, T.,
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Onishi, T., Mizuno, A., Kawamura, A., and Fukui, Y.:
2001, Protostellar Collapse in Dense Cores in Taurus,
Proc. of "Science with the Atacama Large Millimeter
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150‑153.
Ono K., Tajima, T., Mizutani, A., Taromaru, Y., Isobe S.,
Takano, T., Sato T.: 2001, Development of the first Japanese space Debris Observation radar, Proc. of the Third
European Conf. on Space Debris, 73‑78.
Ouchi, M., Shimasaku, K., Furusawa, H., Miyazaki, M.,
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Komiyama, Y., Miyazaki, S., Nakata, F., Sekiguchi, M.,
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07.01.
Parthasarathy, M., Takeda, Y., Aoki, W., Ita, Y., Nakada,Y., Izumiura, H., Ando, H., and Karoji, H.: 2001, Analysis of the HDS Spectrum of a Very Metal-Poor Post-AGB
Star HR4049, Subaru Users Meeting 2001, 298‑307.
Preston, R. A., Lister, M. L., Tingay, S. J., Piner, B. G.,
Murphy, D. W., Jones, D. L., Meier, D. L., Pearson, T. J.,
Readhead, A. C. S., Hirabayashi, H., Kobayashi, H., andInoue, M.: 2001, Pearson-Readhead Survey from Space,
Proc. of the IAU Symp. 205, "Galaxies and their constituents at the highest angular resolutions", eds. R. T. Schilizzi,
S. N. Vogel, F. Paresce, and M. S. Elvis, 124‑125.
Pyo, T.-S., Hayashi, M., Kobayashi, N., Terada, H., Goto,
M., Yamashita, T., Tokunaga, A. T., Itoh, Y.: 2001,
Subaru Telescope NIR Echelle Spectroscopy of L1551
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Raju, K.-P., Sakurai, T., and Ichimoto, K.: 2001, A Spectroscopic Study of the Solar Corona from Norikura and
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Symp., 203, 488.
Sakurai, T.: 2001, Stokes Profile Inversion without Resort
to Specific Atmospheric Models, Advanced Solar Polarimetry - Theory, Observation, and Instrumentation, ed.
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Sato, K., Yoshizawa, M., Nishikawa, J., Fukushima, T.,
Ohishi, N., Torii, Y., Matsuda, K., Kubo, K., Iwashita,
H., Suzuki, S., Saint-Jacques, D., Nemoto, Y., and Kotani,T.: 2001, The second stage interferometer MIRA-I.2 ofMitaka optical and InfraRed Array (MIRA ) project, The
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Sawada, T., Hasegawa, T., Handa, T., and Jim Cohen, R.:
2001, A Molecular Face-On View of the Galactic Center,
Proc. of the international spring meeting of "Dynamics ofStar Clusters and the Milky Way", eds. S. Deiters, B.
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Sawada-Satoh, S., Inoue, M., Shibata, K. M., Kameno, S.,
Nakai, N., Migenes, V., and Diamond, P. J.: 2001, HI and
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of the IAU Symp. 205, Galaxies and their constituents at63

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Vogel, F. Paresce, and M. S. Elvis, 196‑197.
Sekiguchi, K., Takata, T., Simpson, C., and Akiyama, M.:
2001, Subaru Deep Survey, ASP Conf. Ser., 232, 458.
Sekimoto, Y., and LMSA working group: 2001, The Atacama
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Shen, Z-Q., Edwards, P. G., Kameno, S., Inoue, M., andLovell, J. E.: 2001, Space VLBI Observations of PKS
1921-293, Proc. of the IAU Symp. 205, "Galaxies andtheir constituents at the highest angular resolutions", eds.
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128‑129.
Shibata, K., and Yokoyama, T.: 2001, Origin of Universal
Correlation between Temperature and Emission Measurefor Solar/Stellar Flares, Proc. of IAU Symp. 203, "Recent
Insights into the Physics of the Sun and Heliosphere: Highlights from SOHO and other Space Missions", eds. P.
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Shibatsuka, T., Kohno, K., Matsushita, S., and Kawabe,
R.: 2001, Multiline Observations of Molecular Gas in theCentral Region of the "Low Star Formation Efficiency"
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Sorai, K., Nakai, N., Kuno, N., and Nishiyama, K.: 2001,
HCN/CO Radio in the Nuclear Regions and the Disks of
Nearby Spiral Galaxies, Proc. of "Galaxy Disks and Disk
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Conf. Ser., 230, 385‑386.
Sudou, H., Taniguchi, Y., Kaburaki, O., Ohyama, Y.,
Kameno, S., Sawada-Satoh, S., Inoue, M., and Sasao, T.:
2001, A Sub-PC-Scale Acceleration of the Radio Jet of
NGC 6251, Proc. of the IAU Symp. 205, "Galaxies andtheir constituents at the highest angular resolutions", eds.
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Sugiyama, N.: 2001, Anisotropies of cosmic microwave
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Z. G. Deng, Y. P. Jing, and G. Boerner, Progress in
Astronomy Supp., 19, 1‑5.
Sugiyama, N.: 2001, Dark Ages can be seen by Cosmic
Microwave Background, Proc. of the 4th RESCEU international Symp. on "Birth and Evolution of the Universe",
eds. K. Sato, and M. Kawasaki, 147‑150.
Sugiyama, N.: 2001, Time Scales of Cosmic Microwave
Background Radiation: Gold Mine in the Universe, Proc.
of "Astrophysical Ages and Time Scales", eds. T. Hippel,
C. Simpson and N. Manset, Astronomical Society of the
Pacific Conf. Ser., 245, 603‑610.
Takami, H., Takato, N., Kanzawa, T., Hayano, Y.,
Kamata, Y., Gaessler, W., Minowa, Y., Iye, M.: 2001,
The first light of Subaru adaptive optics system, VeniceConf. on "Beyond Conventional Adaptive Optics".
Tamura, M., Suto, H., Murakawa, K., Hayashi, S., Kaifu,
N., Itoh, Y., Fukagawa, M., Oasa, Y., and Naoi, T.: 2001,
64

Coronagraphic Imager with Adaptive Optics (CIAO) for
the Subaru 8.2m Telescope, Bull. AAS, 198, 7704.
Tanaka, I., Yamada, T., Turner, E. L., and Suto, Y.: 2001,
Superclustering of Galaxies Traced by a Group of QSOs
at z = 1.1, Proc. of an international workshop: QSO hosts
and their environments, 351‑353.
Tanikawa, K. and Yamaguchi, Y.: 2001, Forcing relationsof symmetric non-Birkhoff periodic points in the Standard-like mappings, in the Proceedings of 33rd symposium on 'Celestial Mecahanics', 309‑329.
Tatematsu, K., Arikawa, Y., Sekimoto, Y., and Mt. Fuji
Submillimeter-wave Telescope Team: 2001, Submillimeter-Wave and Millimeter-Wave Observations of the Interaction of Supernova Remnants with Molecular Clouds,
Explosive phenomena in astrophysical compact objects :first KIAS astrophysics workshop, eds. H.-Y. Chang, C.H. Lee, M. Rho, I. Yi, AIP conf. proc., 556, 382‑388.
Ticha, J., Tichy, M., Jelinek, P., Galad, A., Kornos, L.,
Dauvergne, J. L., Demeautis, C., Matter, D., Merlin, J.
C., Postel, J. B., Pozzoli, V., Naves, N. R., Campas, M.,
Asami, A., Asher, D. J., Fuse, T., Hashimoto, N., Ibrahim,
A.I., Isobe, S., Nishiyama, K., Oshima, Y., Terazono, J.,
Umehara, H., Urata, T., Yoshikawa, M., Ezaki, Y.,
Akahori, A., Maeno, H., Suzuki, M., Kadota, K., Abe, H.,
Seki, T., Stevens, B., Testa, A., Cavagna, M., Rodriguez,J., Serra, F., Kagawa, T., and Marsden, B. G.: 2002,
COMET C/20, Minor Planet Electronic Circ., 2002‑D36.
Ticha, J., Tichy, M., Kocer, M., Jelinek, P., Barbieri, C.,
Pignata, G., Magrin, S., Bertini, I., Hahn, G., Hoffmann,M., Mottola, S., Galad, A., Kornos, L., Cernis, K.,
Laugalys, V., Daugirdas, D., Manteca, J., Dauvergne, J.
L., Demeautis, C., Matter, D., Merlin, J. C., Postel, J. B.,
Pozzoli, V., Buzzi, L., Naves, N. R., Campas, M., Reina,
L. E., Ligustri, R., Asami, A., Asher, D. J., Fuse, T.,
Hashimoto, N., Ibrahim, A. I., Isobe, S., Nishiyama, K.,
Oshima, Y., Terazono, J., Umehara, H., Urata, T.,
Yoshikawa, M., Biggs, J., Ezaki, Y., Maeno, H., Kadota,
K., Nakamura, A., Abe, H., Seki, T., Sugie, A., Garradd,
G.J., Camarasa, Y. M., Rodriguez, D., Gilmore, A. C.,
Testa, A., Cavagna, M., Helin, E. F., Pravdo, S., Lawrence,
K., Kervin, P., Maeda, R., Africano, J., Hicks, M., Casas,R., Josa, R., Lopez, J., Pinto, M., Spratt, C. E., Hovland,E., Bickler, T., Schroeder, J., Scherr, L., Thicksten, R.,
Deetz, A., Scotti, J. V., Tubbiolo, A. F., Van Ness, M. E.,
Blythe, M., Shelly, F., Bezpalko, M., Huber, R., Manguso,
L., Adams, S., Piscitelli, J., Stuart, J., Sayer, R., Evans, J.
B., Viggh, H., Robinson, L., Elliott, R., Hainaut, O. R.,
Akiyama, M., Hale, A., Ferrando, R., and Marsden, B.
G.: 2002, OBSERVATIO, Minor Planet Electronic Circ.,
2002‑D38.
Tichy, M., Ticha, J., Galad, A., Gajdos, S., Asami, A., Asher,
D. J., Fuse, T., Hashimoto, N., Ibrahim, A. I., Isobe, S.,
Nishiyama, K., Oshima, Y., Terazono, J., Umehara, H.,
Urata, T., Yoshikawa, M., Ezaki, Y., Kwon, S.-G., Kim,
S.-L., Kadota, K., Garradd, G. J., Pravec, P., Kusnirak,
P., Smalley, K., Roland, S., Aoki, M., Kushida, Y., Mas,
A., Hale, A., and Marsden, B. G.: 2002, COMET C/20,
Minor Planet Electronic Circ., 2002‑E43.
Tomisaka, K.: 2001, Outflow from YSO and Angular Mo-

mentum Transfer, IAU Simp. 200, "The Formation of
Binary Stars'', 401‑405.
Tosaki, T., Hasegawa, T., Shioya, Y., Kuno, N., andMatsushita, S.: 2001, Molecular Clouds and Star Formation in M51, Proc. of "The Central Kiloparsec of Starbursts
and AGN: The La Palma Connection", eds. J. H. Knapen,
J. E. Beckman, I. Shlosman, and T. J. Mahoney, ASP Conf.
Ser., 249, 723‑726.
Tsuboi, Y., Koyama, K., Hamaguchi, K., Tatematsu, K.,
Sekimoto, Y., Balley, J., and Reipurth, B.: 2001, Discovery of X-Rays from Class 0 Protostar Candidates, Proc.
of "New Century of X-Ray Astronomy", eds. H. Inoue andH. Kunieda, ASP Conf. Ser., 251, 18‑21.
Tsujimoto, T., Shigeyama, T., and Yoshii, Y.: 2001, Theoretical interpretation of abundance trends seen in extremely
metal-poor stars, Cosmic evolution, 219‑220.
Tsujimoto, T., Yoshii, Y., and Kawara, K.: 2002, Ageproblem based on the abundance ratio from a high-redshift QSO, Cosmic chemical evolution, IAU Symp., 187,
153‑157.
Usuda, T., Kobayashi, N., Terada, H., Matsushita, S.,
Tsuru, T. G., Harashima, T., Matsumoto, T., Kawabe,R., Goto, M., and Tokunaga, A.: 2001, Near IR Imaging
and Spectroscopy of an Intermediate Mass Black Hole
Candidate in M 82, Proc. of the "Astrophysical Ages andTime Scale", eds. T. von Hippel, C. Simpson, and N.
Manset, ASP Conf. Ser., 245, 454‑456.
Vila-Vilaro, B., Butner, H. M., Bieging, J. H., Matsushita,S., and Kohno, K.: 2001, High-Density and Temperature
Molecular Gas at the Centers of M51 and NGC 1068,
Proc. of "The Central Kiloparsec of Starbursts and AGN:
The La Palma Connection", eds. J. H. Knapen, J. E.
Beckman, I. Shlosman, and T. J. Mahoney, ASP Conf.
Ser., 249, 727‑730.
Wada, K., and Fukuda, H.: 2001, Gas Dynamics andFueling Processes in the R < 0.1-1 kpc Region, The Physics of Galaxy Formation, 261‑266.
Wada, K.: 2001, Two and Three dimensional structure of
the Inhomogenous Gas Dynamics in the Central Kpc, The
central kpc of starbursts and AGN: the La Palma connection, 249, 679‑685.
Watanabe, J., Fukushima, H., and Nakamura, T.: 2001,
The Activity Profile of Comet 55P/Tempel-Tuttle in 1998
return: Meteoroid Release Concentration on the Perihelion , Proc. Meteoroids 2001 Conf., ESA SP‑495, 175‑
177.
Watanabe, J., Fukushima, H.: 2001, Revealing Variety of
Comets by Long-Term Monitoring Observation of a 50cm Telescope, Small-Telescope Astronomy on Global
Scales, IAU Coll. 183, eds. W. P. Chen, C. Lemme, B.
Paczynski, ASP Conf. Ser., 246, 265‑270.
White, S. M., Kundu, M. R., Garaimov, V. I., andYokoyama, T.: 2001, The Physical Properties of a Flaring
Coronal Loop, American Geophysical Union, Spring
Meeting 2001, abstract #SP42A‑06.
Yamaguchi, Y. and Tanikawa, K.: 2001, Forcing relationsof non-Birkhoff periodic points in forced pendulums,
Proc. of 33rd symp. on 'Celestial Mecahanics', 330-350.
Yano, T., Chiba, M., and Gouda, N.:2001, Kinematics of

the Spiral Structure of our Galaxy, The Physics of Galaxy
Formation, 427‑430.
Yokono, Y., Inutsuka, S., Miyama, S., Ogasawara, R.,
Takeuchi, T. and Chikada, Y.: 2001, Development ofSpecial Purpose Computer for Cosmic Hydrodynamics
with SPH Method, New horizons of computational science, Proc. of the international symp. on supercomputing
held in Tokyo, Japan, September 1-3, 1997, ASSL, 263,
309.
Yokoyama, T., Akita, K., Morimoto, T., Inoue, K., andNewmark, J.: 2001, Observation of Reconnection Inflow
of a Solar Flare, Proc. of IAU Symp. 203, "Recent Insights
into the Physics of the Sun and Heliosphere: Highlightsfrom SOHO and other Space Missions", eds. P. Brekke,
B. Fleck, and J. B. GurmanManchester, 203, 344.

5. Presentations
Abe, M., Ohba, Y., Ishiguro, M., Hasegawa, S., Fuse, T.,
Aoki, K., Ohyama, Y., Kashikawa, N., The Focas Team,
Tokunaga, A., Goto, M., Usuda, T., Terada, H.,
Kobayashi, N., The Ircs Team, and Fujiwara, A.: 2002,
Physical Model and Taxonomic Type of 1998 SF36, theTarget Asteroid of Sample Return Mission, MUSES-C,
33rd Annual Lunar and Planetary Science Conference,(Houston, Texas, March 11‑15).
Abe, S., Watanabe, J., Yano, H., and Ebizuka, N.: 2001,
Spectroscopic Study of Meteor and Persistent Train, Meteoroids 2001, 4-1, (Swedish Institute of Space Physics,
Kiruna, Sweden, August 6‑10).
Agata, H., Kawai, K., Okuno, H., Naitoh, S.: 2001, Remote
Telescope for HOU activity at Tokyo Science Museum,2nd Conference on Global Science Education and An International Workshop for Coordinating a Scalable andSustainable Small Automated Telescope Network(Lawrence Berkeley, U.S.A., July 25‑29).
Akiyama, M.: 2001, AGN Samples from Optical Identification of ASCA Surveys, IAU Coll. 184, AGN Surveys,(Byurakan, Armenia, Jun. 18‑22).
Akiyama, M.: 2001, Fibre Multi Object Spectrograph for
Subaru Telescope, Next Generation Wide-Field MOS
workshop, (Tucson, Oct. 11).
Arai, K., and the TAMA collaboration: 2001, Sensing andcontrols for power-recycling of TAMA300, 4th Amaldi
Conference on Gravitational Waves (Perth, Jul. 8‑13).
Baba, H., Yasuda, N., Ichikawa, S., Yagi, M., Iwamoto,N., Takata, T., Horaguchi, T., Taga, M., Watanabe, M.,
Ozawa, T., and Hamabe, M.: 2001, Development of the
Subaru-Mitaka-Okayama-Kiso Archive System, Astronomical Data Analysis Softwares and Systems XI,(Victoria, BC, Canada, Sep. 30‑Oct. 3).
Chikami, I., Agata, H., Goshima, M., Matsumoto, N., Ueda,
S.: 2001, JAHOU and Japanese Science Education, 2nd
Conference on Global Science Education and an International Workshop for Coordinating a Scalable and Sustainable Small Automated Telescope Network, (Lawrence
Berkeley, U.S.A., July 25‑29).
Culhane, J. L., Doschek, G. A., Watanabe, T., Lang, J.:
2001, The Solar-B Mission - Instruments and Scientific65Aims, (EGS, April).
Goto, M., Kobayashi, N., Terada, H., Takato, N., Gaessler,
W., Takami, H., Hayano, Y., Tokunaga, A. T., Potter, D.,
and Cushing, M.: 2001, Near Infrared AO Spectroscopyof Binary Brown Dwarf Discovered in HD 130948 triple
system, American Astronomical Society Meeting 199,
61.01.
Gouda, N., Tsujimoto, T., Kobayashi, Y., Nakajima, T.,
Yasuda, N. and Matsuhara, H.: 2001, Japanese Astrometry
Satellite Mission for Infrared Exploration, Census of the
Galaxy: Challenges for Photometry and Spectrometry with
GAIA, (Vilnius, Lithuania, July 2‑6).
Hanada, H., Iwata, T., Kono, Y., Matsumoto, K., Tsuruta,
S., Ishikawa, T., Asari, K., Ping, J., Heki, K. and
Kawano, N.: 2002, VRAD mission; precise observationof sub-satellites in SELENE with international VLBI Network, 2nd. IVS General Meeting.
Hara, H.: 2002, Changes of Coronal Structures over the 11year Solar Cycle, Multi-Wavelength Observations of Coronal Structure and Dynamics, Yohkoh 10th Anniversary
Meeting, (Kona, U.S.A., Jan. 21‑24).
Hayano, Y., Takami, H., Takato, N., Kamata, Y.,
Kobayashi, N., Minowa, Y., Iye, M.: 2002, Laser guidestar adaptive optics for Subaru telescope. Lasers for Adaptive Optics in Astronomy, (SSL, UC Berkeley, and Berkeley Marina Radisson Hotel, March 20‑21).
Heki, K.: 2001, Seasonal loads, crustal deformation, andseismicity in Japan, AGU Fall Meeting, (San Francisco,Dec. 10‑14).
Heki, K.: 2001, Seasonal modulation of interseismic strain
build-up in an island arc driven by snow loads, IAG 2001
Scientific Assembly, (Budapest, Sep. 2‑7).
Honma, M.: 2001, Current Status of VERA project, 5th
East-Asia Meeting, (Taiwan, Nov. 13‑16)
Honma, M.: 2001, VERA - Science (invited), 2001 AsiaPacific Radio Science Conference, (Tokyo, Aug. 4‑6).
Ichimoto, K.: 2002, OTA Status Report, 3rd Solar-B Science Meeting, (Hawaii, Jan. 25‑26).
Ichimoto, K.: 2002, Solar-B Observation Program - A Personal View, 3rd Solar-B Science Meeting , (Hawaii, Jan.
25‑26).
Imanishi, M.: 2002, 3-4 µm Spectroscopy of Seyfert 2
Nuclei to Quantitatively Assess the Energetic Importanceof Nuclear Starbursts, AAS meeting, (USA, Washington
DC, Jan 6‑10).
Iwamoto, N., Kajino, T., Mathews, G. J., Fujimoto, M. Y.,
and Aoki, W.: 2001, Discovery of Early Generation sprocess rich Star and the Nucleosynthesis, International
Conference on Nuclear Data for Science and Technology,(Tsukuba, Oct. 7‑12).
Iwamoto, N., Wanajo, S., Kajino, T., Kubono, S., Ogawa,K., and Nomoto, K.: 2001, rp-process Nucleosynthesis in
ONeMg Novae and the Nuclear Flow Path, International
Symposium on Clustering Aspects of Quantum ManyBody Systems, (Kyoto, Nov. 12‑14).
Iwata, T., Sasaki, T., Kono, Y., Hanada, H., Kawano, N.,
Namiki, N.: 2001, Results of the critical design for theselenodetic mission using differential VLBI methods by
SELENE, 2nd. IVS General Meeting, (Taipei, Nov. 12‑66

16).
Iye, M.: 2002, Active and Adaptive Optics of the 8.2m
Subaru Telescope and future telescopes, Proc. CRL International Symp. on Light Propagation and Sensing Technologies for Future Applications, (Tokyo, Mar. 13‑14).
Kajino, T., Orito, M., Mathews, G. J., and Boyd, R. N.:
2001, Universal Lepton Asymmetry: New Constraints
from the Cosmic Microwave Background and Primordial
Nucleosynthesis, International Workshop on Particle
Physics and the Early Universe COSMO-01, (Finland,Aug. 30‑Sep. 4).
Kajino, T.: 2001, Cosmological Nucleosynthesis in BigBang and Supernovae, International Conference on Nuclear
Data for Science and Technology, (Tsukuba, Oct.7‑12).
Kajino, T.: 2001, Recent progress in cosmology and nuclear
physics, Yukawa International Seminar 2001 (YKIS01)
Physics of Unstable Nuclei, (Kyoto, Nov. 5‑10).
Kajino, T.: 2002, New Constraints on Massive Degenerate
Neutrinos from Primordial Nucleosynthesis and Cosmic
Microwave Background Fluctuations, Fourth HEIDELBERG International Conference on Dark Matter in Astroand Particle Physics, (South Africa, Feb.4‑9).
Kawakita, H., Watanabe, J., Fuse, T., Furusho, R., Abe, S.:
2002, Spin Temperature of Cometary Ammonia determined from NH2, IAU Coll. No.186, Cometary Science
After HALE-BOPP, 52, (Spain, Jan. 21‑25).
Kawamura, S.: 2001, The Current Status of the GroundBased Laser-Interferometric Gravitational Wave Antennas, 16th International Conference on General Relativity& Gravitation, (Durban, Jul. 16).
Kawano, N., Hanada, H., Iwata, T. and Tsubokawa, T.:
2001, Japanese lunar explorer "SELENE" and geodetic
observations of the Moon, Astronomy and geodesy in new
millenium.
Kodama, T., Arimoto, N., Barger, A., and AragonSalamanca, A.: 2001, IAU Symp. 187, 226, (Kyoto, Aug.
26‑30).
Kokubo, E., and Ida, S.: 2001, Lunar Accretion from an
Impact-Generated Disk, IAU Symp. 208, AstrophysicalSupercomputing Using Particle Simulations, (Tokyo, July.
10‑13).
Kono, Y., Hanada, H., Kawano, N., Iwadate, K., Koyama,
Y., Fukuzaki, Y.: 2002, Precise positioning of spacecrafts
by multi-frequency VLBI, 2nd. IVS General Meeting.
(Tsukuba, Feb. 4‑8).
Manabe, S., Imai, H., Jike, T., and VERA analysis software group: 2002, Astrometric and geodetic analysis system of VERA, IVS General Meeting, (Tsukuba, Feb. 4‑8).
Mariska, J. T., Brown, C. M., Dere, K. P., Doschek, G. A.,
Korendyke, C. M., Culhane, J. L., Watanabe, T.: 2001,
The Extreme Ultraviolet Imaging Spectrometer on SolarB, AGU, (May).
Mathews, G. J., Ichiki, K., Kajino, T., Orito, M., andYahiro, M.: 2001, Constraining Cosmic Quintessence, International Workshop on Particle Physics and the Early
Universe COSMO-01, (Finland, Aug. 30‑Sep. 4).
Matsumoto, K., Heki, K., and Hanada, H.: 2002, Global
lunar gravity field recovery from SELENE, 2nd. IVSGeneral Meeting.

Matsuo, H.: 2001, Large Aperture Submillimeter-wave
Space Telescope, Asia-Pacific Radio Science Conference,(Tokyo, Aug. 1‑4).
Matsuo, H.: 2001, Observation of Sunyaev-Zel'dovich effects with the Nobeyama 45-m telescope, Tracing Cosmic Evolution with Galaxy Clusters, Sesto Pusteria, (Italy,
July 3‑6).
Nagashima, M., and Gouda, N.: 2001, Galaxy Number
Counts in a Hierarchical Galaxy Formation Model, Studies of Galaxies in the Young Universe with New Generation Telescopes, (Sendai, Jul. 24‑28).
Nagashima, M., Yoshii, Y., Totani, T., and Gouda, N.:
2001, Galaxy Number Counts in the Subaru Deep Field: A
Constraint on a Hierarchical Galaxy Formation Model,
New Trends in Theoretical and Observational Cosmology, 5th RESCEU International Symp., (Tokyo, Nov.13‑
16).
Nakamura, T., Asakura, S., Tsuda, T., Ueda, M., and
Watanabe, J.: 2001, Observation of Leonid Activity in1998 and 1999 with the MU Radar and an All-sky TV
Camera, Meteoroids 2001, (Sweden, August 6‑10).
Ohyama, Y., Hamana, T., Kashikawa, N., Chiba, M., andFutamase, T.: 2001 Subaru Spectroscopy of the Gravitational Lens HST 14176+5226: Implications for a Large
Cosmological Constant, American Astronomical Society
Meeting, 199, 16.16.
Pyo, T.-S., Hayashi, M., Kobayashi N., Terada, H., Goto,
M., Yamashita, T., Tokunaga, A. T., Itoh, Y.: 2001,
Subaru Observation of the L1551 Jets, East Asian Meeting of Astronomy V, (Taiwan, Nov. 13‑16).
Shibasaki, K.: 2001, Signature of Energy Release and Particle Acceleration Observed by the Nobeyama
Radioheliograph "CESRA Workshop", (Munich, July 2‑
6).
Shimizu, T.: 2001, The Solar Corona, 4th Japanese American Frontiers of Science (JAFoS4) 2001 Tokyo Symp.
(Tokyo, Oct. 9‑12).
Shimizu, T.: 2002, Connection between Photospheric Magnetic Fields and Coronal Structure/Dynamics, Multi-Wavelength Observations of Coronal Structure and Dynamics,
Yohkoh 10th Anniversary Meeting, (Hawaii, Jan. 21‑24).
Shimizu, T.: 2002, Solar-B Operations Planning - Introduction (Strawman), 3rd Solar-B Science Meeting, (Hawaii,Jan. 25‑26).
Shimojo, M., Hara, H., and Kano, R.: 2001, The temperature analysis of Yohkoh/SXT data using the CHIANTI
spectral database Multi-Wavelength Observations of Coronal Structure and Dynamics, Yohkoh 10th Anniversary
Meeting, proc. of the conf., (Hawaii, Sep. 17‑20).
Sugiyama, N.: 2001, CMB Probe the Dark Ages, The 8th
Taipei Astrophysics Workshop AMiBA 2001 "High-z
Clusters, Missing Baryons, and CMB Polarization", (Taiwan, Jun.11‑15).
Takagi, T., and Arimoto, N.: 2001, The spectral evolution of
elliptical galaxies in FIR and beyond, IAU Symp. 187,
237, (Kyoto, Aug. 26‑30).
Takahashi, R., Arai, K., and the TAMA collaboration:
2001, Improvement of the vibration isolation system for
TAMA300, 4th Amaldi Conference on Gravitational

Waves, (Perth, Jul. 8‑13).
Takahashi, R., Fukushima, M., Arai, K., Tatsumi, D.,
Heinzel, G., Kawamura, S., Yamazaki, T., Saito, Y.,
Ando, M., Moriwaki, S.: 2001, Direct Measurement ofResidual Gas Effect on the Sensitivity in TAMA300,
IUVSTA 15th International Vacuum Congress, (San Francisco, Oct. 29‑Nov. 2).
Takami, H., Takato, N., Hayano, Y., Kanzawa, T.,
Gaessler, W., Minowa, Y., Iye, M., Saint-Jacques, D.:2001, Subaru AO 1st light, proc. of the conf., (Venice,May 7‑10).
Tamura, Y., VERA Group: 2002, Geodetic Observation
System in VERA, IVS General Meeting, (Tsukuba, Feb.
4‑8).
^
Tanikawa, K. and Soma,
M.: 2001, Reliability of the totality of the eclipse in AD628 in the Nihongi, International
Conf. on the 770th Birth Anniversary of Guo Shoujing andthe Histories of Time Apparatus, (China, Oct. 18‑22).
Terasawa, M., Sumiyoshi, K., Kajino, T., and Mathews, G.
J.: 2001, r-Process Nucleosynthesis in Type-II Supernova
Model with Neutron Star Mass ~ 1.4MX, International
Symp. on Clustering Aspects of Quantum Many-Body
Systems, (Kyoto, Nov.12‑14).
Tsujimoto, T., Shigeyama, T., and Yoshii, Y.: 2001, The
Site for r-process Nucleosynthesis, The Evolution of Galaxies. II- Basic Building Blocks, (France, Oct. 16‑21).
Tsujimoto, T.: 2002, Inhomogeneous Chemical Evolution
and the Production Site for r-Process Elements, Low Z at
Low z and High z: Early Chemical Evolution, (USA, Mar.
21‑23).
Tsujimoto, T.: 2002, Inhomogeneous Chemical Evolution
and the Production Site for r-Process Elements, Stellar
Abundances & Nucleosynthesis Conf., (USA, Mar. 27‑
29).
Tsukamoto, T., Abe, S., Ebizuka, N., Yano, H., Hirahara, Y.,
and Watanabe, J.: 2001, Spectroscopic Analysis of Fine
Structures in Leonids, Meteoroids 2001, (Sweden, August 6‑10).
Wada, K.: 2001, 2-D and 3-D inhomogeneous gas dynamics
in the central kpc, The Central KPC in Galaxies, (Spain,
May 6‑11).
Watanabe, J., Fukushima, H., and Nakamura, T.: 2001,
The Activity Profile of Comet 55P/Tempel-Tuttle in 1998
return: Meteoroid Release Concentration on the Perihelion, Meteoroids 2001, PSA‑14, (Swedish Institute ofSpace Physics, Kiruna, Sweden, August 6‑10).
Watson, M. G., and Sekiguchi, K.: 2001, First XMMNewton results from the Subaru Deep Survey region, Two
Years of Science with Chandra, (Washington DC, Sep. 5‑
7).
Yamada, T., Kajisawa, M.: 2001, Deep Near-Infrared
Imaginmg of Galaxies at z~2 with Subaru, Mass of Galaxies at Low and High Redshift, (Venice, Oct.).
Yano, H., Abe, S., Ebizuka, N., Fujino, N., and Watanabe,J.: 2001, Fine Structures within the Leonid Dust Trail:
Resonant Filament Model Examined by Optical Video Observations, Meteoroids 2001, (Swedish Institute of Space
Physics, Kiruna,
Yano, T., Kan-ya, Y., and Gouda, N.: 2001, Dynamics of67

Stellar Orbits in Disk Galaxies, The 5th RESCEU International Symp.: New Trends in Theoretical and Observational Cosmology, (Tokyo, Nov. 13‑16).
Yokoyama, T., and Shibata, K.: 2001, MHD Simulation of
a Solar Flare & Derived Scaling Law between the Temperature and the Emission Measure of Stellar/Solar Flares,
Stellar Coronae 2001, (Snowmass, Jun. 25‑29).
Yokoyama, T., Nakajima, H., and Shibasaki, K.: 2001,
Microwave Observation of Rapid Propagation of a NonThermal Source in a Solar Flare by Nobeyama
Radioheligoraph, CESRA Workshop, (Munich, Jul. 2‑6).
Yokoyama, T., Nakajima, H., and Shibasaki, K.: 2001,
Statistical Study of Spatial Distribution of Non-thermal
Microwave Index in Flare Loops, CESRA Workshop,(Munich, July 2‑6).
Yokoyama, T.: 2001, CME and Flares on 1999-3-18, SHINE
workshop, (Snowmass, June 17‑21).
Yokoyama, T.: 2001, Numerical Simulation of a FlareMulti-Wavelength Observations of Coronal Structure andDynamics, Yohkoh 10th Anniversary Meeting, Proc. of aconf., (Hawaii, Sep. 17‑20).
Yokoyama, T.: 2001, Our Active Star, the Sun, 4th Japanese-American Frontiers of Science Symp., (Tokyo, Oct.
10‑12).
Yoshida, H.: 2001, Non-existence of the modified first
integral by symplectic integration methods, CELMECH
III meeting, (Italy, Jun. 25‑31).
Yoshida, H.: 2001, Non-preservation of super-integrabilityof Hamiltonian systems by symplectic integration methods, SciCADE'01 meeting, (Canada, Jul. 25‑31).

68