Ⅰ Scientific(April 2002 -March

Highlights
2003 )

1 . The First Stellar Fringes Observed with
Mitaka Optical /IR Array (MIRA -I .2) 30m Baseline .......................................................... YOSHIZAWA
2 . Development of the Solar -B X -Ray Telescope Focal Plane Camera ................................................... KANO
3 . Thermo -Optical Testing of the Solar Optical Telescope of the Solar -B ..................................... ICHIMOTO
4 . ALMA Cartridge -type Receiver System on ASTE ........................................................................ SUGIMOTO

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5 . Gravitational Wave Detector TAMA300 Power Recycling andInternational Joint Observation ................................................................................................... FUJIMOTO
et al .
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6 . New Limits on the Mass of the Milky Way
SAKAMOTO
et al .
7 . Kinematics of Tidal Debris from ω Centauri ʼs Progenitor Galaxy ............................................. MIZUTANI
et al .
8 . Gravity -Driven Turbulence in Galactic Disks ......................................................................................... WADA et al .
9 . Detection of crystalline silicates in the protoplanetary disk around the T Tauri starHen 3 ‑600A .......................................................................................................................................... HONDA et al .
10. Error Estimation of the Doppler Measurements for Gravity Field Recovery of
the Far -side of the Moon ....................................................................................................................... KONO et al .
11. Microwave Imaging Observation of High -Energy Electron Propagation ina Solar Flare .................................................................................................................................. SHIBASAKIet al .
12. Investigation of Supernova Nucleosynthesis from Elemental Abundances ofMetal -Deficient Stars ................................................................................................................................ AOKI et al .
13. Centroid Experiment of Artificial Stars ................................................................................................... ARAKI et al .
14. Prominence Eruptions and Coronal Mass Ejection :A Statistical Study Using Microwave Observations ....................................................... GOPALSWAMY
et al .
15. Two Types of Shock -waves and Selective Acceleration of High -Energy Particles ......................................... OHKI
16. Molecular Outflow Search in the ρOphiuchus A and B2 Regions ......................................... KAMAZAKI
et al .

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17. Deep Imaging Observations of the Lupus 3 Cloud :Dark Cloud Revealed as Infrared Reflection Nebula ............................................................ NAKAJIMA
et al .
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18. Optical Spectropolarimetry of SN 2002ap with Subaru Telescope
KAWABATAet al .
19. Compact Nuclear Starbursts in Seyfert 2 Galaxies ..................................................................................... IMANISHI

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20. Size Distribution of Sub -km Main Belt Asteroids Derived from
Subaru Telescope Observations ...................................................................................................... YOSHIDA
21. Plug -In Cryogenic System for Cartridge -Type SIS Receivers .................................................. YOKOGAWA
22. Seismic Noise Reduction of a Gravitational Wave Detector at the Kamioka Mine .................. TATSUMI
23. Construction and Enlargement of Dilatonic Wormholes by Impulsive Radiation ..................... KOYAMA
24. Near Infrared ［Fe II ］Spectroscopy of Young Stellar Outflows .............................................................. PYO
25. Observations of Ammonia in Starburst Galaxies NGC 253 and M 82 ......................................... TAKANO
26. Kinematic Analysis of Spiral Structures in the Local Disk .................................................................. YANO
27. On Stationarity of Spiral Structure in Disk Galaxies ............................................................................. YANO
28. Revised Fluorescence Efficiencies of Cometary NH : Ammonia Abundance in Comets ..... KAWAKITA
29. Heliocentric Dependence of the Sodium Emission of Comet 153P /Ikeya -Zhang ................. WATANABE
30. Dense Molecular Gas in Lenticular Galaxies .......................................................................................... KUNO
31. A Noise Evaluation of a High Output Power W -band Photomixer .................................................... UEDA
32. K3 ‑50A : An Ultracompact HII Region Ionized by Multiple Ionizing Stars ............................ OKAMOTO
33. Relations between Galaxy Formation and Environments of Quasars ................................................ ENOKI

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34. Observation of Solar Flare Hard X -ray Spectra using CdTe Detectors ................................. KOBAYASHI
35. Observational Study of the Three -Dimensional Magnetic Field Structure andMass Motion in Active Regions ........................................................................................... CHOUDHARY
36. Subaru /XMM -Newton Deep Survey .............................................................................................. SEKIGUCHI
37. The Evolution of Vector Magnetic Fields in an Emerging Flux Region ............................................ KUBO
38. Searching for Dark Matter Halos in the Suprime -Cam 2 Square Degree Field ...................... MIYAZAKI
39. Fabrication of a Bandpass Filter for the Solar Optical Telescope of Solar -B using the IBS .... WASEDA
40. Formation of Protoplanet Systems and Diversity of Planetary Systems ........................................ KOKUBO
41. Spectroscopic Observation of Coronal Waves ................................................................................... SAKURAI
42. Spectroscopic Studies of the Solar Corona Using Fe X , XIII , XIV Lines ....................................... SINGH
43. Measurement of Magnetic Helicity Injection andFree Energy Loading into the Solar Corona ................................................................................ KUSANO
44. The Source of Magnetic Field Twist in Solar Active Regions ................................................................. BAO
45. Relation between Pressure Balance Structures and Polar Plumes from
Ulysses High Latitude Solar Wind Observations ................................................................... YAMAUCHI
46. Dynamical Ordering of Accelerator Modes ............................................................................... YAMAGUCHI
47. Observational Constraints on Dark Radiation in Brane Cosmology ................................................. ICHIKI.....................................SUMIYOSHI
48. Astrophysical Reaction Rate for α(αn , γ) Be by Photodisintegration2

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PREFACE
We report here the achievements by NAOJ during thefinancial year 2002 . Please find the details in each fieldpresented in the following text sections .
The NAOJ started its history as an inter -university
national research institute in 1988 . During the followed 15
years the NAOJ had pushed forward the frontier in various
fields of astronomy by developing and operating top level
observational facilities ; the Radio Heliograph at Nobeyama
for solar activity monitoring , the 8.2-m Subaru Telescope at
Mauna Kea , Hawaii for optical and IR observations , four
20-m aperture high performance antennas of the VERA
project at Mizusawa , Kagoshima , Chichi -Jima and Ishigaki -Jima for VLBI astrometry . Also
new bases to respond to the varying requests from scientific and public communities had beenfounded at headquarters in Mitaka , Tokyo , by establishing the super computer system for thetheoretical simulation astrophysics , the world -first gravitational telescope TAMA -300, theAdvanced Technology Center for astronomical engineering , and the Public Relations Center
for a variety of outreach activities . Such improvements of research platforms and scientificactivities of the NAOJ throughout these 15 years are quite high and successful . Sincere
thanks to the community , staff members and leaders for their tremendous efforts .
As mentioned above , the NAOJ is promoting manifold fields of astronomy and astro physics including various ground -based astronomy and theoretical astrophysics . Anotherrole of NAOJ as an inter -university national research institute is to provide top -level facilities
for university scientists as well as to represent the Japanese astronomy and astrophysics onbehalf of astronomical community in Japan . Based on these characteristics the NAOJ has
been promoting the research and education of astronomy , and tried to respond to the strong
public interest about the universe .
The observations of the universe are now growing rapidly . One of the most epoch making progresses is a sequential discovery of extra -solar planets since 1995 . The astronomy
is entering into the era to observe and study the numerous number of planets and even theevidence of life on them . Another exciting new observational data from WMAP arerevealing the early history of the expanding universe and suggested the existence of “
darkenergy ”. The observational cosmology is getting more excitement through the activities of
8-m class telescopes including the Subaru Telescope which is rewriting the distance record of
the remote galaxies . The construction of the ALMA , an extremely large mm and sub -mm
wave telescope array atop the Atacama Plateau in northern Chile will start soon . Japan(NAOJ ) will also join the construction , and the ALMA will be the first telescope which is
jointly constructed by the world -wide cooperation . The full operation of ALMA will startin 2011 .

The reorganization of all Japanese national universities and inter -university research
institutes to be independent agencies from April FY2004 is another major subject for NAOJ .
Intensive discussions are ongoing in NAOJ and among the brother institutes to create a
flexible and active organization for powerful research in wide area of natural sciences .

Norio Kaifu
Director General
National Astronomical

Observatory of Japan

The First Stellar Fringes Observed with Mitaka
IR Array (MIRA -I .2) 30m Baseline

Optical /YOSHIZAWA, Masanori , OHISHI , Naoko , SUZUKI , Shunsaku
MATSUDA , Ko , KUBO , Koichi , IWASHITA , Hikaru(Division

NISHIKAWA(Divisionof Astrometry and Celestial Mechanics , NAOJ ), Jun , TORII , Yasuo

SATO , Koichi(Division

KOTANI , Takayukiof Optical and Infrared Astronomy , NAOJ )of Earth Rotaion , NAOJ )FUKUSHIMA(Public Relations

The first detection of stellar fringes with MIRA -I .2(Mitaka oprical /IR Array second phase ) was achieved ona night of June 2002 during the observations of Vega (Lyr ［) 1 ］. After the first detection , many fringe observa tions were carried out successfully using Vega and Deneb( Cyg ) until December 2002 (Figure 1).
MIRA -I .2 is an optical interferometer for high spatial
resolution stellar observations consisting of two 30cm
siderostats that are placed separated by 30m to each other(Figure 2). The suitable range of apparent stellar diame ter to be observed with MIRA -I .2 is between 2 and 4
milli -arc -second at 800nm wavelength . The first action
for developing the components of MIRA -I .2 began in
1995 . Then baseline construction and laboratory setup
were started in 1999 , followed by the stellar fringe detec -(Univ . of Tokyo ), Toshio

YOKOI , Takuya

Center , NAOJ )(Hosei Univ .)tion with a 6m test baseline in June 2001 prior to thepresent first fringes by using the 30m baseline .
In each telescope hut , a 30cm siderostat , a 13cm
Newtonian telescope with a collimator lens , and a tip -tilt
mirror are placed (Figure 3). The star light is lead fromeach hut to the main laboratory through the vacuum
pipe -line of about 50 m long . In the laboratory , an 8 m
vacuum delay line (Figure 4), 4m coarse delay line , light
dividing optics , detectors for scintillation and star danc ing measurements , beam combining optics and fringe
detectors (Figure 5), and computers for control and data
［2 ］
［3 ］
acquisition , are placed ［1 ］.
After the test observations , MIRA -I .2 has been up graded for regular observations of stars brighter than 4
mag .
References［1 ］Nishikawa , J.: 2003 , Proc . SPIE , 4838 , 101.
［2 ］Ohishi , N ., Matsuda , K ., Torii , Y ., Nishikawa , J., Yoshizawa ,M ., Sato , K ., Kubo , K ., Iwashita , H ., Kotani , T., Fukushima , T.:2003 , Proc . SPIE , 4838 , 736.
［3 ］Sato , K ., Nishikawa , J., Yoshizawa , M ., Ohishi , N ., Fuku shima , T., Torii , Y ., Matsuda , K ., Kubo , K ., Iwashita , H ., Suzuki ,S ., Kotani , T., Yokoi . T.: 2003 , Proc . SPIE , 4838 , 1072 .

Figure 1: Fringes of Vega and Deneb

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Figure 2 : Mitaka optical and InfraRed Array 30m baseline(MIRA -I .2).

Figure 3 : Optics in the North observing hut .

Figure 4 : 8 m vacuum optical delay line .

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Figure 5 : Optical table in the main laboratory .

Developmentof the Solar -B X -Ray Telescope Focal Plane Camera

KANO , Ryouhei , HARA , Hirohisa , KUMAGAI, Kazuyoshi , SAWA , Masaki , TSUNETA, Saku(Solar Physics Division , NAOJ )SAKAO , Taro , MATSUZAKI, Keiichi(The Institute of Space and Astronautical
The Solar -B satellite is scheduled for launch in sum mer 2006 by the Institute of Space and Astronautical
Science (ISAS ). Its goal is to better understand theoverall magnetohydrodynamic
behavior of the sun byobserving the solar corona , chromosphere and photos phere . The X -Ray Telescope (XRT ) is one of three
instruments on Solar -B and is designed to image the solar
corona in the soft X -ray. Soft X -ray images reveal tem perature distributions and magnetic field structure of thesolar corona , allowing us to observe the energy transport ,storage and release process starting from the photosphereand extending throughout the corona .
The XRT is a grazing incidence telescope similar to
the Soft X -ray Telescope (SXT ) on the Yohkoh satellite ,but with several major improvements : (1) By combining alarger aperture (34 cm ) and higher precision mirror system with a larger focal plane detector (2k 2k pixel
CCD ), spatial resolution has been increased to 1 arc second while retaining a sufficient field of view to image
the whole sun . (2) The use of a backside illuminated
CCD allows the XRT to observe longer wavelength
radiation , up to the 〜60A and longer XUV range . This
allows observation of 1 million K plasma in addition to
the 2 million K and higher temperatures observed by the
Yohkoh SXT . (3) Using an optimized set of diagnostic
filters , the XRT can observe and distinguish different
temperature plasma from 1million K to the super ‑hot 30
million K flares . (4) The control system is based on theobservation table system proven on the Yohkoh SXT , butwith the addition of onboard image analysis by thesatellite ʼs Mission Data Processor (MDP ) which allows
automatic adjustment of exposure and imaging region .
The CCD is mounted on an adjustable focus stage
with a ±1mm range along the optical axis . This elimi nates the risk of focal adjustment error which would
otherwise be difficult in a telescope of this size . In
addition , because of the curved focal plane of the tele scope , focal adjustment allows us to choose between
maximum resolution at image center or optimal focus
over a larger field of view to match those of the other
instruments on the satellite , the Solar Optical Telescope
and the EUV Imaging Spectrometer .
The XRT is a collaboration with the Smithsonian
Astrophysical Observatory (SAO ) and NASA in the
USA . The Japanese participants , NAOJ and ISAS , arein charge of the design and construction of the X ‑ray
CCD camera and the MDP . The camera contains a
cooling system based entirely on radiative cooling , since
thermoelectric coolers can cause outgas that leads tocontamination of the detector . The camera is designed
to achieve an on ‑orbit CCD temperature of ‑45 C . The
CCD charge is read out at 500k ㎐ and readout noise of〜20e has been achieved .

Science )The flight CCD camera was assembled in the ProjectRoom 1 in the NAOJ Advanced Technology Center(ATC ), recently converted into a class 100 cleanroom toeliminate molecular and dust contamination . The per formance and functionality of the camera is being verified
thanks to the cooperation of the ATC machine shop andoptical shop . Tests included (a) X ‑ray quantum efficiency measurements in the medium vacuum chamberusing an interchangeable target X ‑ray generator and X‑ray monochromator , and CCD gain measurement using
an Fe source , (b) Testing and verification of the focus
mechanism through thermal tests , and (c) Vibration andshock tests conducted at ISAS .
After testing in Japan , the camera will be shipped to
SAO in summer of 2003 and mated to the telescope
optical tube . The complete telescope will be tested in the
USA and be shipped to ISAS for satellite integration testin May 2004 .

Figure 1: Flight CCD camera , shown with the radiator side up
to cool the CCD .

Figure 2: CCD camera mounted in the ATC medium vacuum
chamber for X -ray quantum efficiency measurement .

5

Thermo -Optical Testing of the Solar Optical Telescope of the Solar -B
ICHIMOTO, Kiyoshi , NAKAGIRI , Masao , SUEMATSU
TAMURA , Tomonori , TSUNETA , Saku
(Division

NOGUCHI, Yoshinori ,of Solar Physics , NAOJ ), Motokazu , KATO , Yoshihiro(Norikura

Solar Observatory , NAOJ )OTSUBO , Seiji(Advanced Technology Center , NAOJ )KATSUKAWA, Yukio , KUBO , Masahito(Tokyo University )1. Introduction
The Optical Telescope Assembly (OTA ) of the Solar B consists of a Gregorian telescope with 500mm apertureand 1500mm distance between the primary and secondary
mirrors and Collimating Lens Unit (CLU ) sending aparallel beam to the focal plane package . The OTA is
aimed to perform a precise polarimetric measurement of
the solar atmosphere from space with a diffraction limited
spatial resolution . The OTA assemble test using proto model mirrors and structures was performed in 2001 -2002
and we established the procedure to realize the diffraction
limited telescope . However , the optical performance was
evaluated only under the room temperature . Extremely
different temperature distribution is expected in orbit ; i.e.
the difference of temperature between the top part of OTA
which is exposed to space and the bottom parts of OTA
which is surrounded by spacecraft structure will be larger
than 50 C . To achieve the positional stability of the
primary and secondary mirrors with a micron -orderprecision under such severe temperature condition has
been a challenging goal of the structural design of OTA ,and we absolutely need to verify it before launching the

Figure 1: Configuration

6of the OTA thermo -optical testing .

telescope . In order to confirm the optical performance of
OTA under the space environment , we constructed a
dedicated vacuum chamber and performed the thermo optical test of the OTA .
2. Overview of the thermo -optical testing
The vacuum chamber for thermo -optical testing has adiameter of 1800mm and height of 4000mm , and has
upper and lower shrouds in it . The OTA is mounted
inside the shrouds with upside down via three legs of thestructural interface to the space craft . The temperaturesof the top and bottom parts of OTA are controlled in dependently by the shrouds in a range of ‑30 C to ＋
50 C . On the base of the chamber , a 60cm diameter flat
mirror is mounted in face to the OTA aperture to provide
a optical reference , and in combination with the interfer ometer mounted on the outside wall of the chamber , we
can measure the wave front error of the OTA in vacuum .
By measuring the tilt of the flat mirror and the alignment
cube attached on OTA structure , we can also evaluate theexcursion of the OTA pointing axis with respect to themechanical reference .
3. Results
The OTA thermo -optical test was performed from 28
January to 4 March in 2003 at the Structure andmechanics test building of ISAS . By simulating thepredicted hot and cold case temperatures and operating
the operational heaters for mirrors successively , we perfor med the measurements of wavefront error , focus shift andpointing axis of the OTA . The major results are sum marized below :1) The sensitivity of the OTA focus position on tempera tures of various parts of OTA was measured reliably .
They are mostly as predicted but a few unexpectedbehaviors were found and the hardware causing theFigure 2: View of the OTA thermo -opitical testing

effect will be modified in flight model .
2) The CFRP truss structure of OTA changes its dimen sion gradually due to dehydration in vacuum . The
effect was previously known , but the amount and thetime constant were evaluated accurately for the firsttime . This result together with the finding 1) gives us
valuable information for initial setup of the on -orbit
focus adjustment mechanism and its operation .

3) Change of the OTA wavefront error was observed withthe change of temperature of the primary mirror . The
major component of the change was caused by apredicted stress from the metal pads of the primary
mirror . However we also observed unexpected compo nent of the wavefront error . The supporting mecha nism of the primary mirror will be partially modified inflight model to mitigate the unexpected stress to themirror . We confirmed that the temperature excursionof other parts of OTA does not cause any significant
wavefront degradation (i.e. positional change of pri mary and secondary mirrors ).
4) There was no detectable change of the pointing axis .
With the OTA thermo -optical testing , we could verify
the overall healthiness of the OTA structure , whilesome problems to be solved were identified at the sametime . It can be said that we are approaching the final
goal to realize the diffraction limited telescope . The
vacuum chamber was moved to the new clean room in
Mitaka after the OTA thermo -optical test and is going
to be used continuously for the baking of the OTA
flight components . The second (final ) thermo -optical
test with the OTA flight model is planned in spring of2004 .

7

ALMA

Cartridge -type Receiver

System on ASTE

SUGIMOTO , Masahiro , SEKIMOTO , Yutaro ,YOKOGAWA, Sozo , OKUDA , Takeshi , TATEMATSU , Ken ʼ
ichi(NAOJ )

KOHNO , Kotaro

OGAWA , Hideo , KIMURA(Institute of Astronomy , University of Tokyo )SUZUKI, Kimihiro(Osaka Prefecture University ), Kazuji , MINAMIDANI, Tetsuhiro(Nagoya University )Figure 1: (a) A photograph of carrying the receiver system into
the receiver cabin . (b) A photograph before instal lation of the receiver system . (c) A photographafter installation . Bottoms of three cartridges andthe cryocooler are seen . The warm IF amplifiers
and bias electronics are not mounted .

We have developed an ALMA cartridge -type receiversystem composed of three cartridge -type receivers and acryostat , which is designed to test on the Atacama Submil limeter Telescope Experiment (ASTE ). It was prelimi nary evaluated at Pampa la Bola (alt . 4800m ) in thenorthern Chile since November 2002［1 ］.
A cartridge -type cryostat , which can house 3 cartrid getype receivers , has been developed for the ASTE . The
ASTE 10m telescope has been developed as a prototype
antenna of the Large Millimeter Submillimeter Array . It
was installed on Pampa la Bola following evaluation at
Nobeyama .
The detail of this cryostat was described by［2 ］. The
cylindrical cryostat can accommodate 2 cartridges of
170mm diameter and 1 cartridge of 140mm diameter .
The cryostat has been developed with following technol ogies ; a central pipe and bellows structure to reducemechanical vibration ; simple and e.cient thermal links forplug -in cartridges ; 3-stage Gifford McMahon cryocooler
and an outdoor compressor .
The concept of the thermal link for the ALMA
receiver was proposed by the Rutherford Appleton Labo ratory (RAL )［3 ］. We have designed and developed asimple and efficient thermal link with high heat conduc tivity ［4 ］
. Measured thermal conductance of φ170mm
links is 1.7, 5.6, 3.3 W K
for 4, 12, and 80K stages .
This simple and compact links have good performanceand can be easily fabricated .
［6 ］
［7 ］,
Engineering models of band 3 (100 GHz )［5 ］
band 8 (500 GHz ), and band 10 (800 GHz ) cartridge -type
receivers were independently developed with cartridgetest
cryostats (See［8 ］for more details of cartridge -test cryos tats ). They were integrated into the cryostat at NAOJ ,then the system was shipped to the site .
8

In November 2002 , 3 cartridge -type receivers were
installed to the ASTE and its photograph is shown in
Figure 1. At the ASTE site , we checked vacuum condi tion of the cryostat and electronic condition of threecartridgetype receivers . Then , the cryostat was attachedunder the Cassegrain focus . On 17 November 2002 , wedetected continuum signals from the moon with all threereceivers . The moon and Jupiter efficiency of the band 3
receiver were 90% and 73% at 100 GHz , respectively . The
pointing accuracy at 498 GHz was about 1 , which
derived from measurements of the Jupiter and the Saturn .
In spite of not adjusting tilt parameters of the subre
reflector , the moon and Jupiter efficiency were 82% and 42% , respectively . After waiting good atmospheric condi tion (τ＜1.3) in several days , on 9 December 2002 , weobserved a spectrum of CI (rest frequency ＝492.16 GHz )from Orion (Figure 2). At that night , the optical depth
at zenith was 〜1.0 and the system noise temperature wasaround 1000K .
We confirmed that the system including three receivers
operates as designed and the concept of cartridge -type
receiver system is very promising for the ALMA .

Figure 2: A spectrum of CI ( P ‑ P ) from Orion KL . The
beam is averaged over 2 arcminutes . H CO (491.97
GHz ) and CH OH (492.28 GHz ) lines also weredetected . Integration time was 1 minute .
References［1 ］Sugimoto et al .: 2003 , ALMA memo , 458.
［2 ］Yokogawa et al .: 2003 , PASJ , 55, L519 .
［3 ］Orlowska et al .: 2002 , ALMA project book , Chapter 6.
［4 ］Sugimoto et al .: 2003 , Cryogenics , in press .
［5 ］Ogawa et al .: 2002 , Proc . IAU 8th APRM , 2, L23 .
［6 ］Asayama et al .: 2003a , Int . J . Infrared and Millimeter Waves ,in press .
［7 ］Asayama et al .: 2003b , ALMA memo , 453.
［8 ］Sekimoto et al .: 2003 , ALMA memo , 455.

Gravitational
Wave Detector TAMA300
Power Recycling and International
Joint Observation
FUJIMOTO, Masa -Katsu , KAWAMURA, Seiji , YAMAZAKI, Toshitaka , TAKAHASHI , Ryutaro
ARAI , Koji , TATSUMI , Daisuke , FUKUSHIMA, Mistuhiro
SATO , Shuichi , NAGANO , Shigeo , TSUNESADA , Yoshiki , and the TAMA collaboration(Divisionof Astrometry and Celestial Mechanics , NAOJ )We report on the implementation of power recyclingof the TAMA300 gravitational wave detector and on the
joint observation period , which exceeded 1,000 hours , byan international network of GW detectors .
The goal of power recycling is to improve the shot noise limited sensitivity by increasing the “effective laser
power ”to the interferometer . This is realized by anadditional recycling mirror between the laser source andthe interferometer , composing an optical cavity with theinterferometer . The total optical configuration becomes
a complicated coupled -cavity system because the Michel son interferometer also contains Fabry -Perot cavities in
its arms . TAMA300 was first successfully operated withpower recycling in the end of 2001 , a few months after
installation . In summer 2002 , considerable improvement
in sensitivity was achieved after a period of optimizationand noise reduction . Signal enhancement by power
recycling , a modified laser frequency stabilization system ,an improved laser intensity stabilization system , and areduction of scattered light contributed to improving thissensitivity . The resulting noise curve has a best sensitiv ity of 1 ×10 mHz
in displacement around 1kHz .
The “binary inspiral range ”, which is the distance theantenna can detect the chirping signals generated by the
coalescence of 1.4M , compact star binaries with an SNR

Figure 1: The interferometer displacement sensitivity . The
best sensitivity for the non -recycled FPMI is shownby the black curve and for the recycled FPMI by the
red curve . The sensitivity was considerably im proved in the higher frequency region above around
1kHz , where the shot -noise is expected to be domi nant .

of 10, exceeds 30 kpc , so the TAMA300 is sensitive
enough to detect an intergalactic gravitational wave event .
As large -scale gravitational wave antennae elsewherearound the world were also becoming operational , anobservation
networkfor GWs
began this year .
TAMA300 participated in an international joint observa tion with the LIGO interferometers (U .S .) for two months
from February to April 2003 (DT8 ). This was the first ,real , joint observation in a sense that the participatinginterferometers were sensitive enough to detect GW events
within our galaxy . The interferometer was operated for1158 hours out of 1424 hours during DT8 , even though
the interferometer had became a complicated coupledcavity system . The duty cycle reached 81.3% , which wascomparable with that of the non -recycled FPMI system(86.5% ), so the power recycled interferometer showedsufficient stability for long -term operation . Of the inter ferometers in the observation network , TAMA300 had thehighest duty cycle (The LIGO interferometers duty cycle
was typically 40-70% ).
Recorded observational data was distributed to data
analysis groups in real -time via superSINET
networksystem , and was analyzed promptly . A preliminary
result of a GW search from the TAMA300 data (single
detector ) is that the upper limit of the event rate ofcoalescence of 1.4M . compact star binaries within ourgalaxy was determined to be 0.0033 event /hour (90% C .
L .). This value was improved by a factor of 3 comparedwith the value from DT6 (0.0095 ), reflecting the improved
sensitivity . Further analysis is ongoing .

Figure 2: Observation status during DT8 . Each green box
shows the period when TAMA300 was fully opera tional and valid data was recorded .

9New Limits on the Mass
SAKAMOTOof the Milky, Tsuyoshi , CHIBA , Masashi(Graduate University for Advanced Studies /NAOJ )We set new limits on the mass of the Milky Way ,making use of the latest kinematic information for Galac tic satellites and halo objects . Our sample consists of 11
satellite galaxies , 137 globular clusters , and 413 fieldhorizontal -branch (FHB ) stars up to distances of 10 kpc
from the Sun . Roughly half of the objects in this sample
have measured proper motions , permitting the use of theirfull space motions in our analysis . In order to bind thesesample objects to the Galaxy , their rest -frame velocities
must be lower than their escape velocities at their esti mated distances . This constraint enables us to show thatthe mass estimate of the Galaxy is largely affected byseveral high -velocity objects (Leo I , Pal 3, Draco , and a
few FHB stars ), not by a single object alone (such as Leo
I ), as has often been the case in past analyses . We alsofind that a gravitational potential that gives rise to a
declining rotation curve is insufficient to bind many of
our sample objects to the Galaxy ; a possible lower limiton the mass of the Galaxy is about 2.2 ×10 M . To be
more quantitative , we adopt a Bayesian likelihood
approach to reproduce the observed distribution of thecurrent positions and motions of the sample , in a pre scribed Galactic potential that yields a flat rotation curve .
This method enables a search for the most likely total
mass of the Galaxy , without undue influence in the final
result arising from the presence or absence of Leo I ,provided that both radial velocities and proper motions
are used . Although the best mass estimate depends some what on the model assumptions , such as the unknown
prior probabilities for the model parameters , the resultant
systematic change in the mass estimate is confined to a
relatively narrow range of a few times 10 M , owing toour consideration of many FHB stars . The most likely
×10 M
total mass derived from this method is 2.5
×10 M (excluding Leo(including Leo I ), and 1.8

10

Way

BEERS , T. C .
(Michigan

State Univ .)I ). The derived mass estimate of the Galaxy within the
distance to the Large Magellanic Cloud (〜50 kpc ) isessentially independent of the model parameters , yielding
×10 M (including Leo I ) and 5.4
×10 M
5.5
(excluding Leo I ). Implications for the origin of halo
microlensing events (e.g., the possibility of brown dwarfs
as the origin of the microlensing events toward the LMC ,may be excluded by our lower mass limit ) and prospects
for more accurate estimates of the total mass are also
discussed .
Reference［1 ］Sakamoto , T., Chiba , M ., & Beers , T. C .: 2003 , Astron . Astro phys ., 397, 899 ‑911.

Figure 1: Likelihood contours in the plane of the mass , M , andvelocity anisotropy , β, obtained from an analysis
that uses both radial velocities and proper motions .
Solid and dashed curves show the results including
Leo I and excluding Leo I , respectively ; the cross andthe asterisk show the maxima of the probabilities foreach case .

Kinematics
MIZUTANIof Tidal Debris from ω Centauri ʼsProgenitor Galaxy, Arihiro , CHIBA , Masashi , SAKAMOTO, Tsuyoshi(Graduate University for Advanced Studies /NAOJ )Omega Centauri , the most massive globular cluster inthe Milky Way , is unique in terms of its stellar popula tion : unlike other Galactic globular clusters , ω Censhows a wide spread in metallicity distribution and inter nal kinematics . Also , the metal -rich sub -population inω Cen is largely enhanced in s -process elements relative
to the stars in other clusters with similar metallicities ,thereby suggesting that the ejecta from low -mass , AGB
stars had to be retained and incorporated into the next generation stars . However , in spite of its large mass (5 ×
10 M ), ω Cen is not unique in its ability to retain the
AGB ejecta as found for other clusters . An isolated
formation of ω Cen is thus unlikely , because the enrichedgas would easily be lost by encountering the Galactic
disk . The most viable explanation for the uniqueness ofω Cen is that it was once the dense nucleus of a nucleateddwarf galaxy . A gravitational potential provided byprogenitor ʼs stellar system and dark matter would help
retaining the enriched gas and let the cluster being self enriched at least over a few Gigayears .
If this hypothesis is the case for the origin of ω Cen ,the question arises : where and in what form does thestellar system of its progenitor galaxy remain ?
We have conducted an N -body simulation for the tidal
disruption of a dwarf galaxy , based on the hypothesis thatits central part once contained ω Cen . Dynamical evolu tion of a self -gravitating progenitor galaxy that follows
the present -day and likely past orbits of ω Cen is calcu lated numerically and the kinematic nature of their tidal
debris is analyzed , in comparison with various observa tions showing signatures of recent merging events in the
Milky Way . In particular , we have found that the retro grade rotation of the debris stars at 〜100 km s accords

with a recently discovered , large radial velocity stream at〜300 km s towards the Galactic longitude of 〜270 .
Further searches for this merging siganture in the Milky
Way , e.g., by the SDSS and RAVE projects , are worth
exploring .
Reference［1 ］Mizutani , A ., Chiba , M ., Sakamoto , T.: 2003 , Astrophys . J .,589, L89 ‑92.

Figure 1: Upper (middle ) panel shows the spatial distributionof the tidally disrupted debris for model 1 (model 2)
after the 1.37 (1.86) Gyr orbital excursion of ω Cen ʼsprogenitor galaxy . Lower panel shows the orbit of
the galaxy center for model 1 (dotted line ) and 2(solid line ). A frame measures 15 kpc on a side ofeach panel , where the Sun is located at x ＝−8 kpc
and xy corresponds to the disk plane .

11Gravity -Driven Turbulencein Galactic

Disks

WADA , Keiichi(Divisionof Theoretical Astrophysics , NAOJ )MEURER, G ., NORMAN(Johns Hopkins
High -resolution , 2-D hydrodynamical
simulations
with a large dynamic range are performed to study the
turbulent nature of the interstellar medium (ISM ) in
galactic disks . The simulations are global , where theself -gravity of the ISM , realistic radiative cooling , andgalactic rotation are taken into account .
In the analysis undertaken here , feedback processes
from stellar energy source are omitted . We find that thevelocity field of the disk in a non -linear phase shows asteady power -law energy spectrum over three -orders ofmagnitude in wave number . This implies that the ran dom velocity field can be modeled as fully -developed ,stationary turbulence . Gravitational and thermal insta bilities under the influence of galactic rotation contributeto form the turbulent velocity field . The Toomre effective Q value , in the non -linear phase , ranges over a wide
range , and gravitationally stable and unstable regions are
distributed patchily in the disk . These results suggestthat large -scale galactic rotation coupled with the self gravity of the gas can be the ultimate energy sources thatmaintain the turbulence in the local ISM .
We find that our models of turbulent rotating disks are
consistent with the velocity dispersion of an extended HI
disk in the dwarf galaxy , NGC 2915 , where there is no
prominent active star formation . Numerical simulations
show that the stellar bar in NGC 2915 enhances thevelocity dispersion , and it also drives spiral arms as
observed in the HI disk .

, C. A.

University )Figure 1: Two -dimensional distribution of the effective Q (r ,φ) (upper panel ) and the density Σ (r , φ) (lower
panel ) at t ＝48 Myr of the high resolution model(4096 zones ). All quantities to calculate the effective Q , i.e. the epicyclic frequency , surface densityand velocity dispersion are averaged in 100 ×60
sub -regions .

Reference［1 ］Wada K ., Meurer , G ., & Norman C . A .: 2002 , ApJ , 577, 197.

Figure 2: Numerical model of the extended HI disk of dwarf
galaxy NGC2915 . The two major spirals are for med due to the outer Lindblad resonance , which is
caused by the central stellar bar of the pattern speed
8 km s kpc .

12

Detectionof crystalline silicates in the protoplanetaryaround the T Tauri star Hen 3-600A
HONDA , Mitsuhiko

KATAZA(Univ . of Tokyo /Subaru Telescope , NAOJ )OKAMOTO, Yoshiko(Kitasato Univ .)MIYATA, Hirokazu(Institute of Space and Astronautical,Takashi(Univ . of Tokyo )YAMASHITA

Science ),Takuya(Subaru Telescope , NAOJ )SAKO , Shigeyuki , TAKUBO , Shinya

ONAKA , Takashi(Univ . of Tokyo /Subaru Telescope , NAOJ )(Univ . of Tokyo )Silicate dust shows spectral features in the mid infrared wavelengths . Observation and analysis of sili cate features provide information about composition ,amorphousness /crystallinity and size of silicate grains .
Previous observations indicate that the silicate dust iscompletely amophous in the interstellar matter (ISM ),which is supposed to be starting material of star andplanetary system formation . On the other hand , in theend of 80ʼ
s, striking evidence of crsytalline silicate dust
was discoverd in the cometary dust that is believed to bea primordial matters . The presence of crystalline silicate
in the cometary dust is contradictory with its formation
condition (〜30 K ), because crystallization of silicate
grains need thermal annealing at high temperature condi tion (more than 800 K ). Recently , a key to the origin of
crystalline silicate grains in the cometary dust was report ed. That was the detection of crystalline silicates aroundintermediate -mass pre main sequence stars (PMSs ), Her big Ae /Be stars . However , due to their faintness , there
was no clear detection of crystalline silicates dust aroundlow -mass PMSs , which might be more similar to the earlystage of our solar system than Herbig Ae /Be stars are .
High sensitivity of the COoled Mid -Infrared Camera
and Spectrometer (COMICS ) enabled us to obtain the
spectra of faint T Tauri stars for the first time . As aresult , we succeeded in detecting clear crystalline silicate
features in the spectrum of T Tauri star Hen 3-600A) for the first time . Our first clear detection(Figure 1,［1 ］
of crystalline silicates among T Tauri stars implies thatthe crsytallization of silicate grains might be an universal
event in the protoplanetary disks around young stars .
That would also explain the origin of crystalline silicate
grains in the cometary dust . Future observational
studies will make clear the relevance between the silicate
dust crystallization and planet formation processes .

disk

Figure 1: The 10μm spectrum of the T Tauri star Hen 3-600A .
The features are explained with a combination of
amorphous olivine (MgFeSiO ; dashed line ), crystal line forsterite (Mg SiO ; long -dashed line ), crystal line enstatite (MgSiO ; dotted line ), silica (SiO ;dotdashed line ).
Reference［1 ］Honda , M ., Kataza , H ., Okamoto , Y . K ., Miyata , T., Yamashita ,T., Sako , S ., Takubo , S ., and Onaka , T.: 2003 , Astrophys . J ., 585,
L59 .

13

Error Estimation of the Doppler Measurements
for Gravity Field Recovery of the Far -side of the Moon
KONO , Yusuke(Division

HANADAof Radio Astronomy , NAOJ )YAMAMOTO, Hideo , KAWANO(Division, Zenichi(Institute of Space and Astronautical
Doppler measurement of a spacecraft around theMoon or planets is one of the major methods to measure
the gravity fields . 2-way and 4-way Doppler measure ments for the global lunar gravity field recovery will be
carried out in SELENE project with the accuracies of 0.2
mm ･s and 0.5 mm ･s in range rate in 18 seconds
integration , respectively . Frequency instability of a frequency standard in a ground station is one of the error
sources . It has been estimated by a round trip test in aground station and a simple modeling of the frequency
instability so far. The more realistic model of the frequency instability of a ground station is applied to the testof Usuda Deep Space Center (UDSC ).
The measurement error σ due to the frequency insta bility of the ground station is given by
＝＜
＞＋＜
＞＋
(1)
where , are carrier frequencies of up -and downlinks ,respectively ,is the two sample standard devia tion with integration time and the measurement interval, and , are standard deviation of frequency instabil ity which are normalized by the carrier frequencies . The
first and second terms in Eq .(1) can be obtained by around trip test in the ground station . The result at
UDSC is shown in Figure 1. Because the third terms in
Eq .(1) cannot be obtained directly , it is estimated from a
5MHz reference signal based on H -maser which is sup plied to both up -and down -converters . The third term is＝obtained by using the relation, wherecan be calculated from measured phasenoise.
is a bias function which
depends on spectral type of the phase noise . Figure 2
shows the result at UDSC .
All the results of the test indicates that the Doppler
system at UDSC has capability of Doppler measurements
within the expected accuracy for gravity field recovery of
the far-side of the Moon .

14, Nobuyuki

of Earth Rotation , NAOJ )Science )Figure 1: Round trip test at UDSC . S -S and S -X band indicate
2- and 4-way Doppler , respectively .

Figure 2: Two sample standard deviation of the 5MHz reference signal 2 (2, 2.6sec., )Microwave

Imaging Observation of High -Energy Electron
Propagation in a Solar FlareSHIBASAKI, Kiyoto , NAKAJIMA(Division, Hiroshi , YOKOYAMAof Radio Astronomy , NAOJ )Melnikov , V . F .
(Radiophysical

Stepanov , A . V .

Research Institute , Russia )Solar flares are phenomena in which high -temperatureplasma and high -energy particles are produced in a shortinterval of time . The mechanism of flares is not yet fully
understood . Especially , particle acceleration mechanism
is poorly understood . When the high -energy electrons
are produced in an active region , they gyrate around
active region magnetic field and propagate along the field .
Gyration motion of electrons emits microwaves . So , if
we can image microwave -emitting region we can identify
the location of electron acceleration . With this idea , weconstructed Nobeyama Radioheliograph(NoRH ) 10
years ago and are continuing observation . As the speedof the high -energy electrons are close to the light speed ,the radio telescope needs to have both high time andspace resolution . The spatial resolution of NoRH is 10
arcsec at 17 GHz and is 5 arcsec at 34 GHz . Temporal
resolution is 100 msec . As the NoRH can observe thefull disk , we do not miss any events if they occur during
the observing time . Even with these conditions , wecould not detect events to identify electron propagation .
In the flare on August 28, 1999 , we finally detected
microwave -emitting electrons propagating along a loop
［1 ］
. Although the flare itself was medium class , wecould observe a large and bright loop -shaped microwave
source (Figure 1). We studied the formation process of
the loop source by radio images every 100 msec (Figure2). First , a compact source (C ) appeared , then , a loop
source started to extend from one foot point near (C )toward the other . The projected length of the loop is
45,000 km and it took 0.5 second for the bright feature to
fill the complete loop . If we take into account the 3-D
structure of the loop and the fact that electrons are
gyrating around the magnetic field , the speed of electrons
should be very close to the light speed .
Based on this observation , we can say that either 1)high -energy electrons were produced in a small loop in
the source (C ) and were injected into the large loop , or 2)
high -energy electrons were produced by interaction
between the small loop and the large loop . This infor -, Takaaki(Pulkovo Observatory , Russia )mation is very important to study the particle acceleration
mechanism in solar flares .
Reference［1 ］Yokoyama , T., Nakajima , H ., Shibasaki , K ., Melnikov , V . F .,and Stepanov , A . V .: 2002 , ApJ , 576, L87 .

Figure 1: Full disk image (left , 17 GHz ) and partial frame
image (right , 34 GHz ) of the 1999 August 28 flare .

Figure 2: Radio brightness distribution every 100 msec at 17
GHz . An extending bright feature from one footpoint of the loop toward the other can be seen .

15

Investigation of Supernova Nucleosynthesis
Elemental Abundances of Metal -Deficient

from
Stars

AOKI , Wako , ANDO , Hiroyasu(Divisionof Optical and Infrared Astronomy , National

NORRIS , J. E .
(Australian

National

University )RYAN , S . G .
(Open University , UK )The most metal -poor stars in the Galactic halo are
believed to contain the material ejected from the first
generations of stars . To investigate the nucleosynthetic
yields of supernovae , the chemical compositions of anumber of extremely metal -poor stars have been studied
recently based on high resolution spectroscopy .
We have made systematic abundance studies for very
metal -poor stars with carbon excesses using the Subaru
TelescopeHigh Dispersion
Spectrograph(HDS ).
Among these stars , we discovered a carbon -rich star
which also shows remarkable excesses of magnesium(Mg ) and silicon (Si ) (CS29498 -043, Figure 1 (left ),［1 ］［2 ］). The iron abundance is very low (about 1 /5000 of
the solar one ). Only one object which has similar abun ), but the endance nature is known (CS22949 -037,［3 ］
hancements of magnesium and silicon are more signifi cant in CS29498 -043. The right panel of Figure 1 depicts
the pattern of the relative elemental abundances for these
two objects , with respect to other very metal -deficientstars . These two objects clearly show large excesses oflight elements from carbon to silicon .
The α‑elements including magnesium and silicon areejected from the nucleosynthesis by type II supernovae ,while the origins of carbon and nitrogen are rather com plicated . The existence of these α‑element -enhanced
stars indicates a variation of the yields by type II super novae .

Astronomical

Observatory )BEERS , T. C .
(Michigan

State University )Recent models of supernova nucleosynthesis suggestthat the ejection of iron in the explosion is strongly
dependent on the explosion energy of the supernovae .
For instance , supernova models assuming low explosion
energy predict low abundance ratios of iron -peak ele ments , which are produced in the deep interior of the core ,in the ejecta . Since magnesium and silicon which arepreserved in outer layer are ejected even by low energy
explosion , the resulting α/Fe ratio is high . The ʻ
α‑rich ʼ
star found by our observation is interpreted as an ʻiron deficient ʼstar in this context ［4 ］. Recently , a supernova
model which includes interior mixing before explosion
was proposed ［5 ］. This model is also trying to explain
the elemental abundances of the most iron -deficient star
HE0107 -5240 discovered last year ［6 ］. Further abun dance studies for extremely metal -deficient stars will givea strong constraint on these supernova models .
References［1 ］ Aoki , W ., Norris , J.E ., Ryan , S . G ., Beers , T. C ., Ando , H .:2002 , ApJ , 576, L141 .
［2 ］ Aoki , W ., Ryan , S . G ., Norris , J. E ., Beers , T. C ., Ando , H .:2002 , PASJ , 54, 933.
［3 ］ Norris , J. E ., Ryan , S . G ., Beers , T. C .: 2001 , ApJ , 561, 1034 .
［4 ］ Tsujimoto , T., Shigeyama , T.: 2003 , ApJ , 584, L87 .
［5 ］ Umeda , H ., Nomoto , K .: 2003 , Nature , 422, 871.
［6 ］ Christlieb , N . et al .: 2002 , Nature , 419, 904.

Figure 1: (left )［Mg /Fe ］as a function of［Fe /H ］
. An extremely Mg -rich star CS29498 -043 was discovered by our observation .
(right ) Relative abundances of elements in CS29498 -043 and CS22949 -037, with respect to the average values of other stars
with similar iron -abundances . These two stars show significant excesses of light elements from carbon to silicon .

16

Centroid
ARAKI , Hiroshi , TAZAWA

Experiment, Seiichi , ASARI , Kazuyoshi , TSUBOKAWA(Mizusawa

HANADA(Divisionof Artificial

Astrogeodynamics, Hideoof Earth Rotation , NAOJ )Stars, Tsuneya , TSURUTA, Seiitsu

Observatory , NAOJ )YANO , Taihei , GOUDA , Naoteru(Divisionof Astrometry and Celestial Mechanics , NAOJ )RISE GroupWe are now investigating a selenodetic mission ILOM
(In -situ Lunar Orientation Measurement ) in a post
SELENE
project in order to study lunar rotation
dynamics by direct observations of the lunar physicallibrations and the free librations from the lunar surfaces
with order of 1 mille -arc -second (1mas ) accuracy .
One of the key technologies of the ILOM project ishigh precision centroiding , which is common to infrared
space astrometry project of NAOJ (JASMINE ). So theILOM and JASMINE groups have started centroid exper iment with CCD camera . The aim of the experiment is
to obtain precise positions of simulated star images onfine controlled CCD . The image data are used forvalidation of centroid determination algorism that has
been developed in JASMINE group .
The apparatus of centroid experiments consists of
optical bench which carries pseudo star unit made of 25
optical fibers and their holder , objective achromatic lens
whose aperture is 5cm and F (focal ratio ) is 2-5, and CCD
camera (Figure 1). One side edges of the optical fiber
illuminated by white light introduced from the other side
are used as pseudo stars . Fine position adjustment of the
CCD camera using stepping motor is possible with lessthan 0.1 m accuracy in the direction perpendicular to theoptical axis . Image data at several positions of CCD
camera to pseudo star unit are obtained systematically by
the computer control system .

It is desirable that pseudo star images on the CCD
cover several pixels for the precise positioning . For thispurpose an iris diaphragm with aperture 1 or 2 mm is
inserted in front of the objective to obtain F value about
100 enough to see the diffraction image enlargement .
It is relatively easy to obtain center position (X ) ofpseudo star by photon weighting mean method . But if
the true center (X ) of pseudo star do not correspond toa pixel center , centroiding error about more than 1 /10
pixel may be introduced due to some discrepancy between
X and X . By using 1st order approximation for X -X
(X -X ＝k X ) and the least square method applied tothe data of distances between X (for star 1) and X (forstar 2) on several positions on CCD , k1 , k2 , X , and X
are obtained . It has been confirmed that the centroidingof pseudo star is possible with the accuracy of 1 /300 pixelby this method (Figure 2). This is the same fine recordthat FAME group had achieved . Centroid experiments
and analysis will continue for the ILOM goal of 1 /1000
pixel accuracy incorporating 3rd order approximation for
X -X and correction of image aberrations .

Figure 2: Results of relative position analysis between 2
pseudo stars . Upper right is a sample of imaged
pseudo stars .
Figure 1: Centroid experiment apparatus .

17

Prominence Eruptions and Coronal Mass Ejection :A Statistical Study Using Microwave Observations
GOPALSWAMY, N ., LU , W ., YASHIRO(Goddard Space Flight Center , NASA )We studied the height -time history and CME associa tion of all the Prominence Eruptions (PEs ) automaticallydetected by the Nobeyama Radioheliograph . Out of the
226 events identified between 1996 January and 2001
December , 186 had simultaneous CME data coverage
from the SOHO mission . From time plots we were able
to classify the PEs into two groups : radial events that had
motion predominantly in the radial direction and trans verse events that had motion roughly parallel to the limb .
Radial events attained larger heights and had greater
average speeds as compared to the transverse events . We
identify the radial and transverse events with the classicaleruptive and active PEs , respectively . The radial events
showed close relationship to the CMEs . We found that
72 % of all the PEs and 83 % of the radial events wereassociated with CMEs . Thus , we have confirmed theclose relationship between PEs and CMEs using a large
sample of microwave prominences . This result is consis tent with three previous studies ［1, 2, 3 ］that used smaller
sample sizes . However , our results contradict those of［4, 5 ］, who reported a poor association between promi nence eruptions and CMEs . Our result that 73% of thePEs are associated with CMEs is twice as large as the 36%
association found for BBSO H α eruptions ［5 ］
. Promi nence eruptions without CMEs are very slow and are
restricted to regions close to the solar surface . These
events are generally the transverse events .
We also studied the spatial and temporal relationshipbetween the PEs and the corresponding CME events .
We found that the onsets of PEs and CMEs were nearly
simultaneous , within 30 minutes . This result may haveimportant implications to the theories of CME initiation .
We also confirmed the spreading of the source locationsof CMEs and prominences to all latitudes toward thesolar maximum . However , the Central Position Angles(CPAs ) of CMEs and PEs generally did not coincide .
During solar minimum , the CPAs of CMEs tend tocluster around the equator , while those of the PEs wereconfined to the latitudes of the active region belt .
During solar maximum , there is no such relationship ,18, S . SHIMOJO, M ., SHIBASAKI, K.

(Nobeyama Radio Observatory , NAO )reflecting the varied influence of the solar dipolar field on
CMEs during solar minimum and maximum .
References［1 ］Munro et al .: 1979 , Sol . Phys ., 194, 371.
［2 ］Gilbert et al .: 2000 , ApJ . 537, 503.
［3 ］Hori and Culhane .: 2000 , A & A , 382, 666.
［4 ］Wang , H . and Goode , P .: 1998 , in ASP Conf . Ser . 130, Synoptic
Solar Physics , 497.
［5］Yang , G . and Wang , H .: 2002 , in Proc COSPAR
Magnetic Activity and Space Environment , 113.

Collq ., Ser 14,

Figure 1: (a) -(d) Eruption of the 2000 October 22 microwave
prominence from the east limb . (e) - (h) SOHO /LASCO images of the white -light CME at several
instances . (i)Height -time plots of the CME (upper
curve ) and the eruptive prominence (lower curve ).
The diamonds represent prominence height mea sured from the NoRH images . The squares denotethe height of the prominence core measured from the
LASCO images . The curves were obtained by fit ting second -order polynomials to the data points .
The times corresponding to the microwave andwhitelight images in (a) - (h) are indicated on theheight -time plots .

Two Types of Shock -waves and Selective
High -Energy Particles

Acceleration

of

OHKI , Ken -ichiro(Divisionof Theoretical

Interplanetary (hereafter IP ) shock -waves produced bysolar flares or by Coronal Mass Ejection (hereafter CME )are observed with radio -waves , particle counters onboard
satellites , and in situ observations by IP spacecrafts .
Thus , the most detailed study comes to be realized .
Particle observations at 1 AU immediately after solar
flares have revealed that impulsive particle events haveabout two orders of magnitudes higher electrons /protons(hereafter e/p) ratios than those of gradual flares . This
result has been interpreted as an increase of electrons due
to wave -resonant acceleration by MHD waves within theflares . However , if we combine gamma -ray data with thee/p observations , it turns out that the large impulsive
events accompanied by gamma -ray emissions probably
indicate higher e/p ratios due to proton depletion asshown in Figure 1. Moreover , since impulsive particle
events generally show a close correlation with meter -wave
Type II bursts (coronal shocks ), we propose that blast wave shocks emitted directly from flare explosions may
accelerate particles in this case . On the other hand , it isestablished that the particle acceleration in the case of
gradual particle events is due to the piston -driven shock
induced by CME . Therefore , the large difference in e/pratios of the two types of events may arise from thedifference between the two acceleration mechanisms ［1 ］.
Meanwhile , according to the in situ observations of
the IP -shocks , it is found that seed particles injected into
the shock acceleration have twice the velocity of the solar
wind . Since this velocity corresponds to more than ten
times the mean thermal velocity in the solar wind plas mas , it could not be a high energy tail of the Maxwell
distribution . In fact, according to observations , thevelocity distribution of this tenuous solar -wind plasma
does not show Maxwellian , but a Kappa -function distri bution that has a characteristic high -energy tail withpower -law distribution ［2 ］. After calculation , the esti mated altitude where the velocity distribution changes
from Maxwellian to Kappa -function seems to be several
to ten times the solar radius . On the other hand , since
blast -wave shocks are observed to decline within threetimes the solar radius , the distribution should not be
converted to a Kappa -function in this case . Consequent ly, the lack of seed particles for proton acceleration would
give a large e/p ratio .
As for the IP -shocks driven by CMEs , it is revealed inthis study that proton acceleration nearby the Sun exclu sively occurs near the “nose ”part of the CME and only
very small numbers of protons are observed at the “flank ”

Astrophysics , NAOJ )part of the shock excited by the CME , probably because
the CME no longer exists just behind the shock at theflank part . Electrons , on the other hand , are observed
everywhere from the CME driven shocks including theflank part with an equal intensity as compared by othertypes of flare emissions ［3 ］.
As shown above , if we combine in situ observations ofparticles and magnetic field etc. with solar observations ofradio , gamma -ray, and X -ray etc., the total physics of theshock acceleration would be revealed . Moreover , when
we can completely solve the problem of injection of seedparticles into the acceleration , some problems of chemicalcompositions in solar and galactic cosmic rays could beanswered . There are many common properties between
them . So , the study of particle acceleration combining
several research fields is hoped in the near future .
References［1 ］Ohki , K .: 2003 , ApJ ., 586, 617-623.
［2 ］Chotoo , K ., et al .: 2000 , JGR , 105, 23107 -23122 .
［3 ］Ohki , K .: 2003 , Solar Phys ., 213, 111-120.

Figure 1: Electron 5-11 keV and proton 25-45 keV are shown .
Open bars and thick bars indicate electron andproton flux respectively . Gamma -ray events areindicated by asterisk marks to the left of the date .
The flux units are particles m sr sec MeV .

19

Molecular

Outflow Search in the ρOphiuchus A and B2 Regions
KAMAZAKI, Takeshi(Nobeyama Radio Observatory , NAOJ )SAITO , Masao(Divisionof Radio Astronomy , NAOJ )HIRANO, Naomi(Academia Sinica Institute of Astronomy and Astrophysics )KAWABE(Division, Ryoheiof Radio Astronomy , NAOJ )We have searched for CO molecular outflows associat ed with the cloud A and B2 of the ρ Ophiuchus star
forming region . On the basis of single dish CO (J ＝3‑2) and interferometric
CO (J ＝1 ‑0) observations , wehave identified three molecular outflows in the ρOph A
cloud and one in the ρOph B2 cloud . Out of the four
outflows observed in these regions , one is the known
outflow driven by the Class 0 source , VLA1623 , and theother three are newly discovered ones . The inclinationand opacity corrected momentum flux Fof newly
detected outflows are roughly comparable to those ofClass I objects observed by［3 ］. All the newly discover ed outflows are likely to be driven by Class II sources ornear infrared sources , and none of them is associated withthe cold submillimetermillimetersources ［2 ］ without
infrared counter parts . These results indicate that protos tars associated with outflows whose mass and momentum
flux exceed our detection limit are not formed yet in thehigh density ridge of the ρOph A region and the north eastern condensation in the ρOph B2 region , suggestingthat they are considered to be pre -protostellar cores ［1 ］.

Figure 1: CO (J ＝3 ‑2) maps of the northern field of the ρ
Oph A region taken with the James Clerk Maxwell
Telescope . (a) Blueshifted emission (V ＝‑1.68〜＋1.31 km s ). (b) Redshifted
emission(V ＝＋5.10 〜＋6.73 km s ). Crosses are thepositions of the submillimeter continuum sources ,SM1 , SM1N and SM2 , identified by ［4 ］
. Starmarks are the positions of a NIR source , GY30 and
VLA1623 . Diamonds are small cores identified by［2 ］.

References［1 ］Kamazaki , T., Saito , M ., Hirano , N ., and Kawabe , R .: 2003 ,ApJ , 584, 357.
［2 ］Kamazaki , T., Saito , M ., Hirano , N ., and Kawabe , R .: 2001 ,ApJ , 548, 278.
［3 ］Bontemps , S ., Andre , P ., Terebey , S ., and Cabrit , S .: 1996 , A &Ap , 311, 858.
［4 ］Motte , F ., Andre , P ., & Neri , R .: 1998 , A & Ap , 336, 150.

20

Figure 2: CO (J ＝1 ‑0) maps of the southern fields of the ρ
Oph A region observed with the Nobeyama Milli meter Array . Large solid circle indicates 40 % levelof primary beam pattern of the NMA 10 m antennas
and large dashed circle indicates the field of view of
the NMA 10 m antennas (FWHM ＝65 ). (a) Blue shifted emission (V ＝‑0.20 〜＋2.24 km s ). (b)Redshifted emission (V ＝＋5.08 〜＋6.71 km s ).
Stars are VLA1623 and NIR sources (LFAM3 andS2 ).

Deep Imaging Observations of the Lupus 3 Cloud :Dark Cloud Revealed as Infrared Reflection Nebula
NAKAJIMA , Yasushi , NAGATA , Tetsuya , SATO , Shuji , NAGAYAMA, Takahiro
NAGASHIMA, Chie , KATO , Daisuke , KURITA , Mikio , KAWAI , Toshihide(Department of Astrophysics , Faculty of Sciences , Nagoya University )TAMURA(Division, Motohide

NAKAYAof Optical and Infrared Astronomy , NAOJ )SUGITANI, Hidehiko(Subaru Telescope , NAOJ ), Koji(Institute of Natural Sciences , Nagoya City University )Dark cloud consists of dust and gas . Dark cloud has
been identified as “dark spot ”in the sky , as optical lightfrom the background stars is effectively absorbed by dustin dark cloud . Dark cloud is one of the sites of starformation . It is important to study nature of dust andgas in dark cloud for understanding of star formation .
The Lupus 3 dark cloud is one of the nearest (〜150
pc ) dark cloud . We carried out deep imaging observa tions of the most extinct part of the Lupus 3 dark cloudin near infrared wavelengths J (λ＝1.25μm), H (1.65μm),
and Ks (2.15μm) bands . The observations were made on
2001 June with the near infrared camere SIRIUS on the
IRSF 1.4m telescope in South Africa . As a result , Lupus
3 showed itself as a near infrared nebula . A JHKs
color -composite image (Blue , green , and red are assigned
to J , H , and Ks , respectively .) is shown in Figure 1. We
obtained surface brightness distribution at each band (J ＝20.6, H ＝19.8, and Ks ＝19.4 mag arcsec
at the maxi mum ) and an extinction map of the background stars dueto the dark cloud (Av ＞47 mag at the maximum ). It is
the first time that such a heavily extinct dark cloud isreported to shine itself in the near infrared . It is also
remarkable that detailed structure of the dark cloudappeared as emission in the near infrared . The surface
brightness of the dark cloud is understood in terms of
scattering of starlight by dust . There are three local
maxima of the extinction with Av ＞30 mag , dark or
tanned parts in Figure 1, which we assume to be dense
cores . The surface brightness distribution depends on
the wavelengths and correlates with the extinction . In
the J band , dark cores are surrounded by a brighter halo ,while , in the Ks band , the dark cores of the J band arebright except for the central part of two of the cores . The
appearance in the H band is intermediate of the J and Ks
bands , having dark cores surrounded by local maxima of
the surface brightness and the surface brightness decreases

Figure 1: J, H , and Ks -band composite image . The FOV is〜9ʼ
×9ʼ(0.4 pc ×0.4 pc ). The epoch is 2000 .0.

again outside . The surface brightness and its relation ship with the extinction are understood quantitatively interms of scattering of starlight by dust . The maximum
surface brightness can be explained by scattering of star light by dust in the cloud if we adopt a model of grain -size
distribution by Weingartner and Draine ［1 ］. Greaternumber density is found for a larger size regime in the
Weingartner and Draine model than in the widely usedmodel of Mathis et al .［2 ］.
References［1 ］ Weingartner , J. C ., & Draine , B . T.: 2001 , ApJ , 548, 296.
［2 ］ Mathis , J. S ., Rumpl , W ., & Nordsiek , K . H .: 1997 , ApJ , 217,
425.

21

Optical Spectropolarimetryof SN 2002ap with Subaru Telescope

KAWABATA(Division, S . Koji

JEFFERY

of Optical and Infrared Astronomy , NAOJ ), D . J.

(University of Nevada )IYE , Masanori , KASHIKAWA, Nobunari , SAITO , Yoshihiko , MISAWAYAMADA , Toru , TANAKA , Ichi
(Division

OHYAMA, Toru ,of Optical and Infrared Astronomy , NAOJ ), Youichi , KOSUGI , George , SASAKI , Toshiyuki , SEKIGUCHIAOKI , Kentaro , TAKATA , Tadafumi, Kazuhiro ,(Subaru Telescope , NAOJ )EBIZUKA, Noboru(RIKEN )NOMOTO , Ken ʼ
ichi , MAZZALI , Paolo , DENG , Jinsong , MAEDA , Keiichi ,UMEDA , Hideyuki , OTA , Kazuaki(University of Tokyo )YOSHIDA, Michitoshi , INATA , Motoko , OKITA , Kiichi , SHIMIZU(Okayama Astrophysical

ASAI , Ryo

OZAWA , Tomohiko , YADOUMARU(SEC , Inc .)TAGUCHI, Hiroko(Waseda Jitsugyo High -scool ), Yasushi(Misato Observatory )NAKATA, Fumiaki(University of Durham )SN 2002ap was discovered in the nearby spiral galaxy
M74 on 2002 January 29. It has been clasified as a TypeIc supernova and suggested to be a hypernova ［1 ］. The
kinetic energy of a hypernovae is approximately ten times
as much as that of a typical supernova . Since someauthors suggested that the high energy is related with theasymmetry of the explosion , polarimetry of hypernovae
has been desired .
We performed optical spectropolarimetryof SN
2002ap with Subaru Telescope and Faint Object Camera
and Spectrograph (FOCAS ) in 2002 February (corre sponding to visual maximum phase ), March and June
［2 ］
. The data show the development of linear polariza tion (Figure 1). Distinct polarization profiles were seen
only in the O I λ7773 multiplet /Ca II IR triplet absorp tion trough at maximum light and in the O I λ7773
multiplet and Ca II IR triplet absorption troughs a month
later , with the latter showing a peak polarization . The
intrinsic polarization shows three clear position angles :80 for the February continuum , 120 for the Februaryline feature , and 150 for the March data . We conclude
that there are multiple asymmetric components in theejecta . We suggest that the supernova has a bulk asym metry with an axial ratio projected on the sky that isdifferent from 1 by an order of 10% . Furthermore , wesuggest very speculatively that a high -velocity ejecta com ponent moving faster than 〜0.115c (e.g., a jet) contrib utes to polarizationin the February epoch . High velocity jet-like clumps have been proposed in somehydrodynamic explosion models for SNe and GRBs , thisresult gives a hint on the physics of core -collapse super 22, Yasuhiro

Observatory , NAOJ )KODAMA, Tadayuki(Theory Division , NAOJ )novae .
References［1 ］ Mazzali , P . A . et al .: 2002 , Astrophys . J ., 572, L61 -65.
［2 ］ Kawabata , K . S . et al .: 2002 , Astrophys . J ., 580, L39 -42.

Figure 1: Flux and polarization spectra of SN 2002ap . From
top to bottom , we plot (a) total flux , (b) polariza tion level , and (c) position angle on each observa tion day as indicated . The interstellar polarization
component is shown by dashed lines in (b) and (c).

Compact

Nuclear

Starbursts
IMANISHI(Divisionin Seyfert 2 Galaxies, Masatoshi

of Optical and Infrared Astronomy , NAOJ )According to the unification paradigm of active galac tic nuclei (AGNs ), Seyfert 2 galaxies (which do not show
broad optical emission lines ) are believed to contain
AGNs obscured behind dusty tori . Since the dusty tori
are rich in molecular gas , they are plausible sites for
starbursts to occur . Although the presence of such
nuclear starbursts has been suggested in Seyfert 2 galaxies ,the true nature of these starbursts is still unclear . To
understand the properties of the compact (＜300 pc insize ) nuclear starbursts , by disentangling from extended
star -formation activity in the host galaxies , slit spectros copy is most effective .
In particular , 3-4 μm slit spectroscopy can provide an
excellent tool not only for detecting the compact nuclear
starbursts , but also for making quantitative estimates of
their luminosities . First , the 3.3 μm polycyclic aromatichydrocarbon (PAH ) emission feature is detected only in
starbursts and not in AGNs , making its luminosity a goodmeasure of starburst activity . Second , the 3.3 μm PAH
emission from starbursts is intrinsically so strong that thesignatures of even weak compact nuclear starbursts aredetectable in normal (S /N 〜20) spectra . Third , theeffects of dust extinction are much lower than at shorter
wavelengths . We have performed 3-4 μm slit spectros copy of 12 Seyfert 2 galaxies (Figure 1) and found thefollowing main conclusions ［1 ］.
1. For three selected Seyfert 2 galaxies , our estimates ofthe magnitudes of compact nuclear starbursts , basedon the observed 3.3 μm PAH emission luminosities ,agreed quantitatively very well with the previous
estimates derived from the UV after dust extinction
corrections had been applied . This agreementmeans that the observed 3.3 μm PAH emission lumi nosities are a good measure of the luminosities ofcompact nuclear starbursts in Seyfert 2 galaxies .
2. Except in one object , the equivalent widths of the 3.3
μm PAH emission feature were much smaller thanthose observed in starburst -dominated galaxies , sug gesting that the 3-4 μm fluxes observed from the
majority of Seyfert 2 nuclei are dominated by AGNs
and not by starbursts .
3. The 3.3 μm PAH to infrared dust emission luminos ity ratios were so small that the compact nuclear
starbursts contribute only insignificantly to the infra red luminosities of Seyfert 2 galaxies .
4. The 3.3 μm PAH emission luminosities are statisti cally correlated with the IRAS 12 μm luminosities(Figure 2). If the IRAS 12 μm luminosities are agood measure of AGN power , then the magnitudes ofcompact nuclear starbursts and AGNs are correlated .
Reference［1 ］Imanishi , M .: 2002 , ApJ , 569, 44.

Figure 1: Examples of 3-4 μm spectra of Seyfert 2 nuclei . The
abscissa is observed wavelength in μm, and theordinate is F in 10
W m μm . The upper
two sources show clear 3.3 μm PAH emission features , while the spectra of the the lower two sources
are nearly featureless , with no detectable 3.3 μm
PAH emission .

Figure 2: Comparison of the 12 μm luminosities measured
with IRAS (abscissa ) and the 3.3 μm PAH emission
luminosities measured in our slit spectra (ordinate ).
Both luminosities are statistically correlated .

23

Size Distribution of Sub -km Main Belt Asteroids
Derived from Subaru Telescope Observations
YOSHIDA, Fumi , NAKAMURA, Tsuko , WATANABE, Junichi , KINOSHITA, Daisuke(NAOJ )YAMAMOTO(National, Naotaka

Institute of Advanced Industrial

The Suprime -Cam with Subaru telescope enabled us
to make a survey observation of large number of small
asteroids which have never been observed so far becauseof their faintness . We discovered 861 Main -Belt Aster oids (MBAs , about 80% of them were less than 1km indiameter ) in only 2-nights observations . We investigatedtheir size distribution statistically and found that the size
distribution expected from theory and collision experi ments is invalid in the small size range less than 1km［1 ］［2 ］.
Seven fields near opposition and near ecliptic wereobserved on February 21 and 24, 2001 . The total survey
area was about 3 square degrees . The limiting magni tude for MBAs was 24.4 (R ) mag . This means that we
could detect asteroids larger than 500m in diameter at theout -edge of the main -belt (3.5AU ). The composite image
produced from several images of the same observational
field like figure 1 are found to be useful to detect aster oids . In the composite images , though the S /N of eachobject slightly reduces , we can avoid overlooking theasteroids that were near the edge of the CCD chips orasteroids overlapped with stars and galaxies . Moreover ,we can remove faint asteroids which become invisible
from time to time because of the light variations , which
are a nuisance in our statistics .
We picked up 861 MBAs from the 1111 detectedmoving objects . After determining statistically the semi major axis and inclination of each object , we assumed analbedo to calculate the size of the asteroid ［3 ］. We
found that the slope of the Cumulative Size Distribution(CSD ) for the asteroids between 0.5km and 1km indiameter is 〜1.0. This value is much shallow than theslope 〜1.75 of the CSD of the asteroids more than several
km in diameter , which was obtained in the past observa tions (such as the Palomer -Leiden Survey ). This meansthat the number of small MBAs is much more depleted
than the expectation so far. Moreover , we divided themainbelt into three parts , and then estimated the CSD ineach part . We found that the slope of the CSD was mostshallow in the outer main -belt (see figure 2)［1 ］. We
consider that the difference in the size distributions
reflects the different impact behavior of the S -type andC -type asteroids in the main -belt .
References［1 ］Yoshida , F . et al .: 2003 , PASJ , in press .
［2 ］Yoshida , F . et al .: 2001 , PASJ , 53, L13 ‑L16 .
［3 ］Nakamura , T. & Yoshida , F .: 2002 , PASJ , 54. 1079 ‑1089 .

24

FUSE , Tetsuharu

Science and Technology )(Subaru Telescope )Figure 1: A composite image consists of the eleven exposures
for two hours . The FOV is 6.5 ×13 . The stars
and galaxies are shown by black images , the black
and white stick -shaped image shows an asteroid .
We can see easily the motions of each asteroid on thecomposite image .

Figure 2: The size distributions of the inner (2.0 ‑2.6AU ), themiddle (2.6 ‑3.0AU ), and the outer -main -belt (3.0
‑3.5AU ) are shown by blue , black , and red , respec tively . The curves with error bars show each CSD .
The detection limits in each region are shown by thevertical lines .

Plug -In Cryogenic

System for Cartridge -Type SIS Receivers

YOKOGAWA, SozoSEKIMOTO(Graduate University for Advanced Studies /NAOJ )SUGIMOTO(Division, Yutaroof Radio Astronomy , NAOJ ), Masahiro , OKUDA , Takeshi(Institute of Astronomy , University of Tokyo )SEKIGUCHI, Tomohiko , KAMBA , Toshiaki , TATEMATSU(Division

NISHINO, Ken ʼichi

of Radio Astronomy , NAOJ ), Tetsuo

OGAWA , Hideo , KIMURA(Advanced Technology Center , NAOJ )NARASAKINODA , Kazufusa(Oshima Prototype Engineering

Co ., ltd .)Kimihiro(Osaka Prefecture University )(Sumitomo, Katsuhiro

Heavy Industries , ltd .)We developed a cryogenic system , which houses 3
cartridge -type superconductor -insulator -superconductor
receivers for millimeter and submillimeter wavelengths .
Since it was designed as a prototype receiver of the
Atacama
Large
Millimeter / submillimeter
Array(ALMA ), high stability , accurate alignment , and easy
handling were required . To meet these requirements , thecryogenic system included the following technologies : 1) athermal link without screws for receiver cartridges ; 2) a
central support structure to reduce vacuum and gravita tional deformation ; 3) bellows structures to reducemechanical vibration of the cryocooler ; and 4) a 3-stage
Gifford McMahon (GM ) cryocooler with an He pot(temperature stabilizer ) to reduce the thermal ripple .

Figure 2: (a) Cross -sectional view of the φ170mm cartridge .
(b) Photograph of the cartridge with the Band 8(385-500 GHz ) SIS receiver . The LNA can be seenon the 12K stage of the cartridge .

Figure 1: (a) Cross -sectional view of the cryostat . The cryos tat is composed of 3 stages named plates ”, 4K , 12K ,and 100K from up to down . The cryostat has 3bays for 3 cartridge -type SIS receivers . The central
support structure is at the center of the vessel .
Bellows structures to reduce mechanical vibrationsof the cryocooler are located between the coldhead
and the plates . (b) Photograph of the cryostat
without radiation shields . The cooled optics of the
500 GHz receiver can be seen on the front cartridge ,and the feed horn of the 100 GHz receiver can beseen on the left side cartridge . The 800 GHz
receiver optics can be seen behind the central sup port structure .

The cryostat and receiver cartridges are composed ofthree stages . The temperatures on the 4K , 12K , and100K stages of the cartridge are 3.5K , 13.4K , and 78.3K ,respectively . The thermal conductances of the thermal
links showed high performances of 1.7 W K
at the 4K
stage , 5.6 W K
at the 12K stage , and 3.3 W K
at the100K stage . The mechanical vibration on the 4K stageof the cartridge was reduced to one -tenth , as small as
2 μm peak -to -peak , compared to that on the 4K coldheadof the cryocooler , 20 μm peak -to -peak . The tempera ture ripple on the cartridge was reduced to as small as 2mK peak -to -peak , which corresponds to oneseventh of theripple on the 4K coldhead with an He pot . See［1 ］,［2 ］
for more details .
References［1 ］Yokogawa , S . et al .: 2003 , PASJ , 55, 519［2 ］Sugimoto , M ., et al .: 2003 , accepted by the Cryogenics .

25

Seismic

Noise Reduction of a Gravitationalat the Kamioka MineTATSUMI(Division, Daisuke , FUJIMOTO

Wave Detector

Masa -Katsu ,of Astrometry and Celestial Mechanics , NAOJ )KURODA , Kazuaki , OHASHI , Masatake , MIYOKI , Shinji ,UCHIYAMA, Takashi , YAMAMOTO , Kazuhiro(Institute for Cosmic Ray Research , University of Tokyo )TERADA

smaller than that required by TAMA300 design sensitiv ity. ATAM300
detector is located at Mitaka campus ,and has a 300m baseline length . This provides a strong
appeal to advantage of the Kamioka site . Around afrequency of 100 Hz , the noise level is 2 10 m / Hzwith some unknown sources . Nevertheless the noiselevel is still smaller than current noise level of the
TAMA300 .
Boyond the low frequency noise inprovement , we also
succeeded in obtaining better sensitivity than TAMA300
despite of short baseline length . For the coalescence ofcompact star binaries , the detector can monitor over 3 kpc
away in a wide mass range from one to seventy solar
masses .

noise (m / Hz )A laser interferometric gravitational wave (GW ) detec tor with a base -line length of 20m was moved to the
Kamioka mine from Mitaka campus in 1999 . The
Kamioka site is located in latitude 36.25 degree north andin longitude 137.18 degrees east . The laboratory is in a
mountain , 1000m below the surface .
We decided to move the GW detector to take advan tage of the quiet seismic environment provided by the site .
Around a frequency of 1 Hz , the seismic motion is smaller
than that at Mitaka by two orders of magnitude . This
noise reduction is equivalent to applying a seismic
isolator with a resonant frequency of less than 100 mHz .
By taking advantage of this , we can reduce the seismic
noise as shown in Figure 1. At frequencies of less than
30 Hz , the noise level was consistent with the designed
goal . At 30 Hz it was 9 10 m / Hz . Moreover it is26, Souichi

Institute of Advanced Industrial

Science and Technology )

10
10
10
10
10

Displecement(National

10
10
10
10
10

Kamioka
Kamioka
TAMA
TAMA

‑11
‑12
‑13

20m 2003 . 02. 14
20m Design
2003 . 02. 20
Design

‑14
‑15
‑16
‑17
‑18
‑19
‑20

1

10

10

f

2

10

3

(Hz )

Figure 1: The detector displacement noise spectrum ; measured［black ］, design ［blue ］, the current TAMA300 ［red ］
and the TAMA300 design ［green ］.

This improvement is an important step for allowing
increased sensitivity thorough further reduction of thethermal noise as planned with a 100m scale cryogenic
detector , CLIO , and a fullscale detector , LCGT .

Construction

and Enlargement of Dilatonic
Impulsive Radiation

KOYAMA(Division, Hiroko

HAYWARDof Astrometry and Celestial Mechanics , NAOJ )The dynamical behavior of traversable wormholes andblack holes under impulsive radiation is studied in an exactly
soluble dilaton gravity model . Simple solutions are presented
where a traversable wormhole is constructed from a black hole ,or the throat of a wormhole is stably enlarged or reduced ［1 ］.
Wormholes are tunnels through space -time , linking other wise separated regions of a single universe , or bridges joining
two different universes . Since traversable wormholes wereintroduced by Morris and Thorne ［2 ］as theoretically allow able space -times in Einstein gravity , wormholes have been
pursued as an attractive research topic involving the possibilityof rapid interstellar travel and even time machines .
The properties of static Morris -Thorne wormholes havebeen studied by many authors and it is known even in non static situations that a negative -energy source is necessary for
traversable wormholes to exist .
Not long ago , a unified framework for black holes andtraversable wormholes was proposed ［3 ］
, indicating that they
are dynamically interconvertible when the trapping horizons
locally characterizing them bifurcate or merge . In seeking
analytic solutions
in full Einstein gravity , we have found non -static solutions to
be difficult to obtain , except in the idealization of impulsive
radiation , where the radiation is concentrated so as to deliver

Figure 1: Penrose diagram of a wormhole -construction model .
A wormhole is constructed from a black hole byirradiating with impulsive negative -energy radia tion , represented by dashed lines . The bold lines
represent the trapping horizons , light shading indi cates past trapped regions and darker shading indi cates future trapped regions . The impulses shift theblack -hole trapping horizons suddenly , making
them coincide , then constant non -impulsive radia tion supports the resulting wormhole .

Wormholesby, Sean A ., KIM , Sung -Won

(Ewha Womans University )finite energy and momentum in an instant .
In this paper , we construct some of the simplest models ofdynamic wormhole processes by employing impulsive radia tion in a generalized dilaton gravity model , specifically :wormhole construction from a black hole , wormhole opera tion by energy balance and wormhole reduction or enlarge ment . The last point addresses a common belief that , while
wormholes are possible or even expected at the Planck scale ,large -scale wormholes are unlikely or even impossible . The
recipe to enlarge the wormhole is to cause the wormhole
mouths to bifurcate , opening up an expanding region of past
trapped surfaces , then merge again , by adding additional
negative energy followed by compensating positive energy .
The general proof involves the first and second laws of
wormhole dynamics and is a future important work in theunified framework for black -hole and wormhole dynamics .
References［1 ］Koyama , H . et al .: 2003 , Phys . Rev ., D67 , 084008 .
［2 ］Morris , M . S . and Thorne , K . S .: 1988 , Am .J . Phys ., 56, 395.
［3 ］Hayward ,S . A .: 1999 , J . Mod . Phys . D8 , 373.

Figure 2: Penrose diagram of a wormhole -enlargement model .
Wormhole enlargement process by symmetric burstsof impulsive radiation , with negative energy fol lowed by positive energy , timed as described in the
text. The non -impulsive radiation is switched off
between the impulses . Then the middle shaded
region is vacuum and expanding .

27

Near Infrared ［Fe II ］Spectroscopyof Young Stellar

Outflows

PYO , Tae -Soo , HAYASHI , Masahiko , KOBAYASHI , Naoto , TERADA , Hiroshi ,GOTO , Miwa , YAMASHITA, Takuya , TAKAMI , Hideki , TAKATO , Naruhisa ,GAESSLER , Wolfgang , HAYANO , Yutaka , KAMATA , Yukiko ,IYE , Masanori , USUDA , Tomonori(NAOJ )TOKUNAGA, A . T.

(University of Hawaii )Young stellar outflows are closely related to theaccretion process of star formation and play importantroles in removing angular momentum from star -disk
systems . To address the issues of accretion and outflow
launching mechanisms , one must obtain not only highspatial resolution images of outflows but also theirkinematical information at the regions close to the driving
sources .
We observed the outflows from L1551 IRS 5［1 ］and
DG Tau ［2 ］
, both located in the Taurus molecular cloudat a distance of 140 pc , in the ［Fe II ］ λ 1.644 μm
emission line using the Infrared Camera and Spectro graph mounted on the Subaru Telescope . These observa tions have shown that the near -infrared ［Fe II ］ line
provides an excellent means to study accretion and out flow launching mechanisms , because the line has small
extinction compared to the optical forbidden lines , allow ing us to probe deeper into the envelopes of embedded
objects , and traces directly driven outflows of partiallyionized gas .
In the position -velocity diagrams of the［Fe II ］emis sion from L1551 IRS 5 and DG Tau , as shown in Figure
1 (b) and 2, respectively , we see similar characteristics
between the outflows from the two objects , although theirlinear scales are different from each other . First , theentire emission ranges of the blueshifted outflows do notcontain stellar rest velocities , suggesting that all the emis sion is of entirely outflow origin . Second , there are two
distinct velocity components seen in the blueshifted out flows : the high velocity component (HVC ) is 200 ‑300 km
s blueshifted with respect to the stellar velocity , while
the low velocity component (LVC ) is 〜100 km s
blueshifted . Third , the HVC and LVC are different innature . The HVC shows a narrow line width and ismore extended and located farther away from the driving
source than the LVC , while the LVC shows a broad line
width and is located closer to the origin . We concluded
that the HVC is a well -collimated jet launched from theregion close to the star and the LVC is a disk wind witha wide opening angle . The two distinct emission compo nents well separated from each other in space and velocity
have confirmed the presence of two types of directly
driven outflows : jets and winds .
Although such tendency has often been observed forclassical T Tauri stars (CTTSs : Class II ), our observa tions have revealed their presence and characteristics with
unprecedented
clarity . More importantly , we havedetected for the first time the tendency that the HVC and
LVC velocities for young stars like L1551 IRS 5 and DG
28

ITOH , Yoichi(Kobe University )Tau are significantly larger than those , respectively , ofmore evolved classical T Tauri stars (HVC 〜50 ‑200 km
s ; LVC 〜5 ‑20 km s ). We also detected forthe first time the kinematical evidence of wind collimationfrom the LVC of L1551 IRS 5; the line width of the LVC
decreases with distance from its origin as it collimates .
For DG Tau , we detected a redshifted counter jet on thenortheast side , with its emission within 0.7 arcseconds
from the star being occulted by the circumstellar disk .

Figure 1: (a) Continuum -subtracted ［Fe II ］λ1.644 μm image
for the L1551 IRS 5 outflows . The parallel dashedlines indicate the slit aperture with a 0.6 arcsecond
width . (b) Continuum -subtracted position -velocity
diagram along the northern jet of L1551 IRS 5.

Figure 2: Continuum -subtracted position -velocity diagram of［Fe II ］λ 1.644 μm emission of the DG Tau out flows .
References［1 ］Pyo T.-S . et al .: 2002 , ApJ , 570, 724.
［2 ］Pyo T.-S . et al .: 2003 , ApJ , 590, 340.

Observationsof Ammonia in Starburst

Galaxies

NGC 253 and M 82

TAKANO , Shuro , NAKAI , Naomasa

KAWAGUCHI, Kentarou(Divisionof Radioastronomy , NAOJ )The results of ammonia observations in NGC 253 andM 82 with the 45 m radiotelescope at Nobeyama Radio
Observatory are reported ［1 ］.
We are studying molecular abundances in nearby
galaxies , and investigating the reasons for the difference inthe abundances in such galaxies . This time the ammonia(J , K )＝(1, 1)−(4, 4) transitions (23.7 ‑24.1 GHz ) weresearched for in these famous starburst galaxies . As aresult the (1, 1)−(3, 3) emission lines were clearly detect ed in NGC 253, but no lines were found in M 82. The
beam size of this observation was 71.
It is remarkable that the shapes of the three emission
lines were different from one another in NGC 253 (Figure1). NGC 253 is a nearly edge -on galaxy , and the line
width can be explained by Doppler effect due to thegalaxy rotation . The difference in line shapes , therefore ,reflects the difference in distributions of the emission
lines . In particular , the (2, 2) emission is narrow ataround 300 km /s.
This velocity corresponds to a position at about 10
southwest from the center ［2 ］.
The rotational temperature here was about 50 K . On
the other hand , the average rotational temperature within
the beam was about 29 K .
Since ortho -and para -ammonia are established at theformation and subsequent transformation is thought to beneglected , the ratio should have information at the time ofammonia formation . In our observed transitions , (3, 3)
belongs to ortho , and others para . Based on the analysis ,the ortho /para abundance ratio was about 1 at the veloc ity with the strong (2, 2) emission . This value can beachieved under the condition of ortho and para distribu tion at more than 40 K . On the other hand , the ratio wasmore than 6 at the velocity with very weak (2, 2) emission(100 ‑250km /s). This value is large and quite remark able . It can be achieved under the condition of ortho
and para distribution at less than 8 K . Some low temper ature processes (e.g., cold dust ) are suggested for ammo nia formation in this velocity component .
The relative abundances of ammonia with respect to
H are obtained to be 2.7 ×10 and 1.4 ×10 in NGC
253 and M 82, respectively . Although both galaxies are
starburst with lot of gas , the ammonia abundances are(Okayama University )different by more than one order . This result further
supports the difference in molecular abundances so far
reported . We investigated molecular abundances includ ing other nearby galaxies , and as a result we found thatabundances of molecules related to formation on dust
were clearly low in M 82. We concluded , therefore , thatthe molecular abundance in M 82 is peculiar regarding
the formation mechanism . A possible reason for this isthat the amount of dust in the central region of M 82 isrelatively small , or that the effective temperature related tomolecular formation is relatively low .

Figure 1: Spectra of ammonia (1, 1), (2, 2), (3, 3), and (4, 4)transitions from bottom to top . The LSR velocity
shown is for each transition . The dashed line indi cates the systemic velocity .
References［1 ］Takano , S ., Nakai , N ., and Kawaguchi , K .: 2002 , PASJ , 54,
195.
［2 ］Canzian , B ., Mundy , L . G ., and Scoville , N . Z .: 1988 , ApJ , 333,
157.

29

Kinematic

Analysisof Spiral Structuresin the Local DiskYANO , Taihei , CHIBA , Masashi , GOUDA , Naoteru(Divisionof Astrometry and Celestial Mechanics , NAOJ )Figure 1: Schematic diagram showing the definition of phases ,and , in the Galactic Plane . Each vector corre sponds to a velocity vector of each star in epicyclic
motion .

We have presented a method , based on the analysis of
local kinematics of disk stars , to clarify whether the
motions of the stars in the solar neighborhood follow
those expected in the density wave theory . The method
utilizes the expected linear relation between the “
position− ＋phases ”of the stars ( ＝ ( / )/) andthose of their epicyclic motions, as shown in Figure 1,
whereis the distance between the star and the Galactic
Center (GC ),is the distance between the Sun and GC ,is the pitch angle of the spiral arm ,is the angle
betweenand, andis the angular velocity of the
spiral pattern in the azimuthal direction . The applica tion of the method to the 78 Galactic Cepheids within 4
kpc from the Sun , for which accurate proper motions areavailable from Hipparcos , has revealed that an expected＋ (mod 2 ), islinear relation between and ,not apparent . Based on the quantitative analysis using
the least square method , we conclude that the currently
available data including large observational errors areinaccurate for use in assessing the presence of density wave motions in the solar neighborhood .
We here investigate to what extent the error in thephaseshould be reduced so as to extract the possible
wave motions of the stars . The error for a star , ,consists of the error associated with the velocity disper sion of the Cepheids ,, the error associated with theirapparent magnitude ,, and the error in Hipparcos
30

proper motions ,. We focus on the latter effectassociated with the uncertainty in the measurement ofproper motions . Three representative models following
density waves with 4 ‑arm ( ＝4), where different valuesofare assigned , are examined and the results areshown in Figure 2. In the first model ,is the sameas that for the current Cepheid data using Hipparcos
proper motions , referred to as. In the second and＝0.5
third models , we adopt the smaller errors ,and 0.1, respectively . As is evident in
Figure 2, the third model shows a noticeable minimum of
the sum of errors , , at ＝4, whereas in the first andsecond models there exists no minimum . Thus , theseexperiments suggest that if the error in proper motion
measurement is less than a tenth of that for Hipparcos
proper motion , then it is possible to obtain a minimum inand so to extract wave motions of stars .
Reference［1 ］Yano , T., Chiba , M ., & Gouda , N .: 2002 , A & A , 389, 143.

Figure 2: The relation
vs. for the three 4-arm models withdifferent errors related to proper motions ,. Thesolid , dashed , and thin dashed lines denote the 4-arm＝＝0.5
models with
,
, and
＝0.1
, respectively .

On Stationarity

of Spiral Structure

in Disk Galaxies

YANO , Taihei , KAN -YA , Yukitoshi , GOUDA , Naoteru(NAOJ )
We investigate whether spiral arm in disk galaxies ispossible to be stationary , assuming that spiral structure issome pattern formed by density wave . We numericallycalculate stellar orbits in assumed galactic potentials withspiral patterns and analyze the orbital behavior in thepotentials to study the criteria for disk parameters , inwhich stationary spiral structure is possible .
We find the following results ; spiral potential drives
the dynamical evolution which results in spiral structure ,bar structure or disappearance of the structure , dependingon the form of an assumed spiral pattern . If stationary
spiral structure appears , the only possible pitch angle ofarms is around 10 . Therefore observed spiral arms inlate -type spiral galaxies with large pitch angles cannot be
stationary structure if the arms are induced by density
wave .
Here , we present the form of the potential and parame ters in calculations .
As an axisymmetric part of the potential we assume apower -law potential . The rotation velocity
in thepotential is described as follows ;
,
(1)
where
is the radius from the galactic center , andis aconstant . In our calculation , we adopt ＝0.25. As anon -axisymmetric part , we give the form of two -armed
spiral potential rotating stationarily ,
＝−

(2

−2 ),

(2)

,
(3)
where ( , ) is the polar coordinates in the frame corotat ing with a spiral pattern ,is some scaling radius which
will be taken as the initial radius of a test star , is thepitch angle of the spiral arm , andis the parameter
which describes local radial slope of the spiral potential .
For convenience we introduce a new parameter,
which we call the “windedness ”,instead of the pitch angle, which is defined as⎧⎜− 2 − ( ＜0 : trailing arm )
⎨
.
(4)
⎜ −
( ＞0 : leading arm )⎩2
Negative and positive values of represent trailing arms

Figure 1: Schematic diagram of the final structure for a given
pair of ( , ).

and leading arms , respectively .
We have investigated the stationarity of spiral arms in
disk galaxies by analyzing the orbital behavior in spiralpotential patterns . We have adopted a power -lawaxisymmetric potential with a two -armed weak spiralpotential pattern . In the analysis , we have compared the
direction of the major axis of a calculated orbit with thatof the expected orbit . We have examined how the pat tern in galaxies evolve for various values of .
Our main conclusion to be emphasized is that the
spiral structure with the pitch angle
10 is the only
possible stationary spiral structure . The stationary spiral−2 withstructure is possible only if −2
0.5 orsufficiently large absolute value of the windedness if thearms are the manifestation of the density wave . Other
spiral pattern cannot be maintained , and develops to a baror blow out such that no structure remains . Those
results are summarized in Figure 1. Therefore spiralstructure in observed late -type spiral galaxies with large
pitch angle cannot be due to the stationary density wave ,but some transient pattern .
References［1 ］Contopoulos , G . & Grosbol , P .: 1986 , A & A , 155, 11.
［2 ］Yano , T., Kan -ya, Y ., & Gouda , N .: 2003 , PASJ , 55, 409.

31

Revised Fluorescence Efficiencies of Cometary
Ammonia Abundance in Comets
KAWAKITA(Gunma Astronomical, Hideyo
Observatory )Ammonia molecule is the first triatomic molecule
discovered in the interstellar space . It is detected inmany molecular clouds , and it seems to be a popularmolecule in the interstellar space . In the case of comets ,ammonia is important as a main reservoir of nitrogen
atom . However , there was no report on secure detectionof cometary ammonia until the first detection in comet
Hyakutake in 1996 . Ammonia molecules sublimatedfrom the cometary nucleus would dissociate into NH andH atom by solar UV radiation ［3 ］. The lifetime of thephoto -dissociation is about several thousand seconds at
1AU from the Sun . Expanding velocity of the gas is
about 1 km s and therefore the region where ammonia
molecules exist is estimated to be about several thousand
km in radius . When we observe inversion transitions ofammonia by radio telescope at the frequency of
23
GHz , the antenna beam size would be larger than theammonia region of a comet . Thus , the dilution effectwould prevent the detection of ammonia in comets . On
the other hand , the amount of ammonia molecules has
been estimated from NH abundance . The fluorescence
efficiencies (g-factor ) of NH are key parameters to deter mine the amount of NH in the coma .
The g-factors of NH were calculated by Tegler &Wyckoff (1989 ) considering electronic and vibrationalenergy levels of NH and transitions between them by thesolar fluorescence , at the first time . They estimated theammonia abundance in comet Halley and compared itwith in situ measurement of ammonia in the comet by
Giotto space craft . However , estimated abundance fromNH was slightly smaller than the in situ measurement .
Furthermore , the dependence of NH flux on heliocentric
distances observed in comet Hale -Bopp could not be
explained by their calculation ［4 ］.
We considered that the rotational structure of energy
levels which are not fully considered in［2 ］was the reasonof these discrepancy . The g-factors of NH are calcu lated by our fluorescence model ［1 ］
. Based on our
results , the ammonia abundance in comet Halley obtained
from the NH observation is consistent with that obtainedby the in situ measurement . The dependence of NH
emission flux on heliocentric distances can be also explained by our calculation . The mean abundance ofammonia relative to water in comets is estimated to beabout 0.5 % based on previous NH observations incomets ［5 ］and our g-factors .

32

WATANABE, Jun -ichi(Public Relations

Center , NAOJ )NH :References［1 ］Kawakita , H ., Watanabe , J. : 2002 , ApJ , 572, 177L .
［2 ］Tegler , S ., Wyckoff , S .: 1989 , ApJ , 343, 445.
［3 ］Kawakita , H ., Watanabe , J.: 1998 , ApJ , 495, 946.
［4 ］Rauer , H ., et al .: 1997 , Science , 275, 1909 .
［5 ］Fink , U ., Hicks , M . D .: 1996 , ApJ , 459, 729.

Figure 1: The comparison between a low dispersion cometary
spectrum and a modeled NH spectrum . The emis sion bands of C and forbidden emission lines ofatomic oxygen as well as NH emission bands wereshown in observed spectrum .

Figure 2: Ammonia abundance relative to water in comets .
Mean abundance of ammonia relative to water isabout 0.5 % . It is found that comet 21P /Giacobini Zinner is a ammonia depleted comet .

Heliocentric

Dependence of the Sodium Emission
Comet 153P /Ikeya -Zhang
WATANABE, Jun -ichi(Public Relations

Center , NAOJ )FURUSHO(Astronomical

KAWAKITA, Hideyo(Gunma Astron . Obs .), Reiko

FUJII , Mitsugu

Data Analysis Center , NAOJ )(Fujii -Bisei Astron . Obs .)Sodium is one of the interesting atoms in comets , but
the release mechanism of the sodium have not beenclarified until now , as same as those in Moon andMercury even that intensive researches on their sodium
atmosphere have been performed so far. Although themain mechanism of sustaining the sodium atmosphere in
the Moon appears to be photosputtering desorption , there
is little or no consensus about the dominating mechanism ,due to many kind of difficulties such as interference of thebright bodies , time variation , and finite structure of theatmosphere with definite spatial distribution . Fortunate ly, cometary sodium can be studied simply because we canregards the sodium produced by small grains , at under
different conditions of the solar flux because of the time
variation of the heliocentric distance of the comets due tothe orbital motion . We tried to utilize the cometary
orbital motion as a variable condition in the naturalexperiment for inspecting the variation of the sodium
production .
A long -term monitor of the sodium on the comet will
be a key to solve the unknown mechanism of the sodium
release from cometary dust particles . A low -dispersion
spectroscopic monitor of comet 153P /Ikeya -Zhang was
carried out from 2002 February through May . The
sodium emission was derived mainly during March , when
the heliocentric distance of the comet was between 0.511
and 0.764 AU . The number of the produced sodium
atoms relative to the total cross section of dust grains
follows a power law of r
, where r is the heliocentric
distance . This fact strongly suggests that the sodium isreleased by a thermal desorption mechanism , not by thephotosputtering mechanism from cometary grains . The
derived potential barrier for the release of the sodium is0.49 ±0.10 eV , which is about half of that in the case of
the Moon .

ofFigure 1: The heliocentric dependence of the sodium emission
relative to the continuum emission of Comet 153P /Ikeya -Zhang . The red crosses are the values in the
pre -perihelion , and the green circles in the postperi helion . The fitted line indicates a power law ofr, where r is the heliocentric distance .

References［1 ］Watanabe , J., Kawakita , H ., Furusho , R ., Fujii , M .: 2003 ,Astrophys . J ., 585, L159 ‑L162 .

33

Dense Molecular

Gas in Lenticular

Galaxies

KUNO , Nario , NAKAI , Naomasa , SORAI , Kazuo , NISHIYAMA(Division, Kohtaof Radio Astronomy , NAOJ )Baltasar Vila -Vilaro(Submillimeter

Telescope Observatory )We made simultaneous HCN and CO observations of
three lenticular galaxies (NGC 404, NGC 3593 , and NGC
4293 ) using the Nobeyama 45-m telescope . We detected
CO emission from all galaxies and HCN emission fromNGC 3593 and NGC 4293 . The I /I
ratios are
0.025 ±0.006 and 0.066 ±0.005 in NGC 3593 and NGC
4293 , respectively , which are comparable to that in late type galaxies . The average of the I /I ratios at thecenter of 12 nearby spiral galaxies including latetype was
0.055 ±0.028.［2 ］The profiles of the HCN emission inboth galaxies show different shapes from those of CO
emission . Namely , the HCN emission was detected fromonly a part of probably the ring -like structure in NGC
3593 . The HCN profile shows a double peak in NGC
4293 . On the other hand , the CO spectra in both
galaxies have a peak near their systemic velocity . These
results indicate that the fraction of dense molecular gas ishigh around the center and that dense gas associates withthe ring -like structure and the star -forming activities inthese galaxies .

Figure 1: CO spectra , HCN spectra , and optical images ofsample galaxies . (a) NGC404 . (b) NGC3593 . (c)NGC4293 . Circles in the optical images indicate
the beamsize of the 45m telescope .［1 ］
References［1 ］Kuno , N ., Nakai , N ., Sorai , K ., Nishiyama , K ., Vila -Vilaro , B .:2002 , Publ . Astron . Soc . Japan , 54, 555.
［2 ］Sorai , K ., Nakai , N ., Kuno , N ., Nishiyama , K .: 2002 , Publ .
Astron . Soc . Japan , 54, 179.

Present address : Hokkaido University
Present address : Japan Spaceguard Center
34

A Noise Evaluationof a High Output Power W -Band Photomixer

UEDA , Akitoshi , NOGUCHI , Takashi , SEKIMOTOTAKANO , Shuro , IWASHITA, Yutaro , ISHIGURO
Hiroyuki, Masato ,(Divison of Radio astoronomy , NAOJ )ASAYAMA, Shinichiro

ITO , Hiroshi , NAGATSUMA(Osaka Pref . Univ .)A large radio telescope array called Atacama large
millimeter /sub -millimeter array (ALMA ) is designed toachieve a large collecting area and high angular resolu tion . The observation frequency ranging
from 30 to 950 GHz is divided into 10 frequency bands ,and each band has a 20 to 30 % bandwidth . Local
oscillator (LO ) sources for ALMA are required to have ahigh frequency stability (10at 1s), wide tuning range ,ultra -low noise (10K /μW ), large output power ( 1 mW
at 100GHz ) and common low phase noise reference foreach antenna . Recently , we have developed a 100 GHz
band photomixer using a unitraveling -carrier photodiode［2 ］(UTC -PD ［) 1］. The UTC -PD has a higher satura tion output while maintaining fast response than previous
types of photodiodes . It is expected that the noise of aphotonic LO is higher than that of a Gunn -diode oscil lator , except under the conditions of using very low -noise
optical sources and having a very high current in thephotomixer . In order to study the excess noise in thephotonic LO , we performed an experiment utilizing a
low -noise SIS receiver with a noise temperature of 20 K at
100 GHz ［3 ］
. The experimental setup for noise measure ments of an SIS receiver pumped by different LO sources
is shown in Figure 1. The photomixer is driven by theheterodyne beatnote of the combined output of two DFB
lasers whose emission wavelengths are around 1.55 μm.
The linewidth of the lasers is a few hundred kHz in a freerunning operation . Measured noise temperatures of the
SIS receiver driven by the Gunn and the photonic LOs areplotted in Figure 2. Both cases show the same noise
temperature of around 20 K double -sideband in the frequency range of 96 ‑110 GHz .

, Tadao , HIRATA , Akihiko(Photonics Labs ., NTT )Figure 1: (a) Schematic of a photonic LO . (b) Experimental
setup to measure noise temperature of an SIS
receiver .

References［1 ］H . Ito et al .: 2000 , Electron . Lett ., 21, 1809 .
［2 ］A . Ueda et al .: 2003 , IEEE Trans . Microwave

Theory andTechniques , 51, 1455 .
［3 ］A . Ueda et al .: 2003 , Jpn . J . Appl . Phys ., 42, L704 .

Figure 2: Receiver noise temperatures of the SIS mixer pumped
by a Gunn LO and a photonic LO are shown as afunction of frequency .

35

K3 ‑50A : An Ultracompact HII Region
Ionized by Multiple Ionizing Stars
OKAMOTO, Yoshiko(Kitasato University )YAMASHITAK.

KATAZA, Hirokazu(The Institute of Space and Astronautical, Takuya(Subaru Telescope , NAOJ )MIYATA

Science ), Takashi(Institute of Astronomy , Univ . of Tokyo )SAKO , Shigeyuki , TAKUBO , Shin -ya, HONDA , Mitsuhiko , and ONAKA , Takashi(Department of Astronomy , Univ . of Tokyo )Newly formed massive stars are embedded in natal
molecular clouds and form ultracompact (UC ) HII
regions by ionizing the molecular gas by their emitting
UV photons . Toward a massive star forming region , notonly the UC HII regions but also objects indicating
existence /formation of massive stars , such as hot molecu lar cores , maser sources , and /or out -flows are observed
together . To understand formation processes of massive
stars , it is essential to know how massive stars are relatedwith each object and to know where the forming /formed
massive stars are .
Toward UC HII regions , some ionic lines are obser ved in the mid -infrared region where extinction is muchless than in the optical region . Especially ,［NeII ］12.8μm,［ArIII ］8.99μm, and ［SIV ］10.51μm lines are radiatedfrom ions formed by 22 ‑35eV UV photons . The ionicabundances and distribution derived from maps of theselines can be used to estimate UV radiation ionizing theregions .
We observed an UC HII region K3 ‑50A using theCooledMid -Infrared
Cameraand Spectrometer(COMICS ) on Subaru Telescope and made extinction corrected emission maps of the three lines (Figure 1).
Especially for the ［NeII ］map , the ［NeII ］emission is
resolved into more than two peaks . This indicates thatK3 ‑50A UC HII region is ionized by two or more ioniz ing massive stars . Though the radio continuum emissionof this region suggested that the Lyman continuum
photons from ionizing stars correspond to a single O5 .5Vstar , our mid -infrared line flux ratios suggest that the UV
radiation hardness of this region corresponds to 〜O8V
stars . The difference also suggests that there are multiple
ionizing stars , which is different from the simple picture
usually assumed for UC HII regions in the past radio
observations ［( 1］).
References［1 ］Okamoto , Y . K ., Kataza , H ., Yamashita , T., Miyata , T., Sako ,S ., Takubo , S ., Honda , M ., and Onaka , T.: 2003 , Astrophys . J .,584, 368 ‑384.

Figure 1: Extinction corrected emission maps of ［NeII ］12.8μm,［ArIII ］8.99μm, and ［SIV ］10.51μm toward K3 ‑50A (color
map ). Contours indicate the 11.7μm image .

36

Relations

between Galaxy Formation and Environmentsof Quasars

ENOKI , Motohiro(Osaka Univ ./Divisionof Astrometry and Celestial Mechanics , NAOJ )NAGASHIMA(Division, Masahiroof Theoretical Astrophysics , NAOJ )GOUDA , Naoteru(Divisionof Astrometry and Celestial Mechanics , NAOJ )We investigate the environments of quasars such as
number distribution of galaxies using a semi -analytic
model which includes both galaxy and quasar formations
based on the hierarchicalclustering scenario . We
assume that a supermassive black hole is fueled by accre tion of cold gas and that it is a source of quasar activities
during a major merger of the quasar host galaxy withanother galaxy . This major merger causes spheroid for mation of the host galaxy . Our model can reproduce not
only general form of the galaxy luminosity functions in
the local Universe but also the observed relation between
a supermassive black hole mass and a spheroid luminos ity, the present black hole mass function and the quasar
luminosity functions at different redshifts . Using thismodel , we predict properties of quasar environments .
First , we analyze the mean numbers of quasars andgalaxies in a dark halo (Figure 1). We find that thedependence of the mean number of quasars on halo mass
is different from the dependence of the mean number ofgalaxies . Since spatial distributions of galaxies andquasars depend on the mean numbers of quasars andgalaxies in a dark halo , using the mean numbers , wecalculate the bias parameters of quasars and galaxies(Figure 2). We find that the evolution of the bias param eter of quasars is different from that of galaxies . In ourmodel , the formation effciency both of galaxies andquasars depends on the cold gas mass fraction and thegalaxy merger rate in a dark halo . However , the quasar
formation effciency depends on galaxy merger rate morestrongly and , furthermore , depends on quasar lifetime .
Next , we show the galaxy number distribution func tion around quasars (Figure 3). At lower redshifts (0.
2 ＜z ＜0.5), most halos with quasars have at most several
galaxies . This indicates that most quasars reside ingroups of galaxies . On the other hand , at higher red shifts (1 ＜z ＜2), the number of galaxies in a dark halowith quasars is from several to dozens ; quasars reside inranging from small groups of galaxies to clusters ofgalaxies . These results show that most quasars at higher
redshifts reside in more various environments than atlower redshifts . In our model , we assume that galaxy
major merger triggers quasar activity . Since the galaxy
merger rate has a maximum in halos corresponding togroups of galaxies , 〜10 M , our model predicts thatmost quasars populate in groups .
Present address Astronomical Data Analysis Center , NAOJ
Present address University of DurhamComparing these predictions with observations in the
future will enable us to constrain our quasar formation
model .
References［1 ］Enoki , H . et al .: 2003 , PASJ , 55, 133.

Figure 1: The mean numbers of quasars and galaxies in a dark
halo .

Figure 2: The evolution of the bias parameter of quasars andgalaxies .

Figure 3: The galaxy number distribution
quasars in a dark halo .

function around37

Observationof Solar Flare Hard X -ray Spectra using CdTe Detectors

KOBAYASHI, Ken

TSUNETA(University of Tokyo )KATSUKAWA, Saku , TAMURA(Division, Tomonori , KUMAGAI, Kazuyoshiof Solar Physics , NAOJ ), Yukio , KUBO , Masahito , SAKAMOTO, Yasushi , KOHARA, Naoki(University of Tokyo )YAMAGAMI, Takamasa , SAITO , Yoshitaka(Institute of Space and Astronautical

Science )Solar flares are observed to produce nonthermal elec trons typically in the 10 to 100 keV range but sometimes
reaching 〜 10MeV range . The acceleration mechanismof these electrons remains unknown . Hard X -ray spectra
provide important diagnostic information such as energy
distribution of accelerated electrons and precise tempera ture measurements of thermal sources . To this end wedeveloped a balloon -borne hard X -ray spectrometer capa ble of 3 keV energy resolution over a 20 ‑120 keV energy
range . This is a factor of 3 better than previously laun ched satellites and only surpassed by the recently laun ched RHESSI satellite .
The system is designed for a one day flight at analtitude of 41km by an 80,000m balloon developed andlaunched by the Institute for Space and Astronautical
Science (ISAS ). The main balloon gondola contains
ballast , electronics and batteries , and the detector system
is mounted on top surrounded by thermal shields (Figure1). The entire gondola weighs 70kg . Detector angle isfixed at 45 elevation , and the gondola azimuth iscontrolled to an accuracy of ±5 using a closed -loopsystem . Sun position sensors and magnetic sensors wereused for attitude control , and an additional 2-axis sun
sensor is used to verify pointing .
The detector system contains sixteen 10 ×10 ×0.5mm
CdTe detectors . CdTe detectors have good stopping
power and do not require cryogenic coolers , making it
possible to construct lightweight hard X -ray detector
systems . At the operating temperature of 0 C , all detec tors were shown to have 2.6 keV or better energy resolu tion at the 60 keV Am -241 line . The detector enclosureis hermetically sealed ; the Rohacell /CFRP composite
window was fabricated by Mitsubishi Heavy Industries
and has an areal density of 0.1g cm . The detectors are
passively shielded by 2mm of lead , and a graded -Z col limator limits the field of view to 10 ×60 . The detector
system contains 16 preamplifiers and a 200V bias battery ,and the output signal is sent to a custom made dataacquisition system inside the gondola . The detector
enclosure and thermal shields are designed to cool thedetector by optimizing radiative cooling .
First flight of the instrument took place on August 29,
2001 from the Sanriku Balloon Center . The observation
was cut short by a battery problem and no flares wereobserved , but a detector temperature of ‑15 C was success fully achieved and the instrument was recovered success fully . On the second flight (May 24, 2002 ), 9 hours ofsuccessful observation was performed at an altitude of
41km and a class M1 .1 flare was successfully observed at
6:41 UT . A background subtracted counts spectrum of
the first minute of the flare is shown in Figure 2, alongwith thermal -spectrum fits . The spectrum is consistent38

MORI , Kunishiro(ClearPulse

Co .)KATO , Genzo(Mitsubishi

Heavy Industries )with a purely thermal plasma of 47MK temperature .
This is an unexpectedly high temperature , but our analy sis of a simultaneous RHESSI satellite data is in good
agreement .

Figure 1: Overview and photographof the entire instrument .

Figure 2: Observed flare spectrum with 1-sigma error bars andfits to thermal spectra .

Observational Study of the Three -Dimensional Magnetic
Field Structure and Mass Motion in Active Regions
CHOUDHARY, Debi Prasad

SUEMATSU(NAOJ and Udaipur Solar Observatory )To study the three -dimensional magnetic field struc ture and associated plasma flow properties , spectro polarimetric observations of active regions were carriedout in the spectral lines of Si I 10827 .1 A and He I 10830
A , using the Norikura Universal Spectro -Polarimeter at
Norikura Solar Observatory , NAOJ . Comparison of Si I
(photospheric ) and He I (chromospheric ) magnetogramswith the potential field model shows that a large fractionof the magnetic field is consistent with the potential fieldstructure , by assuming that the height difference between
the origin of the two lines is about 1200 km . The slopeof the scatter plot between Si I and He I magnetograms is
0.5 and 0.76 in an emerging flux and a larger active
region , respectively . These values are lower than the
scatter plot slopes obtained from Kitt Peak photosphericand chromospheric magnetograms , in which case thecorresponding values are 0.83 and 0.9, respectively .
Considering the height difference between these two setsof chromospheric magnetograms , this implies that themagnetic field spreads out faster near the transition region
heights . Dopplergrams
obtained by determining thecentroid of the asymmetric line profiles show that , in case

Figure 1: Sample spectra of wavelength region Si I 10827 .1
A − He I 10830 A obtained with Norikura Univer sal Spectro -Polarimeter . The observed spectra havebeen normalized with a synthetic spectrum obtainedby fitting the contiuum windows . The spectra frommany pixels with different magnetic field strengthand polarity are averaged to produce three sample
spectra . The limits set for grouping the pixels are:‑150 G negative and
150 G for positive ,between ± 150 G for weak . The changes are only
seen in the He I 10830 A feature .

, Yoshinori , ICHIMOTO, Kiyoshi(Solar Physics Division , NAOJ )of emerging flux region , the chromospheric up flow
regions with maximum velocity of about 5 km s arelocated in the magnetic neutral line areas .
References［1 ］Choudhary , D . P . et al .: 2002 , Solar Phys . 209, 349.

Figure 2: The photospheric and chromospheric magnetogramsof the active region NOAA 8350 observed on 10
October 1998 . The field of view is 152 ×160 arc
sec . White and black pixels represent the positive
and negative megnetic fields , respectively .

Figure3: The scatter plot of the observed and computed
chromospheric magnetograms of the active region
shown in Figure 2.

39Subaru /XMM -Newton Deep Survey
SEKIGUCHI
Kazuhiro , AKIYAMA , Masayuki , AOKI , Kentaro , FUSE , Tetsuharu ,FURUSAWA , Hisanori , ISHIDA , Cathy , KAROJI , Hiroshi , KOBAYASHI , Naoto ,KOMIYAMA, Yutaka , KOSUGI , George , MIYAZAKI , Satoshi , NOUMARU ,Jun ʼichi , OGASAWARA, Ryusuke , SASAKI , Toshiyuki , TAKATA , Tadafumi(Subaru Telescope , NAOJ )IMANISHI, Masatoshi , IYE , Masanori , KODAMA , Tadayuki , MIZUMOTOTANAKA , Ichi , YAMADA , Toru , YASUDA , Naoki, Yoshihiko ,(NAOJ )

DOI , Mamoru , OUCHI , Masami , SHIMASAKU, Kazuhiro(Tokyo Univ .)MAEDA , Yoshitomo , UEDA , Yoshihiro

KAJISAWA, Masaru(Tohoku Univ .)NAKATA(ISAS ), Fumiaki , SIMPSON, Chris(Univ . of Durham )YOSHIDA, Michitoshi(Okayama Observatory , NAOJ )Subaru /XMM -Newton Deep Survey is one of theobservatory big -projects of the Subaru Telescope , and weare conducting deep imaging observation down to thelimit of the Subaru Telescope with Suprime -Cam andspectroscopic survey of objects with R ＜24 with FOCAS ,in wide field (1.3 degree ) centered on 0218 -05(J2000 .0).
The aims of the project are
to reveal constituents of the young universe and theirdistribution ,to examine the distribution and the evolution of theluminosity function of QSOs and galaxies ,to reveal the natures of the faint X -ray sources .
In this observing field , X -ray survey with ESA ʼ
s X -raysatellite , XMM -Newton , Sub -mm survey with SCUBA on

Figure 1: The optical image of the survey field taken with
Subaru Prime -Focus Camera (Sprime -Cam ). B , R , ibands three color image with 5 FoV of Suprime Cam . The total FOV is 1.3 degree .

40

JCMT , ultra -deep near -infrared imaging with WFCAM
on UKIRT , deep radio survey with VLA are ongoing .
With these data sets, we can reveal the characteristics ofobjects in the young universe in multi -wavelength in thescale which is free from cosmic variance .
Deep BRi z bands imaging with Suprime -Cam and
X -ray survey observation with XMM -Newton are almost
finished this fiscal year. Radio observation in 1.4GHz
waveband with VLA B -array archives flux limit of 50μJy.
Near -infrared survey observation with SIRIUS on IRSF
(South -African Observatory ) covers 800 arcmin area
down to K ＝19.5. SCUBA observation aiming to reachdown to S ＝8mJy is started . The follow -up spectros copic observation of 1200 X -ray sources and 1000 radiosources found so far is planed in the next year.

Figure 2: X -ray image of the survey field taken with XMM Newton . Blue color means hard X -ray sources , redcolor represents soft X -ray sources . The 1 FoVcovers 30 arcmin diameter , and the image is madefrom 7 FOVs .

The Evolution of Vector Magnetic
KUBO , Masahito

Fields in an Emerging Flux Region

SHIMIZU(University of Tokyo /NAOJ ), Toshifumi , TSUNETA, Saku(Solar Physics Division , NAOJ )B . W . Lites(NCAR /HAO )It is widely believed that the magnetic fields of the sun
are generated in the convection zone and then emerge tothe solar surface via magnetic buoyancy . Regions withemergence are known as emerging flux regions (EFRs ).
Transient phenomena , such as flares , occur frequently andquasi -steady coronal heating is maintained in association
with flux emergence . To understand the mechanisms ofcoronal heating , it is essential to investigate the evolutionof magnetic fields inside EFRs . We have in detail stud ied the evolutions of magnetic fields in an EFR andinterpreted our findings in the process of formation ofsunspots .
Properties of magnetic field in EFRs have long beenstudied using the longitudinal component of the magnetic
field with filter magnetograph . In order to understandmagnetic fields in three dimension and physical parame ters of plasma precisely , we observed the evolution of an
EFR with Advanced Stokes Polarimeter(ASP ) at
National Solar Observatory (Sacramento Peak ) in the
United States . The ASP is a spectropolarimeter capableof precisely measuring the full state of polarization (I , Q ,U , V ). Vector magnetic fields in the photosphere arederived from Stokes profiles .
The previous study indicates that young emerging flux
is horizontal with respect to the solar surface and it has
upward motion (〜0.5km s ). The intrinsic
fleldstrength is about 500 ±300 Gauss , which is weaker thanthat of vertically oriented magnetic field in sunspots . In
this study , we find that an area with high filling factor (＞80% ) newly appears with flux emergence (Figure 1).
Filling factor represents the percentage occupied bymagnetic atmosphere in each pixel . In this area , mag netic field is almost horizontal and their intrinsic fieldstrength ( B 〜500 Gauss ) is weaker than the surrounding
horizontally oriented magnetic field . Compact bipolar
flux region is located at the either end of the horizontal
magnetic field . This region gradually increases in bothsize and its total magnetic flux in association with the flux
emergence . In this region , the magnetic field becomes
vertically oriented and the intrinsic field strength becomesstronger , but filling factor becomes lower . At 12 hours
after its first appearance , the magnetic field is almost
vertical and the intrinsic field strength is about 1500
Gauss . This result may be explained by convective
collapse (Parker 1978 ), in which magnetic field is com pressed to kilogauss because of convergence of magnetic
field by convective flows and ensuing superadiabatic
effect. This is significant result for understanding themechanism that emerging magnetic flux tubes (a few
hundred Gauss ) concentrates up to kilogauss . As thecompact bipolar flux region grows to the sunspot over thefollowing two days , the filling factor increases to 80% .
However , the inclination and field strength are not chan ged . This result may be explained by concentration ofmagnetic flux tubes .
We also obtain the result indicating that the magnetic
field in the EFR is slightly deformed by the preexisting
magnetic environment surrounding the EFR throughmagnetic pressure , although the magnetic field at thephotosphere is dominantly controlled by gas pressure .
This result implies that the emerging flux loops have theenergy larger than potential energy when they reach thephotospheric level .
Reference［1 ］Kubo , M ., Shimizu , T., Lites , B . W .: 2003 , ApJ , accepted .

Figure 1: Magnetic flux images (left ) and filling factor images(right ) in the region where development of new
emerging flux is in progress . These images are
created from ASP observations . White (black ) is
positive (negative ) in the magnetic flux images andwhite (black ) is 0% (100% ) in the filling factor
images .

41

Searchingfor Dark Matter Halos in the Suprime -Cam
2 Square Degree Field
MIYAZAKI, Satoshi(NAOJ )HAMANA, Takashi(IAP /Paris )SHIMASAKU, Kazuhiro , DOI , Mamoru , KIMURA , Masahiko ,OKAMURA , Sadanori , OUCHI , Masami , SEKIGUCHI, Maki(University of Tokyo )FURUSAWA , Hisanori , IMI , Katsumi , KOMIYAMA, Yutaka ,NAKATA , Fumiaki , OKADA , Norio , YAGI , Masafumi , YASUDA , Naoki(NAOJ )

Figure 1: Demonstrating Suprime -Cam ʼs cability for locating
mass concentrations (or halos ) from weak lensing
data in the 2 deg GTO field ［2 ］
. Red contours
indicate mass over -densities where the lensing (con vergence ) signal /noise exceeds 3. Black contours
show the surface density of visible (20 ＜R ＜23)
galaxies . Regions marked (a-h) represent known
clusters which clearly constitute only a fraction of
the massive structures detected in this field .

Clusters of galaxies represent the largest bound systems in the universe and provide important tools fortesting theories of structure formation and constraining
cosmological models . Clusters have traditionally been
identified using their optical or X -ray emission and thus
the available catalogs are inevitably biased toward theselection of luminous objects . However , in dark matter
dominated cosmologies , the usefulness of such catalog ishighly questionable . This proposal is concerned with
providing definitive and unambiguous versions of thesetests based on clusters selected , for the first time , by theirmass rather than their light .
Weak gravitational lensing offers the most reliable
route to selecting clusters independently of any assump tions about their baryon content and thermodynamical
state . The technique uses statistical measures of the
distorted shapes of faint distant galaxies induced by thetidal gravitational field integrated along the line of sight .
This , in turn , allows a reconstruction of 2-D surface massdensity maps which can be used as the basis for the mostreliable searches for mass concentrations completely irre -42

FigureHAMABE, Masaru(Japan Women University )2: Optical counterpart of halo X (see left panel )identified as a new cluster at z ＝0.41 with subse quent FOCAS spectroscopy . This cluster is notlisted in the NASA /IPAC NED catalog .

spective of the nature of the baryonic material in thosesystems . Using GTO data secured with Suprime -Cam［1 ］over a contiguous 2.1 deg field (3 3 Suprime -Campointings ), we demonstrated the first reliable detection of
5 mass concentrations with S /N ＞5 (Figure 1),［2 ］),
thereby paving the way for a systematic search for suchconcentrations or “
dark matter halos ”. An exposure
time of 30 minutes in R -band is sufficient to detect the
weak lensing signal corresponding to a 〜3 10 h M
structure at z ＝0.5 with 8 in 3.5 arcmin aperture . This
corresponds roughly to a modest cluster of galaxies .
The result is consistent with the prediction assuming
the Press -Schechter mass function and the NFW halo
profile under the cluster normalized CDM cosmology .
Although the present statistics is not enough due to thelimited field of view , this work demonstrates that dark
matter halo count via weak lensing is a promising way totest the paradigm of structure formation and cosmologicalmodel .
References［1 ］ Miyazaki , S . et al .: 2002 , PASJ , 54, 833.
［2 ］ Miyazaki , S . et al .: 2002 , ApJ , 580, L97 .

Fabrication of a Bandpass Filter for the Solar Optical
Telescope of Solar -B Using the IBSWASEDA(Division, Kouichi

ICHIMOTO

of Optical and Infrared Astronomy , NAOJ )1. Introduction
The Solar Optical Telescope of the Solar -B mission
consists of a 50cm diameter Gregorian telescope (OTA :Optical Telescope Assembly ) and the Focal Plane Pack age (FPP ). OTA has a collimating lens unit (CLU )sending lights to FPP as a parallel beam . CLU consistsof 6 lens elements and is required to have a very highwavefront performance to provide the diffraction limited
image . One of the most critical issues of the solar tele scope in space is its thermal design ; i.e. unexpectedheating up of the high precision optical elements due tothe absorption of solar light easily causes a degradation of
wavefront performance . To suppress the heat load on
CLU and FPP , a band pass coating is applied on theincidence surface of the CLU to reject the unnecessary
UV and IR lights . Thus the coating is a key component
for the success of diffraction limited solar telescope . We
developed a band pass coating using the Ion Beam
Spattering facility of NAOJ , and after extensive qualifica tion tests , we completed a flight coating for the Solar -B .

(Division, Kiyoshi

of Solar Physics , NAOJ )ment is made , and 4) total thickness of 4 μm. As a result
we obtained a quite satisfactory coating design consistingof 55 layers . Using 8 coating samples (202.3t) weperformed various qualification testing to verify the dura bility in space environment as follows ; 1) transmissivity /reflectivity measurements , 2) tape test, 3) polarization
property measurement , 4) thermal cycling test, 5) humid ity test, 6) UV illumination test, 7) -ray exposure test, 8)
proton -beam exposure test, 9) electron -beam exposure
test. The coating reveals an excellent transmission curveand showed no change of its property after any environ mental tests ; thus we have successfully verified the feasibil ity of its space usage .
3. Fabrication of the flight coating
After the series of qualification tests , we finally decid ed to adopt this coating for flight model and performed
the IBS operation on the flight CLU element on 9-11
November 2002 . The first element of the CLU has 53mm
diameter and a concaved incidence surface with the radiusof curvature of about 250mm . Figure 1 is the view of thecoated lens and Figure 2 shows a measured transmission
curve together with the theoretical one . The coincidenceof measured and theoretical transmission
curves isremarkable . The coated lens was assembled into theflight CLU and a series of optical performance andmechanical environment test have been done successfully .
The CLU is to be installed in the flight telescope in thisautumn .

Figure 1: CLU G1 lens with a coating by IBS .

2. Design of the bandpass coating and the qualificationtests
For materials of the multi -layer coating , we selected a
combination of SiO ＋Ta O , which is known to be
durable against the general environment stress and tohave fairly high transmissivity in a short wavelength .
The optimized design of the multi -layer is obtained using
the Macleod software with conditions that the coating has
1) high transmissivity in observing wavelength ranges(380-470nm , 500-570nm , 620-680nm ), 2) high reflectivity
in UV (300-370nm ) and IR (700-1100nm ), 3) highest
transmissivity at 630nm in which interferometric measure -Figure 2: Transmission curves of the flight bandpass filter .
Measured and theoretical curves are closely over lapped . Vertical bars on the top show wavelengths
of SOT observation .

43

Formation of Protoplanet

Systems and Diversity of Planetary

Systems

KOKUBO , Eiichiro(Divisionof Theoretical Astrophysics , NAOJ )IDA , Shigeru(Department of Earth and Planetary Sciences , Tokyo Institute of Technology )We investigate the dependence of the habitat segrega tion of planets on the mass and the mass distribution of a
protoplanetary disk ［1 ］
. In the solar system , there are
terrestrial (rocky ) planets , Jovian (gaseous ) planets , andUranian (icy ) planets from inside to outside . We explain
this habitat segregation of the planets using the oligarchic
growth model of protoplanets and the condition of Jovian
planet formation . The surface density of the dust compo nent of a protoplanetary disk is given by the power -lawdistribution , Σ ＝Σa , where Σ is the surface den sity at 1AU , a is the heliocentric distance , and α＝3 /2 isthe powerlaw index . Inside the snow border awhere
the disk temperature equals the ice condensation tempera ture , the dust is rocky . For the standard disk model ,2.7AU . Outside the snow border , the dust is icy
and the surface density increases about 4 times due to ice
condensation .
For this model , the oligarchic growth model gives themass and the growth time scale of protoplanets , M Σ
a
and T
Σ
, respectively ［1, 2 ］.
In order for a protoplanet to be a Jovian planet , theprotoplanet must satisfy the two conditions : (1) the con traction time scale (T ) of the gas onto the protoplanet
from the gas disk is shorter than the lifetime of the gas
disk (T ), and (2) the growth time of the protoplanet is

Figure44

1: Habitat segregation of terrestrial , Jovian , andUranian planets . The horizontal axis is the dis tance from the central star and the vertical axis is thesurface density of the solid component at 1AU ,which is proportional to the disk mass .
,,stand for the inner and outer boundaries for
Jovian planet region , and the snow border . The
disk life time is T ＝10 yr (solid ) and 10 yr (bro ken line ).

Figure 2: Schematic illustration of the diversity of planetarysystems . The left large filled circles represent thecentral stars and the other single and double circles
represent terrestria1 /Uranian and Jovian planets ,respectively .

shorter than the lifetime of the gas disk . The contraction
time scale decreases with the mass of protoplanets ［3 ］,
while the growth time of protoplanets increases with themass of protoplanets . For the disk with α＜2, condi tions (1) and (2) determine the inner and the outerboundaries of the Jovian planet region where Jovian
planets can form , respectively . In the inner and the outerregions outside the Jovian region , terrestrial and Uranianplanets form , respectively . Figure 1 shows the habitat
segregation for the disk with α＝3 /2, where the contrac tion time scale is give by T ＝10 (M /M ) yr［3 ］.
We find that for the disk life time 〜10 year, several
Jovian planets would form from massive disks with Σ
30 with Uranian planets outside the Jovian planets .
Only terrestrial and Uranian planets would form fromlight disks with Σ 3. Solar system -like planetary systems would form from medium disks with Σ 10.
The existence of the snow border , the oligarchic
growth model , and the conditions for the Jovian planet
formation naturally explain the habitat segregation ofplanets in the solar system . In other words , the mass , themass distribution , and the temperature profile of the
protoplanetary disk , and its life time determine the basic
structure of planetary systems .
References［1 ］ Kokubo , E ., and Ida , S .: 2002 , ApJ , 581, 666.
［2 ］ Kokubo , E ., and Ida , S .: 1998 , Icarus 131, 171.
［3 ］ Ikoma , M . et al .: 2000 , ApJ 537, 1013 .

Spectroscopic
SAKURAI

Observation, Takashi , ICHIMOTO

of Coronal, Kiyoshi(Solar Physics Division , NAOJ )Observations of solar coronal waves provide valuable
insights into the unresolved problem of coronal heating
mechanisms . Although there have been several reports
on coronal oscillations , their detailed characteristics arestill unclear . Therefore we have conducted a series ofspectroscopic observations of coronal oscillations andwaves by using a coronagraph at the Norikura Solar
Observatory ［1 ］. As a result , a time sequence of over 80
minutes of coronal green line spectra was obtained in1998 . Doppler velocities , line intensities , and line widths
were derived through fitting a single Gaussian to theobserved line profiles . Coronal waves have been clearly
detected in the Doppler velocity data . The Fourier
analysis shows powers in a 1-3 mHz range , and in higher
frequencies (5-7 mHz ) at localized regions . The propa -Waves

RAJU , K . P ., SINGH , Jagdev(Indian Institute of Astrophysics )gation speed of the waves was estimated by correlation
analysis . The line intensity and line width did not show
clear oscillations , but their phase relationship with the
Doppler velocity indicates propagating waves rather thanstanding waves . The existence of Alfven waves whose
speed is 500 km s or faster is possible but inconclusive ,while the existence of slower waves (of the order of 100
km s , possibly sound waves ) is evident . The energy
carried by the detected sound waves is far smaller than therequired heat input rate to the quiet corona .
Reference［1 ］ Sakurai , T., Ichimoto , K ., Raju , K . P ., and Singh , J.: 2002 ,Solar Phys ., 209, 265.

Figure 1: The observed Doppler velocity as a function of time (abscissa ) and position along the spectrograph slit (ordinate ). Whitemeans red shift .

45

Spectroscopic

Studies of the Solar Corona Using Fe X , XIII , XIV Lines

SINGH , Jagdev

SAKURAI, Takashi , ICHIMOTO(Indian Institute of Astronomy , Bangalore ), Kiyoshi , SUEMATSU, Yoshinori(Solar Physics Division , NAOJ )TAKEDA, Aki(Institute of Space and Astronautical
Detailed information on the physical characteristics ofthe solar corona can be obtained from studies of emission line profiles of forbidden lines in the visible and infrared
wavelengths . We have been conducting observations ofcoronal emission lines with various ionization stages byusing a coronagraph at the Norikura Solar Observatory .
From the data of the green (Fe XIV 5303 A ) and red(Fe X 6374 A ) emission lines obtained in 1998 , we stud ied any systematic differences in their properties between
closed and open field structures ［1 ］. The difference inthe time -averaged values of the widths of the green line inopen and closed coronal structures at a given height
above the limb is small , whereas the width of the red line
in open structures is substantially larger than that in theclosed loop -like coronal structures .
We also obtained data of a density -sensitive line pair ,10747 A Fe XIII and 10798 A Fe XIII , in 1998 and 1999
［2 ］
. The ratio of the intensities of the 10747 A and

Science )10798 A emission lines in the individual coronal struc tures range between 1.0 and 2.5 at 10″above the limb ,which corresponds to a density range of 9.8 ×10 −2.4 ×
10 cm . The scale -height temperature values , derived
from the variations of the intensity ratio with height
above the limb for all individual coronal structures , range
between 0.6 ×10 and 8.3 ×10 K with a most -frequentvalue around 1.8 ×10 K . The large values of the scale height temperature for 70% of the structures indicate thatthese structures may not be in hydrostatic equilibrium nor
be isothermal in nature .
References［1 ］Singh , J., Sakurai , T., Ichimoto , K ., Suematsu , Y ., Takeda , A .:2002 , Publ . Astron . Soc . Japan , 54, 793.
［2 ］Singh , J., Sakurai , T., Ichimoto , K ., Takeda , A .: 2002 , Publ .
Astron . Soc . Japan , 54, 807.

Figure 1: Images of the solar corona constructed from the line profiles observed on 1998 September 9. The top row shows the
distribution of 10747 A and 10798 A line intensities in the observed coronal region . The middle and bottom rows indicate
the velocity and line -width distributions , respectively .

46

Measurementof Magnetic Helicity Injection and Free Energy
Loading into the Solar Corona

KUSANO , Kanya , MAESHIRO(Hiroshima, Tomohiro

University )YOKOYAMA, Takaaki(Nobeyama Solar Radio Observatory , NAOJ )SAKURAI, Takashi(Solar Physics Division , NAOJ )Magnetic helicity has attracted great attention recently
in the framework of flare models . However , precise
measurement of the helicity based on real data has notbeen available yet. Therefore we developed a new
methodology which can determine magnetic helicity flux
as well as Poynting flux across the photosphere based on
the magnetographobservation . By applying
thismethod , we studied the injection mechanism of magnetic
helicity and magnetic free energy into the solar corona .
In order to derive the helicity and energy fluxes , first thevelocity tangential to the solar surface is constructed byapplying a correlation tracking technique on the magnetic
observation , and secondly the velocity component acrossthe photosphere is derived from the condition that themagnetic evolution must be consistent with the induction
equation . Through this procedure , we can determine thehelicity and energy fluxes separately for the shear motion
effect and for the flux emerging effect. Based on this new
method , the active region NOAA 8100 was analyzed from
Nov . 1 to 5, 1997 , using the data observed by SOHO /MDI
and the vector magnetograph at NAOJ /Mitaka . The
results indicate that the photospheric shear motion andthe flux emerging process have equally contributed to thehelicity injection , and they supplied magnetic helicity ofthe opposite sign into this active region .

Figure 1: The top panel shows the full -sun X -ray flux in the
period of 1997 November 1-6 monitored by the
GOES satellite . The middle panel shows thehelicity injection rate due to flux emergence (thickline ) and to the shear motion (thin line ). The
bottom panel shows the energy injection rates . The
enhanced flare activity corresponds to the injectionof magnetic helicity .

Reference［1 ］Kusano , K ., Maeshiro , T., Yokoyama , T., Sakurai , T.: 2002 ,Astrophys . J ., 577, 501.

47

The Source of Magnetic

Field Twist in Solar Active Regions

BAO , Shudong(Solar Physics Division , NAOJ /Beijing Astronomical

SAKURAI
Observatory )Observations have revealed that a hemispheric prefer ence of magnetic chirality exists throughout the solar
atmosphere . For example , the current helicity of active
regions is predominantly negative (left -handed twist ) in
the northern hemisphere and positive (right -handed twist )in the southern hemisphere . The explanation for thishemispheric tendency is still open to question , and we will
present our views as follows ［1 ］.
In the photosphere , the differential rotation acting on
already emerged sunspot magnetic fields will lead tonegative current helicity in the northern hemisphere , but
the same effect caused by the Coriolis force is opposite insign . In the turbulent convection zone , the Coriolis force
acting on the rising magnetic flux tubes will result in thenegative magnetic helicity in the northern hemisphere , but, Takashi , SUEMATSU, Yoshinori(Solar Physics Division , NAOJ )the corresponding action by the differential rotation will
give rise to the opposite sign . Moreover , in this region
the α-effect will produce the wrong sign . It should be
noteworthy that the two current helicities generated by the
α-effect, the one in the mean field and the other in thefluctuations , have opposite signs , and the former is posi tive while the latter is negative in the northern hemi sphere . In the overshoot region at the base of the convec tion zone , the current helicity created by the α-effect has
the correct sign .
Reference［1 ］Bao , S .D ., Sakurai , T., and Suematsu , Y .: 2002 , Astrophys . J.,
573, 445.

Figure 1: Influence of differential rotation on the formation of spiral patterns . Panels (a) and (c) represent two pairs of simple
bipolar sunspots . The circular arrows denote the direction of the vortices . In (b) and (d) are shown two twisted flux
tubes above the photosphere that connect the sunspot pairs . The axial electric currents in the tube S S (S S ) flow
antiparallel (parallel ) to the field , respectively .

48

Relation between Pressure Balance Structures and Polar
Plumes from Ulysses High Latitude Solar Wind Observations
YAMAUCHI(NASA, Yohei , SUESS , S .T.

MarshallSpace Flight Center )SAKURAI, Takashi(Solar Physics Division , NAOJ )Ulysses observations have shown that pressure bal ance structures (PBSs ) are a common feature in high latitude , fast solar wind near solar minimum . Previous
studies of Ulysses /SWOOPS plasma data suggested thatthese PBSs may be remnants of coronal polar plumes .
Here we find support for this suggestion in an analysis of
PBS magnetic structure . We used Ulysses magnetometerdata and applied a minimum variance analysis to mag netic discontinuities in PBSs . We found that PBSs pref erentially contain tangential discontinuities , as opposed
to rotational discontinuities and to non -PBS regions inthe solar wind . This suggests that PBSs contain struc tures like current sheets or plasmoids that may be associated with network activity at the base of plumes .
Reference［1 ］Yamauchi , Y ., Suess , S .T., and Sakurai , T.: 2002 , Geophys . Res .
Letters , 29, 21-1.

Figure 1: Illustration of a possible scenario for polar plumeformation . The entire diverging field region will bea plume if heating is supplied in the chromosphereby the reconnection .

49

Dynamical

Ordering

YAMAGUCHI

Yoshihiro(Teikyo Heisei University )of Accelerator
TANIKAWA(Division

Kiyotakaof Theoretical Astrophysics , NAOJ )The standard mapping is the typical model of twist
mappings and has a simple form . However its properties
are not clearly understood .
(1)
(2)
where
is a positive parameter . The anomalous diffu sion along the -axis has been investigated over twenty
years .
Let
be an iteration number andbe adiffusion constant satisfying the relation. If
is satisfied , we call the diffusion anomalous . This isoriginated by the rapid motion along the axis . Ichik awa ‑Kamimura ‑Hatori ［1,2 ］ found that the origin of
anomalous diffusion is the accelerator modes (AMs ).
For example ,positive integers )-AM jumps
in the direction every three iterations and jumps
in the -direction at the first three iterations . The
jumping rate along theaxis increases due to the incre ment of the value of -coordinate of AM . If a mapping
point comes in the vicinity of AMs , it jumps rapidly in the
direction .
We study the mechanism of the appearance of AMs
and derive their dynamical ordering ［3 ］
. We use thefollowing procedure .
［1 ］Using two involutions
and , we expressas. The symmetry axes are defined by the sets offixed points of and .
［2 ］We search the symmetric accelerator modes (SAMs )that start from the symmetry axis and have an orbital
point in the other symmetry axis .
［3 ］We obtain the dynamical ordering of SAMs .
Here we give our results . The following is the
dynamical ordering of SAMs starting from the intervals
in the -axis (one of the symmetry axes ). A
notationmeans that if the initial point of a
3-SAM is located in , the initial point of a 5-SAM exists
in . The symbol (↓) means the same relation . We let
.

50

Modes

Dynamical

ordering

↓

↓

↓

↓

↓

↓

↓

↓

↓

↓

↓

↓

Let
be a critical value of SAMs included in the
dynamical ordering . For example ,is the criticalvalue of. Let
be a critical value at which thelast KAM (Kolmogorov -Arnold -Moser ) curve is des troyed . We prove the following relation .
(3)This means that SAMs appear just after the destruc tion of the last KAM curve . However the anomalous
diffusion aroundwas not observed . We hope a moreaccurate calculation of the diffusion process .
Recently , without using the reversibility , the existenceof accelerator modes in the twist mapping has been
proved ［4 ］.
References［1 ］Ichikawa , Y .H ., Kamimura , T. and Hatori , T.: 1984 , Statistical
Physics & Chaos in Fusion Plasmas (Wiley , 1984 ), 21.
［2 ］Ichikawa , Y .H ., Kamimura , T. and Hatori , T.: 1987 , Physica
D29 , 247.
［3 ］Yamaguchi , Y . and Tanikawa , K .: 2002 , Prog . Theor . Phys .
108, 669.
［4 ］Addas -Zanata , S .: 2002 , Nonlinearity , 15, 1399 .

Observational

Constraints

on Dark Radiation

ICHIKI , Kiyooki

YAHIRO(University of Tokyo )(University of the Ryukyu ), Masanobu
MATHEWS

in Brane Cosmology

KAJINO , Toshitaka , ORITO , Manabu(Theoretical Astrophysics

Division , NAOJ ), G . J.

(University of Notre Dame )We analyze the observational constraints on bran eworld cosmology whereby the universe is described as athree -brane embedded in a five-dimensional anti -de Sitter
space ［1 ］
. In such scenarios , our universe is a sub manifold embedded in a higher -dimensional spacetime .
Physical matter fields are confined to this submanifold ,while gravity can reside in the higher -dimensional
spacetime . In this brane -universe cosmology , the Fried mann equation is modified by the appearance of extra
terms which are derived from the existence of the extra
dimensions ［2 ］
,
Λ

(1)

In the present work we concentrate on the “
dark radia tion ”term which diminishes with cosmic scale factor as
a . The coefficient μ is a constant of integration
obtained by integrating the five-dimensional Einsteinequations . Both positive and negative μ are possible
mathematically . Its magnitude and sign can depend on
the choice of initial conditions when solving the fivedimensional Einstein equation . Hence , even the sign of
μremains an open question . We show that , although theobservational constraints from primordial abundances
allow only a small contribution when this term is positive ,a much wider range of negative values is allowed .
Furthermore , such a negative contribution can reconcile

Figure 1: Light -element abundances as a function of baryon tophoton ratio η. Plotted are models with 0%(blue ), ＋10.5% (red ) and -41% (green ) dark radia tion (relative to the background photon energy
density just before the e e annihilation epoch )with ±2σ uncertainties in the model predictions .
Observational constraints are indicated as horizon tal lines as labeled . Constraint on ηfrom CMB isalso shown as vertical shaded region .

the tension between the observed primordial He and D
abundances (Figure 1). The shaded region on Figure 2
shows allowed values of the dark radiation fraction , ρ /ρ, where ρ is the total energy density in backgroundphotons just before the BBN epoch at T ＝1MeV . Note ,that only a small ( 11% ) positive dark radiation contri bution is allowed while substantial negative dark radia tion (up to 123% ) is allowed and even preferred by theBBN constraints . It is well known that the CMB spec trum is sensitive to many cosmological parameters whichhave almost no effect on BBN . For simplicity , therefore ,we have fixed most cosmological parameters to theiroptimum values and explore the effects of varying thedark radiation content and baryon to photon ratio η.
We have calculated CMB power spectra and made thestandard χ goodness of fit analysis to the combined
BOOMERANG, DASI , and MAXIMA -1 data sets, which
gives the limits to a ratio of dark radiaion to photon
energy density of ＋92% and -135% just before nu cleosynthesis . Figure 2 shows the contours of the darkradiation fraction and Ω h allowed by nucleosynthesis
and the CMB . This shows that the combined nu cleosynthesis and CMB constraints severely limit thepossible sign and amplitude of the dark radiation . The
combined 2σ95% confidence limit from the concordanceof both constraints corresponds to -41% ρ /ρ ＋10.
5% for 4.73 η 5.56 (or 0.0176 Ω h 0.0207 ).

Figure 2: Constrains from the primordial abundances (lines )and the CMB (contours ) on ηand the fraction of the
background photon energy density in dark radiation
ρ /ρ just before the e e annihilation .
References［1 ］Ichiki K . et al .: 2002 , PRD , 66, 043521 .
［2 ］Binetruy P . et al .: 2000 , PLB , B477 , 285.
［3 ］Mukohyama S .: 2000 , PLB , 473, 241.

51

Astrophysical

Reaction Rate for

SUMIYOSHI, Kohsuke

Be by Photodisintegration

UTSUNOMIYA(Numazu College of Technology ), Hiroaki(Konan University )GOKOU , Shinji(Konan University )KAJINO , Toshitaka(Divisionof Theorefical Astrophysics , NAOJ )We study the astrophysical reaction rate for the forma ［1 ］.
tion of Be through the three body reaction
This reaction is one of the key reactions which could
bridge the mass gap at A ＝8 nuclear systems to produce
intermediate -to -heavy mass elements in alpha - andneutron -rich environments such as r-process nucleosynth esis in supernova explosions ［2, 3, 4, 5 ］, s-process nu cleosynthesis in asymptotic giant branch (AGB ) stars［6 ］,
and primordial nucleosynthesis in baryon inhomogeneous
cosmological models ［7 ］.
To calculate the thermonuclear reaction rate in a wide
range of temperatures , we numerically integrate the ther mal average of cross sections assuming a two -steps forma tion through a metastableBe ,Be (n, ) Be .
Off -resonant and on -resonant contributions from theground state in Be are taken into account . As input
cross section , we adopt the latest experimental data by
photodisintegrationof Be with laser -electron photon
beams , which covers all relevant resonances in Be .
Experimental data near the neutron threshold are addedwith -ray flux corrections and a new least -squares analy sis is made to deduce resonance parameters in the Breit Wigner formulation . Based on the photodisintegration
cross section , we provide the reaction rate forBe
in the temperature range from T ＝10 to T ＝10 (T isthe temperature in units ofK ) both in the tabular form
and in the analytical form for potential usage in nuclear
reaction network calculations .
The calculated reaction rate is compared with thereaction rates of the CF88 and the NACRE compilations .
The CF88 rate , which is based on the photoneutron crosssection for the 1 /2 state in Be by Berman et al ., is valid
atdue to lack of the off-resonant contribution .
The CF88 rate differs from the present rate by a factor of
two in a temperature range. The NACRE rate ,which adopted different sources of experimental informa tion on resonance states in Be , is 4-12 times larger thanthe present rate at, but is consistent with thepresent rate to withinat. Due to theslight increase of the reaction rate at, the produc tion of seed elements in the neutrino -driven wind and thealpha -rich freeze -out scenarios can be enhanced . This
may lead to a slightly smaller neutron -to -seed ratio at theonset of r-process , and hence may make an appreciable52

influence on the entropy condition anddynamics of the neutrino -driven wind ［8 ］.

expansion

Figure 1: The reaction rate N ＜ααn ＞ in the present study isshown by the solid curve as a function of tempera ture . The reaction rates by CF88 and NACRE are
shown by dashed and dotted curves , respectively .

References［1 ］Sumiyoshi , K ., Utsunomiya , H ., Goko S ., and Kajino , T.: 2002 ,Nucl . Phys ., 709, 467.
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［3 ］ Sumiyoshi , K ., Suzuki , H ., Otsuki , K ., Terasawa M ., andYamada , S .: 2000 , Publ . Astron . Soc . Japan , 52, 601.
［4 ］Terasawa , M ., Sumiyoshi , K ., Kajino , T., Mathews G . J., andTanihata , I .: 2001 , Astrophys ., J ., 562, 470.
［5 ］ Terasawa , M ., Sumiyoshi , K ., Yamada , S ., Suzuki H ., andKajino , T.: 2002 , Astrophys ., J ., 578, L137 .
［6 ］Iwamoto , N ., Kajino , T., Mathews , G . J., Fujimoto M ., andAoki , W .: 2001 , submitted to ApJ .
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［8 ］Kajino , T., Wanajo , S ., and Mathews , G . J.: 2002 , Nucl . Phys .,A704 , 165.

Ⅱ Publications , Presentations
1. Refereed

Publications

Ahrens , V ., Lewen , F ., Takano , S ., Winnewisser , G .,Urban , S ., Negirev , A . A ., and Koroliev , A . N .: 2002,
Sub -Doppler Saturation Spectroscopy of HCN up to
1 THz and Detection of J ＝3→2 (4→3) Emission
from TMC 1, Zeitschrift fuer Naturforschung , 57a ,669 ‑681.
Ajiki , M ., Taniguchi , Y ., Murayama , T ., Nagao , T .,Veilleux , S ., Shioya , Y ., Fujita , S . S ., Kakazu , Y .,Komiyama , Y ., Okamura , S ., Sanders , D . B ., Oyabu ,S ., Kawara , K ., Ohyama , Y ., Iye , M ., Kashikawa ,N ., Yoshida , M ., Sasaki , T ., Kosugi , G ., Aoki , K .,Takata , T ., Saito , Y ., Kawabata , K . S ., Sekiguchi ,K ., Okita , K ., Shimizu , Y ., Inata , M ., Ebizuka , N .,Ozawa , T ., Yadoumaru , Y ., Taguchi , H ., Ando , H .,Nishimura , T ., Hayashi , M ., Ogasawara , R ., Ichi kawa , S .: 2002 , A New High -Redshift Ly αEmitter :Possible Superwind Galaxy at z ＝5.69, Astrophys . J.
Lett ., 576, L25 ‑L28 .
Akiyama , M ., Ueda , Y ., Ohta , K .: 2002 , A Candidate ofa Type 2 Quasi -stellar Object at z ＝0.9 ： Large
X -Ray Absorption with a Strong Broad H α Emis sion Line , Astrophys . J., 567, 42 ‑49.
Ando , S ., Sato , K ., and Totani , T .: 2003 , Detectabilityof the supernova relic neutrinos and neutrino oscil lation , Astropart . Phys ., 8, 307 ‑318.
Aoki , W ., Ando , H ., Honda , S ., Iye , M ., Izumiura ,H ., Kajino , T ., Kambe , E ., Kawanomoto , S ., Nogu chi , K ., Okita , K ., Sadakane , K ., Sato , B ., Shelton ,I ., Takada -Hidai , M ., Takeda , Y ., Watanabe , E .,and Yoshida , M .: 2002 , Chemical CompositionofCarbon -Rich , Very Metal -Poor Subgiant LP 625 ‑44
Observed with the Subaru /HDS , Publ . Astron . Soc .
Japan , 54, 427 ‑449.
Aoki , W ., Honda , S ., Beers , T . C ., and Sneden , C .:2003 , Measurementof the Europium Isotope Ratio
for the Extremely Metal poor , r -Process -enhanced
Star CS 31082 ‑001, Astron . J ., 586, 506 ‑511.
Aoki , W ., Norris , J . E ., Ryan , S . G ., Beers , T . C ., andAndo , H .: 2002 , Chemicalcompositionof thecarbon -rich , extremely
metal poor star CS29498‑043 ： A new class of extremely metal poor stars
with excesses of magnesium and silicon , Astrophys .
J ., 576, L141 ‑144.
Aoki , W ., Ryan , S . G ., Norris , J . E ., Beers , T . C ., andAndo , H .: 2002 , Subaru /HDS Study of the Extreme ly Metal -Poor Star CS 29498 ‑043 ： Abundance
Analysis
Detailsand Comparison
with Other
Carbon -Rich Objects , Publ . Astron . Soc . Japan , 54,
933 ‑949.
Aoki , W ., Ryan , S . G ., Norris , J . E ., Beers , T . C .,Ando , H ., and Tsangarides , S .: 2002 , A Subaru /High Dispersion Spectrographstudy of lead (Pb )abundances in eight s-process element -rich , metal -poor stars , Astrophys . J ., 580, 1149 ‑1158 .
Arnaboldi , M ., Freeman , K . C ., Okamura , S ., Yasuda ,N ., Gerhard , O ., Napolitano , N . R ., Pannella , M .,Ando , H ., Doi , M ., Furusawa , H ., Hamabe , M .,Kimura , M ., Kajino , T ., Komiyama , Y ., Miyazaki ,S ., Nakata , F ., Ouchi , M ., Sekiguchi , M ., Shimasa ku , K ., and Yagi , M .: 2003 , Narrow band imaging in［OIII ］ and H -α to search for ICPNe in the Virgocluster , Astron . J ., 125, 514 ‑524.
Asada , H ., Hamana , T ., Kasai , M .: 2003 , Images for an
isothermal
ellipsoidal
gravitationallens from asingle real algebraic equation , Astron . Astrophys .,397, 825 ‑829.
Asada , K ., Inoue , M ., Uchida , Y ., Kameno , S ., Fujis awa , K ., Iguchi , S ., and Mutoh , M .: 2002 , A Helical
Magnetic Field in the Jet of 3C 273, Publ . Astron .
Soc . Japan , 54, L39 ‑L43 .
Asai , A ., Ishii , T . T ., Kurokawa , H ., Yokoyama , T .,and Shimojo , M .: 2003 , Evolution of Conjugate
Footpoints
inside Flare Ribbons during a GreatTwo -Ribbon Flare on 2001 April 10, Astrophys . J.,
586, 624 ‑629.
Asai , A ., Masuda , S ., Yokoyama , T ., Shimojo , M .,Isobe , H ., Kurokawa , H ., and Shibata , K .: 2002 ,Difference between Spatial Distributions of the H α
Kernels and Hard X -Ray Sources in a Solar Flare ,Astrophys . J. Lett ., 578, L91 ‑L94 .
Bao , S . D ., Sakurai , T ., and Suematsu , Y .: 2002 , The
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Regions , Astrophys . J., 573, 445 ‑453.
Barraud , C ., Olive , J .-F ., Lestrade , J . P ., Atteia , J .-L .,Hurley , K ., Ricker , G ., Lamb , D . Q ., Kawai , N .,Boer , M ., Dezalay , J .-P ., Pizzichini , G ., Vanderspek ,R ., Crew , G ., Doty , J ., Monnelly , G ., Villasenor , J .,Butler , N ., Levine , A ., Yoshida , A ., Shirasaki , Y .,Sakamoto , T ., Tamagawa , T ., Torii , K ., Matsuoka ,M ., Fenimore , E . E ., Galassi , M ., Tavenner , T .,Donaghy , T . Q ., Graziani , C ., Jernigan , J . G .: 2003 ,Spectral analysis of 35 GRBs /XRFs observed with
HETE -2 /FREGATE , Astron . Astrophys ., 400, 1021
‑1030 .
Barucci , M . A ., Boehnhardt , H ., Dotto , E ., Doressoun diram , A ., Romon , J ., Lazzarin , M ., Fornasier , S ., deBergh , C ., Tozzi , G . P ., Delsanti , A ., Hainaut , O .,Barrera , L ., Birkle , K ., Meech , K ., Ortiz , J . L .,Sekiguchi , T ., Thomas , N ., Watanabe , J ., West , R .
M ., and Davies , J . K .: 2002 , Visible and near -infrared
spectroscopyof the Centaur 32532 (2001 PT13 ),Astron . Astrophys ., 392, 335 ‑339.
Beers , T . C ., Drilling , J . S ., Rossi , S ., Chiba , M ., Rhee ,J ., Fuhrmeister , B ., Norris , J . E ., Hippel , T .: 2002 ,Metal Abundances and Kinematics of Bright Metal poor Giants Selected from the LSE Survey : Implica tions for the Metal -weak Thick Disk , Astron . J.,
124, 931 ‑948.
53

Boehnhardt , H ., Delsanti , A ., Barucci , A ., Hainaut , O .,Doressoundiram , A ., Lazzarin , M ., Barrera , L ., deBergh , C ., Birkle , K ., Dotto , E ., Meech , K ., Ortiz , J .
E ., Romon , J ., Sekiguchi , T ., Thomas , N ., Tozzi , G .
P ., Watanabe , J ., and West , R . M .: 2002 , ESO Large
Program on Physical Studies of Transneptunian
Objects and Centaurs : Visible Photometry ‑ First
Results , Astron . Astrophys ., 395, 297 ‑303.
Bouquillon , S ., Kinoshita , H ., and Souchay , J .: 2003 ,Extension of Cassini ʼs Lawa , Celest . Mech . Dyn .
Astr ., 86, 29 ‑57.
Carilli , C . L ., Kohno , K ., Kawabe , R ., Ohta , K ., Hen kel , C ., Menten , K . M ., Yun , M . S ., Petric , A ., andTutui , Y .: 2002 , High -Resolution Imaging of Molecu lar Line Emission
from High -Redshift
QSOs ,
Astron . J., 123, 838 ‑1846 .
Chin , C . C ., Wang , M . J ., Shah , W . L ., Zhang , W .,Cheng , H . W ., Shi , S . C ., and Noguchi , T .: 2002 , A
Fixed Tuned Low Noise 600 ‑700 GHz SIS Receiver ,Int . J. of IR and MM Waves , 23, 731 ‑744.
Choudhary , D . P ., Suematsu , Y ., and Ichimoto , K .:2002 , Observational Study of the Three -Dimensional
Magnetic
Field Structureand Mass Motionin
Active Regions , Solar Phys ., 209, 349 ‑360.
Chrysostomou , A ., Aitken , D . K ., Jenness , T ., Davis , C .
J ., Hough , J . H ., Curran , R ., and Tamura , M .: 2002 ,The magnetic field structure in W51A , Astron .
Astrophys ., 385, 1014 ‑1021 .
Deguchi , S ., Fujii , T ., Nakashima , J .-I ., and Wood , P .
R .: 2002 , Near -Infrared Observations of the IRAS /SiO Sources in the Galactic Bulge : a Large Scale
Distribution , Publ . Astron . Soc . Japan , 54, 719 ‑734.
Dermawan , B ., Nakamura , T ., Fukushima , H ., Sato ,H ., Yoshida , F ., and Sato , Y .: 2002 , CCD
photometry of the MUSES -C mission target : Aster oid (25143 ) 1998SF36 , Publ . Astron . Soc . Japan , 54,
635 ‑640.
Enoki , M ., Nagashima , M ., and Gouda , N .: 2003 ,Relations between Environmentsof Quasars andGalaxy Formation , Publ . Astron .Soc . Japan , 55, 133‑142.
Enomoto , R ., Tanimori , T ., Naito , T ., Yoshida , T .,Yanagita , S ., Mori , M ., Edwards , P . G ., Asahara , A .,Bicknell , G . V ., Gunji , S ., Hara , S ., Hara , T ., Haya shi , S ., Itoh , C ., Kabuki , S ., Kajino , F ., Katagiri , H .,Kataoka , J ., Kawachi , A ., Kifune , T ., Kubo , H .,Kushida , J ., Maeda , S ., Maeshiro , A ., Matsubara , Y .,Mizumoto , Y ., Moriya , M ., Muraishi , H ., Muraki ,Y ., Nakase , T ., Nishijima , K ., Ohishi , M ., Okumura ,K ., Patterson , J . R ., Sakurazawa , K ., Suzuki , R .,Swaby , D . L ., Takano , K ., Takano , T ., Tokanai , F .,Tsuchiya , K ., Tsunoo , H ., Uruma , K ., Watanabe , A .,Yoshikoshi , T .: 2002 , The accelerationof cosmic ray protons in the supernova remnant RX J1713 .7‑3946 , Nature , 416, 823 ‑826.
Enya , K ., Yoshii , Y ., Kobayashi , Y ., Minezaki , T .,Suganuma , M ., Tomita , H ., Peterson , B . A .: 2002 ,JHK ʼImaging Photometryof Seyfert 1 Active
Galactic
Nucleiand Quasars .I . Multiaperture
54

Photometry , Astrophys . J. Suppl . Ser ., 141, 23 ‑29.
Enya , K ., Yoshii , Y ., Kobayashi , Y ., Minezaki , T .,Suganuma , M ., Tomita , H ., Peterson , B . A .: 2002 ,JHK ʼimaging photometry of Seyfert 1. I . (Enya ＋,
2002 ), VizieR On -line Data Catalog , 141, 23.
Enya , K ., Yoshii , Y ., Kobayashi , Y ., Minezaki , T .,Suganuma , M ., Tomita , H ., Peterson , B . A .: 2002 ,JHK ʼImaging Photometryof Seyfert 1 Active
Galactic Nuclei and Quasars . II . ObservationofLong -Term Variability , Astrophys . J. Suppl . Ser .,141, 31 ‑44.
Enya , K ., Yoshii , Y ., Kobayashi , Y ., Minezaki , T .,Suganuma , M ., Tomita , H ., Peterson , B . A .: 2002 ,JHK ʼImaging Photometryof Seyfert 1 Active
Galactic
Nuclei and Quasars . III . VariabilityofRadio -Quiet and Radio -Loud Active Galactic Nu clei , Astrophys . J. Suppl . Ser ., 141, 45 ‑59.
Famiano , M . A ., Boyd , R . N ., and Kajino , T .: 2002 ,Light element nucleosynthesis
from jet interactionsin active galactic nuclei , Astrophys . J ., 576, 89 ‑100.
Ford , A ., Jeffries , R . D ., Smalley , B ., Ryan , S . G .,Aoki , W ., Kawanomoto , S ., James , D . J ., andBarnes , J . R .: 2002 , Lithium 6104A in Population II
stars , Astron . Astrophys ., 393, 617 ‑628.
Fujimoto , H ., Mochizuki , M ., Mitsuzawa , K ., Tamaki ,T ., Sato , T .: 2003 , Ocean bottom pressure variationsin the southeastern Pacific following the 1997 ‑98 El
Nino event , Geophys . Res . Lett ., 30, 10.1029 /2002GL016677 .
Fujita , S . S ., Ajiki , M ., Shioya , Y ., Nagao , T ., Mur ayama , T ., Taniguchi , Y ., Okamura , S ., Ouchi , M .,Shimasaku , K ., Doi , M ., Furusawa , H ., Hamabe , M .,Kimura , M ., Komiyama , Y ., Miyazaki , M ., Miyaza ki , S ., Nakata , F ., Sekiguchi , M ., Yagi , M ., Yasuda ,N ., Matsuda , Y ., Tamura , H ., Hayashino , T .,Kodaira , K ., Karoji , H ., Yamada , T ., Ohta , K .,Umemura , M .: 2003 , A Search for Ly α Emitters at
Redshift 3.7, Astron . J ., 125, 13 ‑31.
Fujita , S . S ., Ajiki , M .,Shioya , Y ., Nagao , T ., Mur ayama , T ., Taniguchi , Y ., Umeda , K ., Yamada , S .,Yagi , M ., Okamura , S ., and Komiyama , Y .: 2003 ,The H α; Luminosity Function and Star Formation
Rate at z 〜0.24 Based on Subaru Deep Imaging
Data , Astropys . J ., 586, L115 ‑L118 .
Fujita , Y ., Takizawa , M , and Sarazin , C . L .: 2003 ,Nonthermal
Emissions from Particles Accelerated
by Turbulence in Clusters of Galaxies , Astrophys .,J ., 584, 190.
Fukagawa , M ., Tamura , M ., Suto , H ., Itoh , Y .,Murakawa , K ., Oasa , Y ., Hayashi , S . S ., Naoi , T .,Kaifu , N ., Doi , Y .: 2002 , Subaru Near -IR Corona graphic Image of LkH α 198, Pub . Astron . Soc .
Japan , 54, 969 ‑973.
Furuya , R . S ., Kitamura , Y ., Wootten , A ., Claussen , M .
J ., and Kawabe , R .: 2003 , Water Maser Survey
toward Low -Mass Young Stellar Objects in the
Northern Sky with the Nobeyama 45 Meter Tele scope and the Very Large Array , Astrophys . J.
Suppl . ser ., 144, 71 ‑134.

Gelfreikh , G . B ., Makarov , V . I ., Tlatov , A . G ., Rieho kainen , A ., and Shibasaki , K .: 2002 , A Study of theDevelopment of Global Solar Activity in the 23rd
Solar Cycle Based on Radio Observations with theNobeyama Radio Heliograph . I . Latitude Distribu tion of the Active and Dark Regions , Astron . Astro phys ., 389, 618 ‑623.
Gelfreikh , G . B ., Makarov , V . I ., Tlatov , A . G ., Rieho kainen , A ., and Shibasaki , K .: 2002 , A Study of theDevelopment of Global Solar Activity in the 23rd
Solar Cycle Based on Radio Observations with theNobeyama Radio Heliograph . II . Dynamics of thedifferential rotation of the Sun , Astron . Astrophys .,389, 624 ‑628.
Gopalswamy , N ., Shimojo , M ., Lu , W ., Yashiro , S .,Shibasaki , K ., and Howard , R . A .: 2003 , Prominence
Eruptions and Coronal Mass Ejection : A Statistical
Study Using Microwave Observations , Astrophys . J .,586, 562 ‑578.
Goto , M ., Gaessler , W ., Hayano , Y ., Iye , M .,Kamata , Y ., Kanzawa , T ., Kobayashi , N ., Min owa , Y ., Saint -Jacques , D . J ., Takami , H ., Takato ,N ., Terada , H .: 2003 , Spatially
Resolved 3 um
Spectroscopyof IRAS 22272 ＋5435 ： Formationand Evolution of Aliphatic Hydrocarbon
Dust inProto -Planetary Nebula , Astrophys . J ., 589, 419 ‑429.
Goto , M ., McCall , B . J ., Geballe , T . R ., Usuda , T .,Kobayashi , N ., Terada , H ., Oka , T .: 2002 , Absorop tion Line Survey of H3 ＋ toward the Galactic
Center Sources I . GCS3 ‑2 and GC IRS3 , Publ .
Astron . Soc . Japan , 54, 951 ‑961.
Gouda , N ., Tsujimoto , T ., Kobayashi , Y ., Nakajima ,T ., Yasuda , N . and Matsuhara , H .: 2002 , Japanese
Astrometry Satellite Mission for Infrared Explora tion , Astrophys . Space Sci ., 280, 89 ‑94.
Gough , D . O ., and Sekii , T .: 2002 , On the effect ofError Correlation
on Linear Inversion , Mon . Not .
Roy . Astron . Soc ., 335, 170 ‑176.
Hamana , T ., Yoshida , N ., Suto , Y .: 2002 , Reliability of
the Dark Matter Clusteringin Cosmological
NBody Simulations
on Scales below the Mean Sepa ration Length of Particles , Astrophys . J ., 568, 455‑462.
Hattori , T ., Yoshida , M ., Ohtani , H ., Ishigaki , T .,Sugai , H ., Hayashi , T ., Ozaki , S ., and Ishii , M .: 2002 ,Tridimensional
Spectroscopic
Observationof theInteracting
System NGC 7592 , Publ . Astron . Soc .
Japan , 54, 393 ‑404.
Heinzel , G ., Braxmaier , C ., Schilling , R ., Rudiger , A .,Robertson D ., te Plate , M ., Wand , V ., Arai , K .,Johann , U ., and Danzmann , K .: 2003 , Interferometry
for the LISA technology package (LTP ) aboard
SMART -2, Class . Quantum Grav ., 20, S153 .
Heki , K .: 2003 , Snow load and seasonal variation ofearthquake occurrence in Japan , Earth Planet . Sci .
Lett ., 207, 159 ‑164.
Honda , M ., Kataza , H ., Okamoto , Y . K ., Miyata , T .,Yamashita , T ., Sako , S ., Takubo , S ., and Onaka ,T .: 2003 , Detection of Crystalline Silicates aroundthe T Tauri Star Hen 3 ‑600A , Astrophys . J. Lett .,585, L59 ‑L63 .
Honda , S ., Aoki , W ., Ando , H ., and Kajino , T .: 2003 ,New detection of r-process elements in extremely
metal -poor stars with SUBARU -HDS , Nucl . Phys .
A , 718, 674 ‑676.
Honma , M ., and Kurayama , T .: 2002 , Astrometric
Microlensingof Distant Sources Caused by Stars in
the Galaxy , Astrophys . J ., 568, 717 ‑725.
Hosokawa , M ., Jauncey , D ., Reynolds , J ., Tzioumis ,A ., Ohnishi , K ., and Fukushima , T .: 2002 , Possible
Fluctuation of the Position of Sagittarius A Rela tive to Extragalactic
Radio Sources , Astrophys . J.,
580, 43.
Huang , G .-L ., and Nakajima , H .: 2002 , Diagnosis ofcoronal magnetic field with data of Nobeyama
Radio Heliograph , New Astronomy , 7, 135 ‑145.
Ibukiyama , A ., and Arimoto , N .: 2002 , HIPPARCOS
age -metallicity relation of the solar neighbourhood
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Takeda , M ., and Noguchi , T.: 2002 , A 200 ‑285 ‑GHz
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Takeda , Y ., Sato , B ., Kambe , E ., Sadakane , K ., andOhkubo , M .: 2002 , Spectroscopic
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Takeda , Y ., Sato , B ., Kambe , E ., Watanabe , E ., Miy azaki , 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 ., andMiyama , S . M .: 2002 , Iodine -Cell SpectroscopyatOkayama AstrophysicalObservatory : First Results ,Publ . Astron . Soc . Japan , 54, 113 ‑120.
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Tanikawa , K ., and Yamaguchi , Y .: 2002 , Non symmetric periodic points in reversible maps : exam ples from the standard map , Progr . Theor . Phys ., 108,987 ‑997.
Tanikawa , K ., and Yamaguchi , Y .: 2003 , Non -Birkhoff
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Tanuma , S ., Yokoyama , T., Kudoh , T ., and Shibata , K .:2003 , Magnetic Reconnection Triggered by the Parker
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Taruya , A ., Hamana , T., Kayo , I .: 2003 , Non -Gaussian
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Taruya , A ., Takada , M ., Hamana , T., Kayo , I .,Futamase , T .: 2002 , Lognormal
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Terasawa , M ., Sumiyoshi , K ., Yamada , S ., Suzuki , H .,and Kajino , T.: 2002 , R -process nucleosynthesis
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M .: 2002 , VSOP Space VLBI and Geodetic VLBI
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Radio
Sources , Astrophys . J. Suppl ., 141, 311 ‑335.
Tomaru , T ., Miyoki , S ., Ohashi , M ., Kuroda , K .,Uchiyama , T ., Suzuki , T ., Yamamoto , A ., Shintomi ,T ., Ueda , A ., Tatsumi , D ., Sato , S ., Arai , K ., Ando ,M ., Watanabe , K ., Nakamura , K ., Watanabe , M ., Ito ,K ., Kataoka , I ., Yamamoto , H ., Bochner , B ., andHefetz , Y .: 2002 , Evaluation of the Performanceof
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Tomisaka , K .: 2002 , Collapse of Rotating Magnetized
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Totani , T., and Inoue , S .: 2002 , Preheating in the uni verse suppressing
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Totani , T., and Panaitescu , A .: 2002 , Orphan Afterglows
of CollimatedGamma -Ray Bursts : Rate Predictions
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Totani , T., and Takeuchi , T . T .: 2002 , A Bridge from
Optical to Infrared Galaxies : Explaining Local Prop erties and Predicting Galaxy Counts and the Cosmic
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Totani , T., Kawasaki , W ., and Kawai , N .: 2002 , A Deep
Optical Observation
for an Enigmatic
Unidentified
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Totani , T.: 2003 , Cluster -Cluster Microlensing
as aProbe of Intracluster Stars , MACHOs , and Remnantsof the First -Generation Stars , Astrophys . J., 586, 735‑744.
Tsuji , T ., and Nakajima , T.: 2003 , Transition from L to
T Dwarfs on the Color -Magnitude
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Tsujimoto , T., and Shigeyama , T .: 2002 , History ofMilky Way Dwarf Spheroidal Galaxies Imprinted on
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Tsujimoto , T., and Shigeyama , T .: 2003 , Relics of Sub luminous Supernovae in Metal -poor Stars , Astrophys .
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Tsujimoto , T., Shigeyama , T ., and Yoshii , Y .: 2002 ,Chemical
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Wada , K ., and Norman , C . A .: 2002 , Obscuring Material
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Wada , K ., Meurer , G ., and Norman , C . A .: 2002 , Gravity Driven Turbulence in Galactic Disks , Astrophys . J.,

577, 197 ‑205.
Watanabe , J ., Kawakita , H ., Furusho , R ., and Fujii , M .:2003 , Heliocentric
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Watanabe , J ., Sekiguchi , T., Shikura , M ., Naito , S ., andAbe , S .: 2002 , Wide -Field TV Observationof theLeonid Meteor Storm in 2001 ： Main Peak overJapan , Publ . Astron . Soc . Japan , 54, L23 ‑L26 .
Watanabe , S ., Akiyama , M ., Ueda , Y ., Ohta , K ., Mu shotzky , R ., Takahashi , T ., and Yamada , T.: 2002 ,Chandra Observations
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White , S . M ., Kundu , M . R ., Garaimov , V . I ., Yokoyama ,T., and Sato , J .: 2002 , The Physical Properties of a
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Yahiro , N ., Mathews , G . J ., Ichiki , K ., Kajino , T., andOrito , M .: 2002 , Constraints on Cosmic Quintessenceand quintessential
inflation , Phys . Rev . D , 65, 063502 .
Yamada , T., Koyama , Y ., Nakata , F ., Kajisawa , M .,Tanaka , I ., Kodama , T., Okumura , S ., De Propris , R .:2002 , Witnessing
the Hierarchical
Assembly of theBrightest
Cluster Galaxy in a Cluster at z ＝1.26,
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Yamaguchi , Y ., and Tanikawa , K .: 2002 , Dynamicalorderingof non -Birkhoff
orbits and topologicalentropy in the standard mapping , Prog . Theor . Phys .,107, 1117 ‑1145 .
Yamaguchi , Y ., and Tanikawa , K .: 2002 , Dynamicalordering of periodic accelerator
modes in the stan dard mapping , Prog . Theor . Phys ., 108, 669 ‑678.
Yamaguchi , Y ., and Tanikawa , K .: 2002 , Non -Birkhoff
periodic orbits in a circle mapping , Prog . Theor . Phys .,108, 231 ‑240.
Yamauchi , Y ., Suess , S . T ., and Sakurai , T.: 2002 ,Relation between Pressure Balance Structures
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Yano , T., Chiba , M ., Gouda , N .: 2002 , Kinematic analy sis of spiral structures in the local disk , Astron .
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Yokoyama , T., Nakajima , H ., Shibasaki , K ., Melnikov ,V . F ., and Stepanov , A . V .: 2002 , Microwave Observa tions of the Rapid Propagationof Nonthermal
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Yoshida , H .: 2002 , Non -existence of the modified first
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Yoshimura , K ., Kurokawa , H ., Shimojo , M ., and Shine ,R .: 2003 , Close Correlation among H α Surges , Mag netic Flux Cancellations , and UV Brightenings Found
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Zare , K ., and Tanikawa , K .: 2002 , Reversible maps intwo degrees of freedom Hamiltoniansystems , Chaos ,12, 699 ‑705.
Zhang , H ., LaBonte , B ., Li , J ., and Sakurai , T.: 2003 ,Analysis of Vector Magnetic Fields in Solar Active
Regionsby Huairou , Mees , and Mitaka
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Zhong , M ., Naito , I ., and Kitoh , A .: 2003 , Atmospheric ,hydrological , and ocean current contributions
toEarth ʼs annual wobble and length -of -day signals basedon output from a climate model , J. Geophys . Res ., 108,
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Zhu , Z . H ., and Fujimoto , M .-K .: 2002 , Cardassian
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Zhu , Z . H ., and Fujimoto , M .-K .: 2003 , Constraints on
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2. Publications
Observatoryof the Nationalof Japan

Astronomical

Soma , M ., and Kato , Y .: 2002 , Limb Profiles of theMoon from Grazing Occultation
Observations
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Miyauchi -Isobe , N ., and Maehara , H .: 2002 , The Sec ond Kiso Survey for Ultraviolent -Excess Galaxies . III ,Publ . Natl . Astron . Obs . Japan , 6, 107 ‑146.
Makita , M .: 2003 , Chromospheric
Structure
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Natl . Astron . Obs . Japan , 7, 1 ‑24.

3. Report of the National Astronomical
Observatory of Japan (in Japanese )Watanabe , M ., Aoki , K ., Miura , A ., Yasuda , N .: 2002 ,Java -based Multi -wavelength
Astronomical
Image
Service ON -line , Rep . Nat . Astron . Obs . Japan , 6, 1 ‑9.
Tanaka , N ., Kobiki , T., Saito , M ., Shinoda , K ., andIrie , M .: 2002 , Observationsof the Mie Scattered
Light Intensities
around the Sun with a Portable
Coronagraph , Rep . Nat . Astron . Obs . Japan , 6, 11 ‑21.
Baba , H ., Yasuda , N ., Ichikawa , S .-I ., Yagi , M .,Iwamoto , N ., Takata , T., Horaguchi , T ., Taga , M .,Watanabe , M ., Okumura , S .-I ., Ozawa , T ., Yamanoto ,N ., and Hamabe , M .: 2002 , Developmentof Pulic
Science Archive System of Subaru Telescope , Rep .
Nat . Astron . Obs . Japan , 6, 23 ‑36.
Saito , M ., and Irie , M .: 2002 , MeteorologicalObserva tions at Norikura
Solar Observatory , Rep . Nat .
Astron . Obs . Japan , 6, 37 ‑47.
64

Tamura , T., Hara , H ., Tsuneta , S ., Ichimoto , K ., andKumagai , K .: 2002 , Contaminations
Evaluation andControl for Solar -B Optical Telescope , Rep . Nat .
Astron . Obs . Japan , 6, 49 ‑58.
Iwashita , H ., and Matsuda , K .: 2003 , First Actions
Towards Dust -proof Clean Conditions in Optical Lab
of Mikata Optical and Infrared Array (MIRA -I . 2):
Clean Level of Air in Laboratory Room , Rep . Nat .
Astron . Obs . Japan , 6, 59 ‑65.
Ozawa , T ., Yadoumaru , Y ., Okyudo , M ., Taguchi , H .,Ichikawa , S .-I ., and Watanabe , J .-I .: 2003 , Develop ment of the Night Sky Movie System Using Timelap se Cinematography , Rep . Nat . Astron . Obs . Japan , 6,
67 ‑78.

4. Other Publications
Abada -Simon , M ., Mouchet , M ., Casares , J ., Evans , A .,Eyres , S . P . S ., Fender , R . P ., Garrington , S . T ., deJager , O ., Kuno , N ., Martinez -Pais , I . G ., de Martino ,D ., Matsuo , H ., Pooley , G ., Ramsay , G ., Salama , A .,and Schulz , B .: 2002 , First Detections of the Cataclys mic Variable AE Aquarii from 4.8 to 7.3 Microns , andat 90 Microns with ISO , SF2A -2002 ： Semaine de l ʼAstrophysique Francaise , eds . F . Combes , and D . Bar ret , EdP -Sciences (Editions de Physique ), Conf . Ser .
Abe , M ., Ohba , Y ., Ishiguro , M ., Hasegawa , S ., Fuse , T.,
Aoki , K ., Ohyama , Y ., Kashikawa , N ., Tokunaga ,A ., Goto , M ., Usuda , T., Terada , H ., Kobayashi , N .,Fujiwara , A .: 2002 , Physical Model and Taxonomic
Type of 1998 SF36 , the Target Asteroid of Sample
Return Mission , MUSES -C , 33rd Annual Lunar andPlanetary Science Conf ., 33, 1666 ‑1667 .
Abe , S ., Yano , H ., Ebizuka , N ., Kasuga , T ., Watanabe ,J ., Sugimoto , M ., Fujino , N ., Fuse , T., Ogasawara ,R .: 2002 , First results of OH emission from meteor
and afterglow : search for organics
in cometarymeteoroids , Proc . Asteroids , Comets , Meteors ‑ ACM
2002 , ESA SP -500, 213 ‑216.
Akabane , K ., and Kuno , N .: 2002 , Dust Content in
Compact HII Regions (NGC 7538 ‑ IRS 1, IRS 2, andIRS 3 ), Proc . of the IAU 8th Asian -Pacific Regional
Meeting , 2, 121 ‑122.
Akiyama , S ., and Hara , H .: 2002 , Soft X -ray High Temperature
Regions
above Solar Flare Loops ,Multi -Wavelength Observations of Coronal Structure
and Dynamics ― Yohkoh 10th Anniversary Meeting ,eds . P . C . H . Martens and D . P . Cauffman , COSPAR
Colloq . Ser ., 13, 367 ‑370.
Aoki , W .: 2003 , Subaru /HDS Studies on Elemental
Abundances of very metal -poor stars , Nuclear Physics ,A718 , 37c -44c .
Appourchaux , T ., Andersen , B ., and Sekii , T.: 2002 ,What Have We Learnt with the Luminosity Oscilla tions Imager over the Past 6 Years ?, ʻ
SOHO 11
Workshop : From Solar Min to Max : Half a Solar
Cycle with SOHO ʼ, ed . A . Wilson , ESA Publication
Division , 47 ‑50.
Asahara , A ., Komiyama , Y ., Kosugi , G ., Kubo , H .,

Miyazaki , S ., Mori , M ., Nakagiri , M ., Nishida , D .,Ogasawara , R ., Orito , R ., Sakurazawa , K ., Takata ,T., Tanimori , T ., Usuda , T.: 2003 , Performance of 10‑100 GeV gamma ray camera for SUBARU
optical infared telescope , Proc . SPIE , 4858 , 347 ‑357.
Asai , A ., Masuda , S ., Yokoyama , T., Shimojo , M ., Ishii ,T . T ., Isobe , H ., Shibata , K ., and Kurokawa , H .: 2002 ,Evolution of Flare Ribbons and Energy Release , Proc .
of the IAU 8th Asian -Pacific Regional Meeting , 2, 415‑416.
Asaki , Y ., Hirosawa , H ., Ichikawa , M ., Hirabayashi , H .,Kobayashi , H ., and Ishiguro , M .: 2002 , Comparison of
AtmosphericPhase Fluctuations
with a 22 GHz
Water Vapor Line Measurements
Along a Single Lineof Sight , Proc . of a workshop “Astronomicalsite
evaluation in the visible and radio range : IAU Techni cal Workshop ”, eds . J . Vernin , Z . Benkhaldom , C .
Munoz -Tunon , ASP Conf . Ser ., 266, 230 ‑237.
Boehnhardt , H ., Barucci , A ., Delsanti , A ., de Bergh , C .,Doressoundiram , A ., Romon , J ., Dotto , E ., Tozzi , G .,Lazzarin , M ., Fournisier , S ., Peixinho , N ., Hainaut ,O ., Davies , J ., Rousselot , P ., Barrera , L ., Birkle , K .,Meech , K ., Ortiz , J . Sekiguchi , T., Watanabe , J .-I .,Thomas , N ., and West , R .: 2003 , Exploring the icy
world of the Edgeworth -Kuiper Belt ‑ an ESO Large
Programme , The Messenger , 111, 22 ‑28.
Boehnhardt , H ., Delsanti , A ., Hainaut , O ., Barucci , A .,Romon , J ., Peixinho , N ., de Bergh , C ., Doressoundir am , A ., Dotto , E ., Lazzarin , M ., Tozzi , G . P ., Davies ,J ., Barrera , L ., Birkle , K ., Meech , K ., Ortiz , J . L .,Rousselot , P ., Sekiguchi , T., Watanabe , J ., Thomas ,N ., and West , R . M .: 2002 , The ESO Large Programon physical studies of TNOs and Centaurs , Proc .
Asteroids , Comets , Meteors ‑ ACM 2002 , ESA SP -500,
47 ‑50.
Bundy , K ., Fukugita , M ., Ellis , R ., Conselice , C .,Kodama , T., Brinchmann , J .: 2002 , The Stellar Mass
Assembly of Galaxies at z ＝1 ― New Results from
Subaru , American Astronomical
Society Meeting 201,
52.15.
Byun , D .-Y ., Koo , B .-C ., Tatematsu , K ., and Sunada , K .:2002 , Interaction
between the Supernova Remnant
HB21 and Molecular
Clouds , Proc . of the IAU 8th
Asian -Pacific Regional Meeting , 2, 131 ‑132.
Delsanti , A ., Boehnhardt , H ., Hainaut , O ., Barucci , A .,Doressoundiram , A ., Barrera , L ., de Bergh , C ., Birkle ,K ., Dotto , E ., Lazzarin , M ., Meech , K ., Ortiz , J .,Romon , J ., Sekiguchi , T., Thomas , N ., Tozzi , G . P .,Watanabe , J ., and West , R .: 2002 , PhotometryofKuiper Belt objects with the ESO Large Program ,Proc . Asteroids , Comets , Meteors ‑ACM 2002 ., ESA
SP -500, 25 ‑28.
Dermawan , B ., Nakamura , T., Yoshida , F ., Sato , Y .:2002 , Search for fast -rotators among the main -belt
asteroids , Bull . AAS , 34, 3, 14.09.
Dermawan , B ., Nakamura , T., Yoshida , F ., Sato , Y .:2002 , Search for fast -rotators among the main -belt
asteroids , Proc . of the 35
ISAS Lunar and Plane tary Conf , 146 ‑149.

Dobashi , K ., Uehara , H ., Kandori , R ., Umemoto , T.,
and Sato , F .: 2002 , A Catalogue of Dark Clouds Using
the Digitized Sky Survey I , Proc . of the IAU 8th
Asian -Pacific Regional Meeting , 2, 67 ‑68.
Ebizuka , N ., Oka , K ., Yamada , A ., Watanabe , M ., Shim izu , K ., Kotate , K ., Kawabata , M ., Teranishi , T .,Kawabata , K . S ., and Iye , M .: 2003 , Development ofVolume Phase Holographic(VPH ) Grism for Visible
to Near Infrared Instrumentsof the 8.2m Subaru
Telescope , Proc . SPIE , 4842 , 319 ‑328.
Ezawa , H .: 2002 , The Atacama Submillimeter
Tele scope Experiment (ASTE ) and Observationsof Gal axy Clusters with Submillimeter
Waves , Proc . of theworkshop “Tracing cosmic evolution with galaxy clus ters ”, eds . S . Borgani , M . Mezzetti , and R . Valdarnini ,ASP Conf . Ser ., 268, 357 ‑360.
Fleishman , G . D ., Melnikov , V . F ., and Shibasaki , K .:2002 , Observational
Constraints on Short -wave turbu lence in Flares , Proc . of 10th European Solar Physics
Meeting , Solar Variability : from Core to Outer Fron tiers , ESA SP -506, 283 ‑286.
Fujita , Y ., Sarazin , C . L ., Nagashima , M ., and Yano ,Y .: 2002 , Analytical Approach to the Mass Distribu tion Function of Subhalos and Cold Fronts in Galaxy
Clusters , The Proc . of the IAU 8
Asian -PacificRegional Meeting , Volume II , ASP Conf . Ser ., 289, 249‑250.
Fujita , Y .: 2003 , The Age and Number of Galaxies in
Clusters : Are Galaxy Groups Unvirialized
GalaxyClusters ?, Carnegie Observatories Astrophysics Series ,3. (published on the Internet )Furuya , R . S ., Kitamura , Y ., Wootten , A ., Claussen , M .
J ., and Kawabe , R .: 2002 , Imaging of 2 ‑mm Dust
Continuum Emission Towards S106 FIR and Its Spec tral Energy Distribution , Proc . of the IAU Symp . 206,
Cosmic MASERs : From Protostars to Blackholes , eds .
V . Migenes and M . J . Reid , 22 ‑25.
Furuya , R . S ., Kitamura , Y ., Wootten , A ., Claussen , M .
J ., and Kawabe , R .: 2002 , Multi -Epoch Water Maser
Survey Towards Low -Mass YSOs , Proc . of the IAU
Symp . 206, “Cosmic MASERs : From Protostars toBlackholes ”, eds . V . Migenes and M . J . Reid , 35 ‑38.
Gaessler , W ., Takami , H ., Takato , N ., Hayano , Y .,Kamata , Y ., Iye , M .: 2003 , Software and algorithms
of Subaru AO , Proc . SPIE , 4839 , 954 ‑963.
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 ,Adaptive Optics Systems and Technology II , eds . R . K .
Tyson , D . Bonaccini , M . C . Roggemann , Proc . SPIE ,4494 , 30 ‑40.
Gopalswamy , N ., Shimojo , M ., Yashiro , S ., andShibasaki , K .: 2002 , Prominence Eruptions and CMEs :A Statistical
Study , American Astronomical
Society
Meeting , 200, # 37.05.
Goto , M ., Hayano , Y ., Kobayashi , N ., Terada , H .,Pyo , T.-S ., Tokunaga , A . T ., Takami , H ., Takato ,N ., Minowa , Y ., Gaessler , W ., Iye , M .: 2003 ,Spectroscopy with Adaptive Optics : Spectroral Slope65

Variations , Proc . SPIE , 4839 , 1117 ‑1123 .
Goto , T ., Okamura , S ., Yagi , M ., and SDSS Collabora tion : 2002 , Morphological
Butcher -Oemler
effectbased on the SDSS Cut & Enhance Galaxy Cluster
Catalog , American Astronomical Society Meeting , 201,
# 148.02.
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Based on the Magnetic Reconnection Model , Proc . of
the IAU 8th Asian -Pacific Regional Meeting , 2, 473‑474.
Yoon , T . S ., Yoo , K . H ., Kim , K . M ., Kang , Y . H ., Kim ,J . H ., Lee , O . K ., Lee , J . A ., Kim , S . H ., Son , D . H .,Izumiura , H ., and Tamura , S .: 2002 , Spectroscopic
and PhotometricObservations of Symbiotic Stars inSouth Korea and Japan , Proc . of the IAU 8th Asian Pacific Regional Meeting , 2, eds . S . Ikeuchi , J . Hearn shaw , and T . Hanawa , 475 ‑475.
Yoshida , M ., Shimizu , Y ., Watanabe , E ., Yanagisawa ,K ., and Uraguchi , F .: 2002 , New Control Software of
the 188cm Telescopeof Okayama
AstrophysicalObservatory , Proc . SPIE , 4848 , 425 ‑433.
Yoshizawa , M ., Sato , K ., Nishikawa , J ., Ohishi , N .,and , Kotani , T .: 2002 , Large stellar interferometer

MIRA -ST , Proc . SPIE , Interferometry
Astronomy II , 4838 , 1282 ‑1289 .

forOptical5. Presentations
Abe , S ., Yano , H ., Ebizuka , N ., Kasuga , T ., Watanabe ,J ., Ogasawara , R ., and Fuse , T.: 2002 , First detectionof OH emission from meteor spectrum , 03 ‑25 poster ,Asteroids , Comets , Meteors ‑ ACM 2002 , (Germany ,July 29 ‑Aug . 2).
Abe , S ., Yano , H ., Ebizuka , N ., Kasuga , T ., Watanabe ,J ., Ogasawara , R ., and Fuse , T.: 2002 , UV video
spectroscopy of Leonid fireballs and persistent trains ,International
Science
Symposiumon the Leonid
Meteor Storms , (Tokyo , May 2 ‑5).
Arai , K ., and the TAMA
collaboration : 2002 ,TAMA300 : Status
Report , Gravitational
Wave
Advanced Detector Workshop
2002 , (Italy , May 20‑25).
Arimoto , N .: 2002 , Star Formation
Historiesof Gal axies derived from the Hess Diagram , Euro Confer ence Kiel 2002 , The Evolution of Galaxies III . From
Simple Approach to Self -Consistent
Models , (Kiel ,Germany , Jul . 16 ‑20).
Barucci , M . A ., Boehnhardt , H ., de Bergh , C ., Dotto , E .,Doressoundiram , A ., Lazzarin , M ., Romon ,J ., Tozzi ,G . P ., Fornasier , S ., Barrera , L ., Birkle , K ., Delsanti ,A ., Hainaut , O ., Meech , K ., Ortiz , J . L ., Sekiguchi , T.,
Thomas , N ., Watanabe , J ., and West , R . M .: 2002 ,Visible and Infrared spectroscopy of the Centaurs andTNOs from ESO Large Program , 01 ‑06 oral , Aster oids , Comets , Meteors ‑ ACM 2002 , (Germany , July 29‑Aug . 2).
Barucci , M . A ., Boehnhardt , H ., Dotto , E ., Lazzarin , M .,Romon , J ., de Bergh , C ., Doressoundiram , A ., Tozzi ,G . P ., Fornasier , S ., Davies , J ., Peixinho , N ., Barrera ,L ., Birkle , K ., Delsanti , A ., Hainaut , O ., Meech , K .,Ortiz , J . L ., Sekiguchi , T., Thomas , N ., Watanabe , J .,and West , R . M .: 2002 , # 07.07, ESO Large Program :Results from Visible and Infrared spectroscopyofCentaurs and TNOs , American Astronomical
Society ,34th DPS meeting , (U .S .A ., Oct . 6 ‑11).
Famiano , M . A ., Boyd , R . N ., and Kajino , T.: 2002 , Light
Element Nucleosynthesis
From Jet -Cloud Interactionsin Active Galactic Nuclei , The 7th Int . Symp . on
Nuclei in the Cosmos , (Japan , Jul . 7 ‑12).
Fujii , T., Nakada , Y .: 2002 , Near -Infrared Monitoring tostudy the Transition from AGB to Post -AGB Stars ,Mass -losing Pulsating Stars and their Circumstellar
Matter , (Sendai , May 13 ‑16).
Fujita , Y ., Sarazin , C . L ., Kempner , J . C ., Rudnick , L .,Slee , O . B ., Roy , A . L ., Andernach H ., and Ehle , M .:2002 , Chandra Observationsof the Disruption of theCool Core in Abell 133, Matter and Energy in Clustersof Galaxies , (Taiwan , Apr . 23 ‑27).
Fujita , Y ., Sarazin , C . L ., Nagashima , M ., and Yano ,Y .: 2002 , Analytical Approach to the Mass Distribu tion Function of Subhalos and Cold Fronts in Galaxy
Clusters , IAU 8th Asian -Pacific Regional Meeting ,73

(Tokyo , Jul . 2 ‑5).
Fujita , Y ., Takizawa , M ., and Sarazin , C . L .: 2002 ,Nonthermal Emissions from Particles Accelerated by
Turbulence in Clusters of Galaxies , XXI Texas Symp .
on Relativistic
Astrophysics , (Florence , Italy , Dec . 9‑13).
Fujita , Y .: 2003 , The Age and Number of Galaxies in
Clusters : Are Galaxy Groups Unvirialized
GalaxyClusters ? Probes of Cosmological
Structure and Gal axy Evolution , (Pasadena , U .S .A ., Jan . 27 ‑31).
Gouda , N ., Tsujimoto , T., Kobayashi , Y ., Nakajima ,T., Yasuda , N ., Kan -ya , Y ., Matsuhara , H ., Yano , T .,Yamada , Y ., and Ueno , M .: 2002 , IR Space
Astrometry , Mass -Losing Pulsating Stars and their
Circumstellar
Matter , (Sendai , May 13 ‑16).
Hachisuka , K ., Miyoshi , M .: 2002 , Phase Reference
VLBI Astrometry for Mira -Type Stars , Mass -losing
Pulsating Stars and their Circumstellar
Matter , (Sen dai , May 13 ‑16).
Hamane , T ., Yano , H ., Yoshida , M ., and Watanabe , J .:2002 , Gas -to -dust ratio and chemical composition
incomet
55P /Tempel -Tuttle , International
Science
Symposium on the Leonid Meteor Storms , (Tokyo ,May 2 ‑5).
Hasegawa , H ., Sekiguchi , T., Ukita , N ., Sunada , K .,Matsuo , H ., Kawakita , H ., and Watanabe , J .: 2002 ,Radio Observations of Comets using NRO 45m , Solar
System Science , Satellite
Meeting IAU 8th Asian Pasific Regional Meeting , (Tokyo , July 6).
Heki , K .: 2002 , Seasonal crustal deformation in Japan ,revisited , AGU Fall Meeting , (San Francisco , Dec . 6‑10).
Heki , K .: 2002 , Secular , transient and periodic crustal
deformation
observed in the Japanese nationwide
GPS array , Weikko
A . Heiskanen
SymposiuminGeodesy , (Ohio State University , Columbus , Oct . 1 ‑4).
Heki , K .: 2002 , Secular , transient and periodic crustal
movements
in Japanese
subduction
Zones , anddynamics underlying them . The Seismogenic
Zone
Experiment
Revisited (SEIZE2003 ), (Snowbird , Mar .
16 ‑20).
Honda , M ., Yamashita , T., Kataza , H ., Miyata , T .,Okamoto , Y . K ., Sako , S ., Takubo , S ., Onaka , T .:2002 , Mid -infrared Spectroscopic
Observations of Old
CTTSs , Chemistry as a Diagnostic of Star Formation ,(Canada , Aug . 21 ‑23).
Honda , S ., Aoki , W ., Ando , H ., Kajino , T.: 2002 , New
Detections of r-Process Elements in Extremely Metal Poor Stars with Subaru /HDS , Nuclei in the Cosmos
VII , (Fujiyoshida , Jul . 8 ‑12).
Ichiki , K ., Yahiro , M ., Kajino , T., Orito , M ., andMathews , G . J .: 2002 , Constraints on Dark Radiationin Brane Cosmology , The 7th Int . Symp . on Nuclei in
the Cosmos , (Japan , Jul . 7 ‑12).
Ichiki , K ., Yahiro , M ., Kajino , T., Orito , M ., andMathews , G . J .: 2002 , Constraints
on the nature ofcosmologicalconstant : from Big -Bang Nucleosynth esis and CMB anisotropies , The 7th Int . Symp . on
Nuclei in the Cosmos , (Japan , Jul . 7 ‑12).
74

Imai , H ., Deguchi , S ., Nakashima , J ., Miyazaki , A .,Kameya , O ., Fujii , T., Ita , Y ., Nakada , Y ., Izumiura ,H ., Glass , L . S .: 2002 , SiO Maser Survey towards theStellar Cluster at the Galactic Center , Mass -Losing
Pulsating Stars and their Circumstellar
Matter , (Sen dai , May 13 ‑16).
Imanishi , M .: 2002 , 3 ‑4 Micron Spectroscopy of Seyfert
2 Nuclei to Quantitatively
Assess the Energetic
Importance of Compact Nuclear Starbursts , IAU 8th
Asian -Pacific Regional Meeting , (Japan , Jul . 2 ‑5).
Imanishi , M .: 2002 , 3 ‑4 Micron Spectroscopy of Seyfert
2 Nuclei , Active Galactic Nuclei : from Central Engine
to Host Galaxy , (France , Jul . 23 ‑27).
Imanishi , M .: 2002 , Buried AGNs in LINER -TypeULIRGs , Active Galactic Nuclei : from Central Engine
to Host Galaxy , (France , Jul . 23 ‑27).
Inoue , S ., and Nagashima , M .: 2002 , Gamma -rays from
Large -Scale Shocks in the Universe , Int . Conf . “The
Universe Viewed in Gamma -Rays ”, (Kashiwa , Japan ,Sept . 26 ‑28).
Inoue , S ., and Nagashima , M .: 2002 , Merger Shocks andNonthermal Emission From Clusters : A Semi -analytic
Approach , Internal Conf . on “Matter and Energy in
Clusters of Galaxies ”, (Taipei , Apr . 25).
Inoue , S ., and Suzuki , T. K .: 2002 , Cosmic Ray Produc tion of Li by Structure Formation Shocks in the Early
Galaxy , Int . Conf . “Nuclei in the Cosmos VII ”, (Fuji Yoshida , Japan , Jul . 8 ‑12).
Inoue , S ., Iwamoto , N ., Orito , M ., and Terasawa , M .:2002 , Nucleosynthesisof Light and Heavy Elements inFailedGamma -Ray Burst
Fireballs , Int . Conf .
“Gamma -ray Bursts in the Afterglow Era : 3rd Work shop ”, (Rome , Italy , Sept . 17 ‑20).
Inoue , S .: 2003 , High Energy Particles
from Inter galactic
Shocks , Int . Symp . “Toward Very HighEnergy Particle Astronomy ”, (Kashiwa , Japan , Mar .
19 ‑21).
Ishiguro , M ., Watanabe , J ., Usui , F ., Tanigawa , T ., andMukai , T .: 2002 , First Detection of an Optical Dust
Trail along the Orbit of 22P /Kopff , 07 ‑35 poster ,Asteroids , Comets , Meteors ‑ ACM 2002 , (Germany ,July 29 ‑Aug . 2).
Ishikawa , K ., Ozawa , T ., Yadoumaru , Y ., Kinoshita , S .,and Watanabe , J .: 2002 , Leonids ʼmovie taken with anelectric -cooled color CCD camera , International
Sci ence Symposiumon the Leonid Meteor
Storms ,(Tokyo , May 2 ‑5).
Iwamoto , N ., Mathews , G . J ., Fujimoto , M . Y ., Kajino ,T., and Aoki , W .: 2002 , A new model for s-process
nucleosynthesis
in low -mass , low -metallicity
AGB
stars , The 7th Int . Symp . on Nuclei in the Cosmos ,(Japan , Jul . 7 ‑12).
Izumiura , H .: 2002 , Violet Spectra of Carbon Stars
Associated with Silicate Features , Mass -Losing Pul sating Stars and Their Circumstellar
Matter , (Sendai ,Japan , May 13 ‑16).
Izumiura , H .: 2003 , A White Dwarf Companion to the
Silicate Carbon Star BM Gem , International
Sympo sium on New Trends of Physics , Part2 , (Sapporo ,Japan , Mar . 17 ‑19).
Ji , J ., Liu , L ., Li , G ., Kinoshita , H ., and Nakai , H .: 2002 ,Stability Mechanism of the HD 82943 Planetary Sys tem , IAU Colloq . 189, (Nanjin ).
Kajino , T., Ichiki , K ., Orito , M ., Yahiro , M ., Otsuki ,K ., Mathews , G . J ., and Wanajo , S .: 2002 , Recent
Progress in Cosmology
and Nuclear Astrophysics ,XVI Particle and Nuclei Int . Conf ., (Japan , Sept . 30
‑Oct . 4).
Kajino , T.: 2002 , New Paradigms
in Primordial
Nu cleosynthesis : Implicationsin CMB , GW , and Brane
Cosmology , INT -02 ‑1 Nucleosynthesis
Program ,(USA , Mar . 25 ‑Jun . 28).
Kajino , T.: 2002 , Quest for supernova r-process : Newdata in astronomy and nuclear physics , and theoreti cal modeling , The 7th Int . Symp . on Nuclei in the
Cosmos , (Japan , Jul . 7 ‑12).
Kajino , T.: 2002 , Ultra -High Energy Neutrinos
from
Cosmic Sites , Int . Collaboration
Meeting on the Obser vatory for Multi Flavour Neutrinos from Supernovae ,(U .S .A ., May 23 ‑24).
Kameya , O .: 2002 , Mizusawa 10m Antenna System forStudy of Pulsating Stars , Symp . on Mass -losing Pul sating Stars and their Circumstellar
Matter -Newest
Results of Observations and Theory -, (Sendai , Japan ,May 13 ‑16).
Kasuga , T ., Ebizuka , N ., Abe , S ., Yano , H ., Fujiwara ,A ., Watanabe , J ., and Yamamoto , T .: 2002 , Highdefinition TV spectra of 1999 ‑2001 Leonids in Vis -UV
region , International
Science
Symposiumon theLeonid Meteor Storms , (Tokyo , May 2 ‑5).
Kawabata , K ., Tanikawa , K ., and Soma , M .: 2002 ,TT −UT in the 7th century derived from astronomi cal records in the Nihongi and the Suishu , Astronomi cal Instruments and Archives from the Asia -PacificRegion , (Cheongju , Korea , July 2 ‑5).
Kawakita , H ., and Watanabe , J .: 2002 , Ortho -to -para
Ratio of Cometary Ammonia in Comet Hale -Bopp :What is indicated by Ortho -to -para ratio of Cometary
Molecules ?, B1 .1 ‑0043 ‑02 poster The World Space
Congress , 34 ‑th Scientific Assembly of the Committeeon Space Research (COSPAR ), (U .S .A ., Oct . 10 ‑19).
Kawakita , H ., and Watanabe , J .: 2002 , Revised gfactors of Cometary NH : Ammonia abundances in
Comets , 21 ‑04 oral , Asteroids , Comets , Meteors ‑ACM 2002 , (Germany , July 29 ‑Aug . 2).
Kawakita , H ., and Watanabe , J .: 2002 , Unidentified
Molecular Bands in Comet Ikeya -Zhang (C /2002 C1 ),21 ‑18 poster , Asteroids , Comets , Meteors ‑ ACM 2002 ,(Germany , July 29 ‑Aug . 2).
Kawakita , H ., Watanabe , J ., and Fuse , T.: 2002 , Ortho to -Para Ratio of Cometary Ammonia , Solar System
Science , Satellite
Meeting
IAU 8th Asian -Pasific
Regional Meeting , (Tokyo , July 6).
Kawamura , S .: 2002 , Bridging the Gap between Terres trial
Detectors
and LISA , Gravitational
Wave
Advanced Detector Workshop , (Italy , May 19 ‑26).
Kawamura , S .: 2002 , Deci -hertz Interferometer
Gravita tional Wave Observatory(DECIGO ), 7th Gravita -tional Wave Data Analysis Workshop , (Kyoto , Japan ,Dec . 17 ‑19).
Kawamura , S .: 2002 , Resonant Sideband Extraction(RSE ) with the Third Harmonic Demodulation , Gravi tational Wave Advanced Detector Workshop , (Italy ,May 19 ‑26).
Kawamura , S .: 2002 , Status and Plans for Future Gener ations of Ground -based Interferometric
Gravitational Wave Antennas , 4th International
LISA Symposium ,(U .S .A ., Jul . 19 ‑24).
Kawamura , S .: 2003 , DECIGO ‑Japanese Space Gravita tional Wave Detector , International
Workshopon
GPS Meteorology , (Japan , Jan . 14 ‑17).
Kinoshita , D ., Yamamoto , N ., Watanabe , J ., Fuse , T.,
Ida , S ., and Nagasawa , M .: 2002 , Wide -Field Survey
near the Ecliptic with Subaru Telescope , Solar Sys tem Science , Satellite Meeting of the International
Solar System Science , Satellite
Meeting
IAU 8thAsian -Pasific Regional Meeting , (Tokyo , July 6).
Kodama , T.: 2002 , Large Scale Environmental
Effects in
Clusters of Galaxies , Int . conf . on Matter and Energy
in Clusters of Galaxies , (Taipei , Apr . 25).
Komiyama , Y .: 2002 , Wide -Field Imaging Survey of theDwarf Irregular Galaxy NGC6822 , Lowell Workshop :The Outer Edges of Dwarf Irregular Galaxies , (U .S .
A ., Oct . 10 ‑11).
Koyama , H ., and Inutsuka , S .: 2002 , A MechanismofEnergy Supply to Interstellar
Turbulence , Star For mation Workshop , (Taiwan , Jun . 12 ‑17).
Koyama , H ., and Inutsuka , S .: 2002 , Production
andDissipation
Mechanisms
of Interstellar
Turbulence
Driven by Thermal
Instability , IAU Symposium ,(Tokyo , Jul . 2 ‑5).
Kurayama , T., Sasao , T.: 2002 , Annual Parallax Mea surementsof Mira -Type Variables
with Phase Reference VLBI Observation , Mass -Losing Pulsating
Stars and their Circumstellar
Matter , (Sendai , May 13‑16).
Machida , M ., Tomisaka , K ., Matsumoto , T .: 2003 ,Binary Star Formationand Mass Outflow in the
Molecular Cloud Core ‑ MHD Nested Grid Simulation‑, The Eighth Int . Symp . on Simulation , (Hayama ,Mar . 5).
Machida , M ., Tomisaka , K ., Matsumoto , T .: 2002 ,Nonaxisymetric
Evolution of Cloud Cores and Mass
Outflows −MHD Nested Grid Simulation −, The Int .
Astronomical
Union 8th Asian -Pacific Regional Meet ing , (Tokyo , July 2).
Machida , M ., Tomisaka , K ., Matsumoto , T .: 2003 ,Binary Star Formationand Mass Outflows ‑MHD
Nested Grid Simulations ‑, IAU Colloq . 191, The envi ronment and evolution of double and multiple stars ,(Mexico , Feb . 3).
Machida , M ., Tomisaka , K ., Matsumoto , T .: 2003 ,Non -axisymmetricevolution of molecular cloud coreand fragmentation
condition , Int . Symp . on New
Trend of Physics , Part II , (Hokkaido , Mar . 18).
Miyoshi , M .: 2002 , VLBA Observation of the v ＝1 andSiO J ＝1 ‑0 Maser Emissions
in VY CMa , Mass 75

Losing Pulsating Stars and their Circumstellar
Mat ter , (Sendai , May 13 ‑16).
Mobasher , B ., Bridges , T . J ., Carter , D ., Poggianti , B .
M ., Komiyama , Y ., Kashikawa , N ., Doi , M ., Iye , M .,Sekiguchi , M ., and 3 authors : 2002 , Galaxies in the
Coma Cluster . V . Dependence of the Spectroscopic
Properties on Location in the Cluster yCat , 21370279 .
Mochizuki , N ., Miyoshi , M .: 2002 , A Comparison of the
SiO Masers in Orion KL with Those of Late -Type
Stars , Mass -Losing Pulsating Stars and their Circum stellar Matter (Sendai , May 13 ‑16).
Nagataki , S .: 2002 , Gamma -ray burst neutrino back ground and star formation history in the universe ,The 7th Int . Symp . on Nuclei in the Cosmos , (Fuji Yoshida , Japan , July 9).
Nakajima , T., Tsuji , T., and Yanagisawa , K .: 2002 , H and K -Band Methane Features in an L Dwarf , 2MASS
0920 ＋35, “Brown Dwarf ”, IAU Symp . 211, (Kona , U .
S .A ., May ).
Nakamura , T ., Watanabe , J ., Tsuda , T ., and Sato , T .,PSMOS /Japan group : 2002 , Observationof Leonid
meteor shower and middle /upper atmosphere with the
MU radar , International
Science Symposium on the
Leonid Meteor Storms , (Tokyo , May 2 ‑5).
Nakamura , T.: 2002 , Global survey project of Japanesematerials relating to astronomy and land -surveying
made before the Meiji -era , European AssociationofJapanese resource specialists conference , (Paris , Sept .
25 ‑28).
Nakamura , T.: 2002 , Japanese heraldic marks relating
to astronomy , International Conference on Astronom ical Instruments and Archives from the Asia -PacificRegion , IAU /IUSPH , (Chengju , Korea , Jul . 2 ‑5).
Ohishi , M ., Nakajima , J ., and Tokumaru , M .: 2003 ,Sharing Studies Between the Radio Astronomy Tele scopes and the Power Line Communication
Systems inthe HF Region , International
Symposium on PowerLine Communications , (Kyoto , Mar . 28).
Ohishi , M .: 2003 , An Application for the Data Grid : A
Prototype of the Japanese Virtual Observatory Sys tem , Global Grid Forum 7, (Tokyo , Mar . 7).
Ohishi , M .: 2003 , An Application for the Data Grid : A
Prototype of the Japanese Virtual Observatory Sys tem , PRAGMA
3, (Fukuoka , Jan . 24).
Ohnishi , K ., Ishikawa , T ., Hattori , S ., Maegawa , K .,Watanabe , J ., and Nakamura , T .: 2002 , Leonid 2001
flux by radio observation using a beam antenna , Inter national Science Symposium on the Leonid Meteor
Storms , (Tokyo , May 2 ‑5).
Ohnishi , K ., Yanagisawa , T ., Torii , K ., Kohama , M .,Hatsukade , Y ., Chaya , M ., Shibata , H ., Kawai , N .,Sato , R ., Nishiura , S ., Miyata , T ., Nakata , Y ., Doba shi , K ., Watanabe , J ., Agata , H ., Koike , K ., Usui , F .,Ishiguro , M ., Eiraku , M ., Mitikami , T ., Sugawara , A .,Uehara , A ., Takano , T ., Yoshikawa , M ., Abe , S ., andAsher , D .: 2002 , RadiantObservation
Project ofLeonid 2001 , International
Science Symposium on the
Leonid Meteor Storms , (Tokyo , May 2 ‑5).
Okamoto , T ., and Nagashima , M .: 2002 , Morphological76

evolution of cluster galaxies , Galaxy evolution : The ory and Observations , RevMexAA , (Cozumel , Apr . 8‑12).
Otsuki , K ., Kajino , T., Mathews , G . J ., Honda , S ., andAoki , W .: 2002 , Nuclear
Cosmochronometry
andUniversality
in the r-process , XVI Particle and Nu cleii Int . Conf ., (Japan , Sept . 30 ‑Oct . 4).
Otsuki , K ., Mathews , G . J ., and Kajino , T.: 2002 ,Nuclear cosmochronometerand universality
in ther-process abundance distribution , The 7th Int . Symp .
on Nuclei in the Cosmos , (Japan , Jul . 7 ‑12).
Otsuki , K ., Mathews , G . J ., Kajino , T., Aoki ,W .,Honda , S .: 2002 , Cosmochronology
and the Universal ity of r -process Abundances , AAS meeting 201, (U .S .
A ., Jan . 5 ‑9).
Otsuki , K ., Mathews , G . J .: 2002 , Cosmochronology
andUniversalityof r -process , APS /DNP2002 , (U .S .A .,Oct . 9 ‑12).
Otsuki , K .: 2002 , Cosmochronology
and the r -process ,INT -02 ‑1 Nucleosynthesis
Program , (U .S .A ., Mar . 25
‑ Jun . 28).
Otsuki , K .: 2002 , Cosmochronology
and the Universalityof the r -process , JINA Workshop02 , (U .S .A ., Oct . 6‑8).
Otsuki , K .: 2003 , Universality and the astrophysical site
for the r -process , Carnegie Observatories
Centennial
Symp . IV , (U .S .A ., Jan . 16 ‑21).
Peixinho , N ., Delsanti , A . C ., Boehnhardt , H ., Barucci ,M . A ., Barrera , L ., de Bergh , C ., Birkle , K ., Davies , J .,Doressoundiram , A ., Dotto , E ., Hainaut , O ., Lazzarin ,M ., Meech , K ., Ortiz , J . L ., Romon -Martin , J ., Rous selot , P ., Sekiguchi , T., Thomas , N ., Tozzi , G . P .,Watanabe , J ., and West , R .: 2002 , # 17.02, ESO Large
Program on TNOs and Centaurs : Visible -IR Results ,American Astronomical
Society , 34th DPS meeting ,(U .S .A ., Octo . 6 ‑11).
Ping , J ., Heki , K ., Matsumoto , K ., and Tamura , Y .:2002 , To estimate the high orders and degrees spheri cal harmonic function model for Lunar topography .
Int . Symp . on Geodesy , (Kanazawa , Oct . 28 ‑30).
Sakurai , T., and Hagino , M .: 2003 , Magnetic Helicity
and Its Solar -Cycle Variations , ʻ
The Workshop
onCurrent Issues in Solar and Space Physics ʼ, (Seoul ,Feb . 10 ‑12).
Sasao T., VERA Project Team : 2002 , AstrometryofMass -Losing Pulsating
Stars with VERA , Mass Losing Pulsating Stars and their Circumstellar
Mat ter , (Sendai , May 13 ‑16).
Sekiguchi , K ., Charles , P ., van Zyl , L ., Woodhouse , G .
F .: 2002 , High -speed imaging and spectro -polarimetry
with Subaru Telescope , IAU Col . 190: Magnetic Cata clysmic Variables , (Cape Town , S . Africa , Dec . 8 ‑13).
Sekiguchi , T., Hasegawa , H ., Sunada , K ., Ukita , N .,Kawakita , H ., Swamy , K . S . Krishna , and Watanabe ,J .: 2002 , HCN observations of C /Ikeya ‑ Zhang using
NRO 45m , 21 ‑20 poster , Asteroids , Comets , Meteors ‑ACM 2002 , (Germany , July 29 ‑Aug . 2).
Sekii , T.: 2003 , ChromosphericReflection
Layer forHigh -Frequency Acoustic Wave , ʻ
The First Far East -ern Workshop
on Helioseismology: Sounding theSolar Interior ʼ, (Seoul , Mar . 14 ‑16).
Shigeyama , T ., and Tsujimoto , T.: 2003 , A Merging
Scenario for Globular Cluster Formation ‑Inhibition
or Promotion of Self -Enrichment ‑, Globular Clusters :Formation , Evolution
and the Role of Compact
Objects , (Santa Barbara , Jan . 27 ‑31).
Shirasaki , Y ., Kawai , N ., Sakamoto , T ., Torii , K .,Tamagawa , T ., Yoshida , A ., Suzuki , M ., Matsuoka ,M ., Yamauchi , M ., Takagishi , K ., Hatsukade , I .,Fenimore , E . E ., Galassi , M ., Lamb , D . Q ., Graziani ,C ., Donaghy , T ., Vanderspek , R ., Ricker , G . R ., andHETE -2 Science Team : 2002 , In -orbit calibrationofthe HETE -2 WXM , Gamma Ray Bursts in the After glow Era ‑ Third Workshop , (Rome Italy , Sep . 17 ‑20).
Soma , M ., Tanikawa , K ., and Kawabata , K .-A : 2002 ,Earth ʼs rotation in the 7th century derived from
eclipse records in Japan and China , Proc . of JOUR NEES 2002 , Systemes de reference spatio -temporels ,Astrometry from Ground and from Space , (Bucharest ,Romania , Sept . 25 ‑28).
Sugano , T., and Heki , K .: 2002 , Lunar gravity studies
from the Lunar Prospector line -of -sight acceleration
data : isostatic compensation of medium sized craters ,AGU Fall Meeting , (San Francisco , Dec . 6 ‑10).
Sugano , T., and Heki , K .: 2002 , Lunar gravity studies
from the Lunar Prospector line -of -sight acceleration
data : isostatic compensation of medium sized craters ,Int . Symp . on Geodesy , (Kanazawa , Oct . 28 ‑29).
Sugiyama , N .: 2002 , From the Beginning to the End ,‑Towards
the Precision
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