COMMISSION J: RADIO ASTRONOMY
Edited by Inoue Makoto

J1 Introduction
Several new observing systems have been operational, particularly in Universities. We formallyparticipated in the ALMA project and began construction. A space mission is waiting for the launch
to the Moon, and the second Space VLBI project has been proposed. The organization system of
National Universities and Institutes was largely changed to agencies, and the effects are not yet
understood.
In J2, instrumentations and observing facilities of newly built or developed ones are shown,
followed by the progress of individual research fields in terms of scientific target: the Solar Radio
Astronomy in J3, and then starting from the Solar System in J4 to Quasars and Active Galactic Nuclei
in J6 by the order of distance from us.
J2 New Instrumentation
J2.1 ALMA
The National Astronomical Observatory of Japan (NAOJ) and the radio astronomy researchcommunity in Japan promoted the Atacama Large Millimeter/submillimeter Array (ALMA) project.
The construction project of the Japanese part of ALMA has started in 2004 April with an approval of
the funding.
Based on the resolution between the ALMA Coordination Committee (ACC) and NAOJ concerning
the Partnership for Planning the Atacama Large Millimeter/submillimeter Array (ALMA) signed on
2001 April by the European and North American delegates of ACC and the Director General of NAOJ,
NAOJ made a funding request for ALMA construction starting from FY2002. Although this initial
request was not successful in getting the construction fund, NAOJ was given a fund for FY2002 andFY2003 for the research and development of key technologies of large millimeter/submillimeter
arrays, i.e., precision reflector antennas, the millimeter/submillimeter receiver front-ends, andwide-band digital spectro-correlators. The European and North American partners successfullyacquired the construction funding starting from 2002, and the construction of ALMA was started witha bilateral agreement between them. In 2003 and 2004 NAOJ continued negotiation with theEuropean and North American partners for the participation in the ALMA construction. In March
2004 the Japanese construction fund starting from FY2004 was approved, and the Agreement
Concerning the Construction of the Enhanced Atacama Large Millimeter/submillimeter Array

(ALMA) was signed in 2004 September between the European Organization for Astronomical
Research in the Southern Hemisphere, the National Science Foundation of the United States and the
National Astronomical Observatory of Japan. The Japanese deliverables defined in the Agreement
included the Atacama Compact Array (ACA) system and three new receiver bands: the ACA system
consists of twelve 7-m antennas, four 12-m antennas and a dedicated ACA correlator, and will takeshort-baseline and total-power data to be combined with the data from the 64-element 12-m antenna
array built by the European and North American partners. Eighty receiver front-end cartridges foreach of the new receiver bands (Band 4: 125–163 GHz, Band 8: 385–500 GHz, Band 10: 787–950
GHz) will be built and integrated into the front-end subsystems at the Cassegrain foci of all ALMA
antennas, along with the four bands built by the European and North American partners.
NAOJ conducted the design and development of the ALMA antenna by building a prototype 12-m
antenna and evaluating it at the ALMA Test Facility (ATF) in Socorro, USA. The prototype antenna
met the major specifications that were verifiable at ATF, and the technical feasibility wasdemonstrated [Ukita et al. 2004].

The development of the receiver front-end was made as

collaboration among NAOJ, Osaka Prefecture University, Nagoya University, and Toyota National
College of Technology. It included design and development of wide-band sideband-separating SIS
mixers without mechanical tuners, prototyping of receiver cartridges for Band 4, 8, and 10 andfield-testing them, refinement of the cartridge concept of the cryostat, and design and production of
cartridge test cryostats [Andoh et al. 2003; Asayama et al. 2003a, 2003c, 2004; Ogawa et al. 2003;
Sekimoto et al. 2003a; Sugimoto et al. 2003a, 2003b; Yokogawa et al. 2003a]. A photonic scheme forthe local oscillator signal generation was developed, and a research on the photomixers was made as
collaboration between NAOJ and NTT [Ishiguro et al. 2002; Ito et al. 2002; Noguchi et al. 2001;
Sekimoto et al. 2003a; Ueda et al. 2003a, 2003b]. NAOJ built a single-baseline test FX correlator andevaluated its performance with an actual observation of the astronomical signal at Nobeyama,confirming the technical feasibility of large scale FFT processing [Okumura et al. 2002, 2003]. A
prototype A/D converter with 4 Gsps in 2 bits was developed and successfully evaluated [Okiura et al.
2002]. Numerical simulations were made to assess the importance of ACA in wide-field imaging by
ALMA and to identify the critical technical requirements that make ACA meaningful [Tsutsumi et al.
2004]. The characterization of the ALMA site was continued, and the methods to compensate theatmospheric phase fluctuation were studied [Matsushita et al. 2002; Sakamoto 2002b, 2003c, 2003d,
2004a, 2004b, 2004c; Watanabe 2004]. The organizational structure to manage the Japanese part ofthe construction project was developed in NAOJ in harmony with the “bilateral” management
structure. Computing was identified as one of the areas that require joint development by a unified
team with members from the three partners, and a plan was made for such a scheme. Astronomers in
China/Nanjin and China/Taipei expressed their interests in collaboration in construction and/or
operation of ALMA, and discussion started between NAOJ and their institutes. (T. Hasegawa)J2.2 NRO 45-m Telescope and NMA
The 45-m telescope of Nobeyama Radio Observatory (NRO), NAOJ, has been operated at afrequency range of 20-150 GHz. A 25-beam SIS receiver at 82-116 GHz, BEARS, and a 6-beam SIS
receiver at 40-50 GHz are available on the telescope. In addition, a bolometer array, seven beams with
30-GHz bandwidth at 150 GHz, is also available. New encoder system for the telescope is underconstruction. The Nobeyama Millimeter Array (NMA), which is composed of six 10-m antennas,
has been operated at 85-116, 126-152, and 220-240 GHz. The RAINBOW interferometer, whichconnects NMA and the 45-m telescope to make an array with large gain, has been provided for open
use. (M.Tsuboi)
J2.3 ASTE
The Atacama Submillimeter Telescope Experiment (ASTE) is a project to operate a 10-m
submillimeter telescope at a high altitude site (4,800 m) located in Atacama Desert in Northern Chile.
The project aims to explore the southern sky with a submillimeter region at 300-900 GHz, as well as tostudy and develop instruments or methods for submillimeter observations. The telescope wasshipped to Chile in 2002. Following the evaluation and testing phase including detection of CO(J=7-6) emission at 807 GHz, we have started the spectroscopic observations mainly at 345 GHz bandto detect various emission lines including CO(J=3-2) or CS(J=7-6) through numbers of astronomical
objects.
The 10-m antenna has an excellent performance with its surface accuracy adjusted within 19
microns rms, which is realized utilizing the motorized actuators supporting the 205 panels which
consists the surface of the main reflector. Several receivers were tested on board in early phase
operation in Chile: SIS receivers at 100 GHz to 800 GHz, and a bolometer system at 350 GHz to 850
GHz. These receivers provided the first chance to observe astronomical radio waves with 800 GHz
band at the Atacama site. Currently the SIS receiver at 345 GHz with cartridge type plug-in
cryogenics is in operation, which is presenting an excellent performance with system noise
temperature within 130 K to 200 K. The spectrometer is an array of 4 XF type digital auto-correlators,
each with spectral channels of 1024 and frequency resolution of 31.25 kHz. The bandwidth can beeither 512 MHz or 32 MHz for each auto-correlators which may cover 750 km/s at 810 GHz. The
control system is designed to enable operating the telescope remotely through the network connection.
The connections are via satellite link from the telescope site to San Pedro de Atacama (alt. 2400 m)
and Universidad de Chile in Santiago, with further connection to Japan through the internet. The
telescope site is powered by two sets of generators, as well as several safety equipments including
oxygen compressors and satellite phones. (H. Ezawa)J2.4 NANTEN 4-m Telescope of Nagoya U
The NANTEN telescope, a 4-m millimeter-submillimeter telescope, was installed at the Las
Campanas Observatory in Chile under a mutual agreement between Nagoya University and theCarnegie Institution of Washington. The observations were carried out mainly in the 12CO, 13CO,

and C18O (J=1-0) emissions at a beam size of 2.7 arcmin. The molecular cloud survey toward LMC
and SMC has been completed and resulted in a detection of ~260 Giant Molecular Clouds. The survey
toward the Galactic plane in 12CO almost covers 60° > l > 240°, -10° < b < 10° with grid spacings of
4 arcmin for |b| < 5° and of 8 arcmin for the rest. This resulted in a number of detections of Giant
Molecular Clouds (GMCs) as well as candidates for supershells along the galactic plane. Detailed
studies of interacting clouds with HII regions and/or SNRs are also carried out. The physicalproperties of the molecular gas toward GMCs, dark clouds, and high latitude clouds in the Galaxy arestudied. These results are described in a section of "Star Formation".
The NANTEN telescope had stopped its operation in October of 2003, and the upgrade forsub-millimeter observations started from the period [NANTEN2 project].

The telescope isinstalling at Pampa la Bola in Chile at an altitude of 4,800m to realize a large-scale survey at submm
wavelengths.

In this new project, we will make large-scale surveys toward the Galaxy and nearby

galaxies including the Magellanic Clouds by using mainly CO and [CI] lines in a 100-800 GHz
range.

The purpose is an elucidation of evolution of interstellar matter and the mechanism of starformation in the local group by revealing the distribution, kinematics, and physical conditions ofinterstellar gas in the atomic-molecular phases with the thorough extensive survey. This project iscollaboration between Universities in Japan (Nagoya University and Osaka Prefecture University),
Germany (University of Cologne and University of Bonn), South Korea (Seoul National University),
and Chile (University of Chile).

The telescope is enclosed in a dome with a shiftable membrane toprevent perturbations such as strong wind and sunlight.
2004.

The installation started at the beginning of

The highest observing frequencies will be covered by the KOSMA SMART receiver, adual-frequency, 2 x 8 pixel array receiver operating between 460 and 880 GHz, and KOSMA array
Acousto Optical Spectrometers as backends. (T. Onishi)
J2.5 Mt. Fuji Submillimeter Telescope
Mount Fuji submillimeter-wave telescope is operated by Yamamoto Group of Department of
Physics, The University of Tokyo, in collaboration with Nobeyama Radio Observatory. It is a 1.2-m
telescope enclosed in the space frame radome with GoreTex membrane, and is used exclusively forsurvey observations of the fine structure lines of the neutral carbon atom ([CI] 492 GHz and 809 GHz).
With this telescope, more than 40 square degree areas of nearby molecular clouds have been observedin the 492 GHz CI line, and several representative sources have been mapped in the 809 GHz CI line.
Among them, Kamegai et al. (2003) presented the large-scale CI (492 GHz) map toward rho-Ophiuchi
molecular cloud. The CI emission peak is found to exist behind dense cores with respect to theexcitation star (HD147889), suggesting that the peak is in the early stage of chemical evolution. Oka
et al. (2004), on the other hand, studied the CI (492 GHz) distribution in the NGC1333 region. Again
the CI peak is located behind dense cores with respect to the excitation stars. With the aid of chemical
model calculations, they showed that it is essentially important to consider the chemical evolutionary
effect in interpretation of the CI distribution.

Unfortunately, Mount Fuji submillimeter-wave telescope will be closed in August 2005. This isbecause the electricity supply from the meteorological weather station becomes unavailable due toshut down of the weather station. (S. Yamamoto)J2.6 The 60-cm Telescope of the U. Tokyo
The radio astronomy group at Institute of Astronomy in the University of Tokyo runs a 60-cm radio
telescope, called the Very Small Telescope 1 (VST1) located at Nobeyama with support of Nobeyama
Radio Observatory. The telescope is designed for survey observations of the Galactic plane andnearby molecular clouds in CO (J=2-1) and other lines near 230 GHz. The beam size of 9 arcmin
enables us to make direct comparison with the CO (J=1-0) line obtained using the 1.2-m telescope
operated by Harvard Smithsonian Center for Astrophysics, which gives density and temperature ofmolecular gas. To improve observation efficiency we have upgraded the telescope system since 2003
with cooperation of radio astronomy groups in Osaka Prefecture University and Tokyo Gakugei
University. The receiver has replaced to sideband separating receiver (2SB), which can simultaneous
observations in both side bands. Using the 2SB receiver we plan to make observations in both 12CO
and 13CO at once. For the dual IF signals obtained by the 2SB receiver, we have designed andinstalled two sets of 2048-channel Acousto-Optical Spectrometers (AOS) with a 250-MHz bandwidth.
The telescope controlling system has been revised from DOS based to Linux based. The new systemcalled UltraASTROS is improved for easy accessibility through the Internet and is designed to makeautomated observations. The new telescope system was performed the first engineering observationsin 2005. (T. Handa)
J2.7 Arrays of Waseda University
Transient radio source survey and EGRET Gamma-ray source identification program has been
started at Nasu Pulsar Observatory of Waseda University. A spherical dish array of 8 x 20-m
elements is operated at 1.4 GHz, covering between 32° to 42°. in Declination.

During earlyobservations, a large outburst was detected at April 20, 2000. (T. Daishido)
J2.8 VERA and VLBI Activities
J2.8.1 VLBI Networks
VLBI Exploration of Radio Astrometry (VERA) aims to determine the distance to celestial objects
in our Galaxy by measuring annual parallaxes and to investigate the structure of our Galaxy. VERA
consists of four 20-m radio telescopes around the Japanese Archipelago (at Mizusawa, Iriki,
Ogasawara, and Ishigakijima). VERA has a dual-beam observing system for the phase referencing
VLBI observations. VERA will observe around one thousand objects to make a three-dimensional
map of our Galaxy. The dynamic structure of our galaxy will be revealed by measuring the motionsof these objects. At 2004, VERA developed a central control system and became regular operation
phase.

The accuracy of astrometry has reached around 100 micro-arcsecond.

endeavored more accurate calibration procedures for the improvement of the accuracy.

VERA hasAt 2004, the new Japanese VLBI network was organized, which consists of 10 VLBI stations:
VERA 4 stations, Tomakomai 11-m telescope, Kashima 34-m telescope, Tsukuba 32-m telescope,
Usuda 64-m telescope, Gifu 11-m telescope and Yamaguchi 32-m telescope. Since December 2004,
observations were started at 8GHz, achieving the mapping dynamic range of 1500. So possibilities ofhigh dynamic range observations were demonstrated. Regularly it has been operated around 20 hours
per month.
At the 6th East Asian Astronomy Meeting held at Seoul in October 2004, East Asia VLBI
consortium was organized. It aims to organize the East Asia VLBI network, which consists of current
and constructed VLBI stations in China, Japan and Korea. Especially this area will have more thanfifteen VLBI stations within 2,000-km in diameter, the distribution of the network is the most dense in
the world. At 2004, Sheshan station of China was joined to Japanese VLBI network observations at
22 GHz and gave good fringes.
J2.8.2 VLBI Activities in Institutes and Universities
National Astronomical Observatory of Japan (NAOJ) has two projects related to VLBI activities.
One is the VERA project and the other is a Space VLBI project. NAOJ has 7 VLBI stations. Four ofthem are VERA stations and others are Nobeyama 45-m, Yamaguchi 32-m and Kagosima 6-m radio
telescopes. VERA project has been developing optical fiber link VLBI system. Tsukuba 32-m,
Kashima 34-m, Usuda 64-m and Gifu 11-m telescopes are combined with optical fiber links, whichmakes it possible to transmit data with 2-Gbps from each station. It is a unique operation VLBI arraywith optical fiber link in the world. A new Space VLBI project VSOP-2, next to HALCA/VSOP, hasbeen proposed to the Institute of Space and Astronautical Science (ISAS), collaborating with theSpace VLBI group in ISAS, and other groups.
National Institute of Information and Communication Technology (NICT) is operating 34-m and11-m radio telescopes at Kashima and another 11-m radio telescope at Koganei. They are mainly
used for geodetic and astronomical VLBI observations and pulsar timing observations. As one of theTechnical Development Centers of International VLBI Service for Geodesy and Astrometry (IVS),NICT has been developing Gbps-class VLBI observing systems to enhance the sensitivity of the VLBI
observations [Nakajima et al. 2001], and the K5 VLBI system to realize e-VLBI in real-time over theshared IP networks [Kondo et al. 2002; Koyama et al. 2002]. Software correlator programs which run
on multiple PC systems for distributed processing are under development as the correlator part of theK5 system. By using the K5 system, rapid turnaround estimation of UT1-UTC as short as 4.5 hours
was demonstrated in June 2004 with a baseline between Kashima and Westford (HaystackObservatory) VLBI stations [Koyama et al. 2003].

The K5 system is also being used forinvestigations about precise orbit determination of spacecrafts. Nozomi and Hayabusa spacecrafts
were observed by differential VLBI technique to improve the accuracy of the position of thesespacecrafts [Kondo et al. 2002]. Theoretical investigations to improve the VLBI measurements arealso carried out, such as ionospheric delay modeling [Sekido et al. 2003a] and relativistic VLBI delay
model for finite distance radio sources [Sekido et al. 2003b].
Geographical Survey Institute (GSI) has a VLBI network of Tuskuba 32-m, Shintotugawa 10-m,
Chichijima 10-m, and Aira 10-m radio telescopes. Japan domestic geodesy VLBI experiments arecarried out using them every month, which is called as JADE. Some other stations of other institutes
were joined in JADE to determine their positions. GSI carries out UT1 experiments between
Tsukuba, Wetzell in Germany, and/or Onsala more than 100 times per year. Tsukuba 32-m telescope
participates in the IVS observations regularly.
Institute of Space and Astronautical Science (ISAS) became a department of Japan Aeronoautical
Exploration Agency (JAXA). It carried out a space VLBI mission VSOP. Usuda 64-m antenna isused for the Japanese VLBI network observations.
determination system using VLBI technique.

ISAS has developed a satellite orbit

Kagoshima 34-m antenna was installed a VLBI

terminal system and is also used for the satellite navigation experiments.
Universities in Japan recently have their own radio telescopes and form optionally the Japanese
VLBI network with VERA and other telescopes in Institutes. Hokkaido University has an 11-m radio
telescope at Tomakomai, operated at 22 GHz. It is mainly used for the galactic plane survey by NH3
as a single dish. It has also a VLBI terminal system and joins to Japanese VLBI network observations.
Gifu University has an 11-m radio telescope at Gifu, operated at 2 and 8 GHz. It is mainly used forgeodetic VLBI experiments and e-VLBI experiments. Yamaguchi University cooperates in theoperation of Yamagauchi 32-m radio telescope with NAOJ. It is used as a station of Japanese VLBI
network.

The group of the Yamaguchi University has carried out methanol maser survey

observations as a single dish.

They discovered some new sources.

Kagoshima University

cooperates in the VERA project of NAOJ. Iriki station, one of four VERA stations, is operated by thegroup of Kagoshima University. (H. Kobayasgi)
J2.9 Space VLBI VSOPThe VLBI (Very Long Baseline Interferometry) Space Observatory Programme (VSOP) was
realized with the launch of the radio astronomy satellite HALCA by the Institute of Space andAstronautical Science (ISAS) in February 1997. HALCA exceeded its nominal five year lifetime,
conducting almost 800 observations at 1.6 and 5.0 GHz to study the compact cores and theparsec-scale jets of extragalactic radio sources and other objects. In addition to open General
Observing Time, observations were undertaken at 5 GHz for the VSOP Survey program, a mission-led
survey to study the statistical properties of the bright, flat-spectrum of active galactic nuclei, withresults for the first 102 sources published last year [Scott et al. 2004]. One of HALCA's four reaction
wheels stopped operating in October 1999, and a second has not been able to be restarted after a loss of
attitude control in October 2003. HALCA is being monitored during one tracking pass per week,with the VSOP team's efforts now being focused on improving access to the VSOP data archive, andon preparations for the submission of a proposal for a next generation mission, VSOP-2, which will
provide gains in sensitivity and angular resolution of an order of magnitude compared with VSOP. (P.G.
Edwards)
J2.10 Lunar exploration
Two radio-metric experiments are planned in Japanese SELENE (Selenological and Engineering
Explorer) mission. One is a 4-way Doppler experiment using a relay sub-satellite. The second is adifferential VLBI experiment with the two sub-satellites which transmit three carrier waves at S bandand one carrier wave at X band. Both experiments are to measure the precise lunar gravity field.
SELENE is scheduled to be launched in 2007. The PFM integration test has already begun in late
2004. The VLBI recording system was equipped to all of VERA antennas and to three stations in
China and Europe, except one for Germany. (N. Kawano)
J3 Solar Radio Astronomy
Nobeyama Radioheliograph (NoRH) is a radio interferometer dedicated for solar observations. It
has been operating since 1992 and has completed one solar cycle observation. Due to the uniform
date set of microwave full disk images of the Sun for one solar cycle or more, statistical studies of solar
activity over solar cycle can be done. On this occasion, an international symposium “Solar Physics
with Nobeyama Radioheliograph” was held on October 2004 to summarize science outputs from
NoRH and to discuss future researches.
High-cadence imaging capability (0.1 second) of NoRH made it possible to detect directly
high-energy electron streams along a large coronal loop. The electrons are accelerated or injected at
one of the footpoints of the large loop. The projected speed of the stream is one-third of the light
speed. Taking into account the gyration of electrons around magnetic field and the angle between theloop and the line-of-sight, actual speed of electrons is close to the light speed and this is consistent
with the fact that the steaming electrons generate microwave emission through gyro-synchrotron
mechanism [Yokoyama et al. 2002].
Properties of extended non-thermal flaring loops have been studied. These loops do not necessarily
associate with high-temperature and high-density plasma that emit soft X-rays. Microwaves are
emitted by interaction of high-energy electrons with magnetic field, hence, microwaves cover thewhole loop. They are clearly observed when the loops sizes are large enough to be resolved by thebeam of NoRH. Recent studies show that, many of these loops have brighter loop top compared toloop legs or footpoints [Melnikov et al. 2002a]. Gyro-synchrotron emission is known to be very
sensitive to magnetic field strength. Model calculations show that loop footpoints are brighter thanloop tops.

However, observations show opposite.

This is interpreted by large pitch angle

distribution of accelerated electrons. This is a very strong constraint to acceleration mechanism ofhigh-energy electrons in solar flares. Oscillations of flaring non-thermal loops were reported and theoscillation mode is identified [Melnikov et al. 2004, Stepanov et al. 2004]. Based on oscillations,diagnostic method of flaring loops has been developed.
After the launch of RHESSI (Ramaty High Energy Spectroscopic Imager) satellite in 2002, manystrong flares were observed simultaneously by RHESSI and NoRH. Some of the analysis of these
events are reported [Kundu et al. 2004, and White et al. 2003]. Due to hard X-ray and gamma-ray
spectroscopy of RHESSI together with imaging capability, studies of high-energy particle acceleration
will be greatly enhanced by combining with two-frequency imaging capability of NoRH. However,
the acceleration mechanisms are not yet conclusive. (K. Shibasaki)
J4 Solar System Radio Astronomy
Tohoku University has established a meter to decimeter wave range radio telescope, named IPRT
(Iitate Planetary Radio Telescope), in 2001 at Iitate, Fukushima, Japan. The antenna of the radio
telescope is a fully steerable offset-parabola type with the physical aperture area of 1023 m2, andcomposed of a pair of same-shaped parabolic rectangular sections (16.5 m x 31 m) installed on one
alt-azimuth mount. The radio telescope has been dedicated for exclusive and regular observation ofplanetary radio emissions to investigate electromagnetic environment of planets, particularly Jupiter’s
inner magnetosphere [Tsuchiya et al., 2002, Tsuchiya et al., 2003; Misawa et al., 2003].
Jovian synchrotron radiations (JSR) emitted from relativistic electrons trapped in the Jupiter'sradiation belt were observed during a rarely strong solar event on October 28 and 29, 2003 by
Tsuchiya et al. (2004). The observations were made by using IPRT at Iitate Observatory during theperiod from October 16 to November 20, 2003. They compared the variation of JSR intensity withthe solar F10.7 flux and found that JSR showed an unusual increase of its magnitude by about 50%
during the period of solar flux enhancement, and subsequent rapid decrease after the solar event withthe decay rate of about 0.3 Jy/day. (A. Morioka)
The interplanetary scintillation (IPS) method can observe the dynamics and structure of the solar
wind in three dimensions with a relatively short time cadence using IPS radio sources distributed overthe sky. Because of this advantage over in-situ measurements, the Solar-Terrestrial Environment
Laboratory (STEL) has been conducting the IPS observations at a frequency of 327 MHz using
four-station system.
To make solar wind observations with higher spatial and temporal resolution using the tomographic
method, the project to build a new large UHF antenna, Solar Wind Imaging Facility (SWIFT), hasbeen commenced. The antenna will have a collecting area of 40 m x 106 m which consists of two
cylindrical parabolic reflectors with 20 m width (EW) and 106 m length (NS).

The antenna isdesigned with a tolerance for radio noise interference and high aperture efficiency.

The SWIFT

will observe meridian-passage radio sources by changing direction of beam from S60 to N30.

A solar wind prediction experiment is being carried out under collaboration between CASS/UCSD
and STEL by using computer-assisted tomography (CAT) analysis.

In this experiment, speed anddensity variations in the near-earth solar wind are predicted from IPS measurements in quasi realtime via STEL and UCSD web servers (http://cassfos02.ucsd.edu/solar/forecast/index.html,
http://stesun5.stelab.nagoya-u.ac.jp/forecast/).
The elucidation of three-dimensional (3D) structure and propagation characteristics of coronal massejections (CME) is an important subject in solar weather research. In particular, our knowledge on the
3D properties of CMEs in the interplanetary space (i.e., beyond the field of view of the coronagraph) is
limited due to the shortage of global observations. We have been studying the 3D structure andpropagation characteristics of ICMEs, using IPS observations. However, there has been a difficulty
in investigating 3D properties of ICMEs precisely from IPS data because of line-of-sight (los)integration effects. Recently, we have developed the model fitting analysis method, which allows us
to remove the los integration effects and to retrieve the 3D structure of ICMEs from IPS data. Using
this revolutionary technique we have studied the structure and dynamics of ICMEs [Ananthakrishnan
et al., 2002; Tokumaru et al., 2003a, b; Yamashitaet al., 2003; Jackson et al., 2003; Kuwabara et al.,
2004; Tokumaru et al., 2005].
Various kinds of coronal holes produce various speed of solar wind and construct 3D structures ofthe solar wind. We have investigated the relation between solar wind velocity and physical propertiesof the corona holes. The relations among a solar wind velocity (V), coronal hole scale size, amagnetic flux expansion rate (f) and photospheric magnetic field (B) are examined, and the highest
correlation was found between V and B/f [Kojima et al., 2004b] and small coronal holes were found tobe sources of the slower solar wind [Ohmi et al., 2003a, b; Ohmi et al., 2004]. (M. Kojima)
J5 Galactic Radio Astronomy
J5.1 Galactic Center Region
The Nobeyama Radio Observatory 45-m telescope (RT45) Galactic Center CO survey indicated that
all the clouds in the GC are in equilibrium with high pressure in the GC environment (Oka et al.2001,
Oka and Hasegawa 2003). Mapping observations of SiO maser sources near the GC were made with
RT45 at 43 GHz, resulted over 200 detections of SiO sources (Deguchi et al. 2002, 2003 Imai etal.2003). The 7-years monitoring observations of Sagittarius A* at 100 and 140 GHz with Nobeyama
Millimeter Array (NMA) found intraday variation of Sgr A* (Miyazaki et al. 2004).

VLBA

observation revealed a radio intraday flare of Sgr A* at 43 GHz (Miyoshi et al. 2003). Aperturesynthesis observations of Sagittarius B2 Main in the FeO (J=5-4) line using NMA confirms thedetection of this line in absorption (Furuya et al. 2004). A comparison between CO and OH data
derived the molecular face-on view of the GC (Sawada et al.2003). Circular polarization of Sgr A*
with RT45 at 100 GHz was measured to be less than 0.5% (Tsuboi et al.2003). (M. Tsuboi)

J5.2 Star Forming Regions
A number of high-density molecular cores were observed in nearby low-mass star forming regions
in order to pursue the initial conditions of low-mass star formation. H13CO+ (J=1-0) observations in
Taurus gave us detailed information of dense cores just before star formation with a nearly complete
sample of 55 high density cores in the region [Onishi et al. 2002]. Physical properties of 179 C18O
cores were summarized [Tachihara et al. 2002], and 8 cores in Taurus were mapped in the line of
N2H+ (1-0) [Tatematsu et al. 2004] to investigate the evolutionary status of the dense cores. Several
molecular lines were used to investigate the chemical evolution of several pre-protostellar cores[Hirota e tal. 2003; Lee et al.2003; Hirota et al. 2004]. Coalescence processes of small clumps aresuggested to be likely to play an important role in forming protostars inside cores with a high spatial
resolution observation by using NMA toward two dense cores [Takakuwa et al. 2003].
Observational study of low-density gas revealed important features to constrain theoretical models
of molecular cloud formation. Large velocity dispersion in a small spatial scale of ~0.01 pc wasdetected toward high latitude clouds and a Taurus cloud, suggesting the structure formation ofmolecular clouds through thermal instability [Sakamoto 2002; Sakamoto and Sunada 2003]. A large
scale survey toward galactic high-latitue region detected a few hundred molecular clouds, and theevolutionary status was investigated by comparing molecular data with infrared and HI data [Onishi etal 2001; Yamamoto et al. 2003].
Ten massive star-forming regions were studied in the lines of 13CO, C18O(J=1-0) and CS(J=2-1)[Ao et al. 2004]. An interferometric and single-dish study of G24.78+0.08, a region associated withhigh-mass star formation, strengthened the proposed scenario star formation would occur frominside-out collapse of the parsec-scale clump, followed by infall reversal due to outflows powered by
the newly formed massive stars [Cesaroni et al. 2003]. Evolutional sequence of high-mass protostars
is studied though high angular resolution observations at millimeter wavelengths of the high-mass star
forming region G24.78+0.08 [Furuya et al. 2002]. Heads of two molecular pillars in the Eagle
Nebula were observed by using the Nobeyama Millimeter Array with a spatial resolution, andpropagation of star formation was suggested in the region [Fukuda et al. 2002].
NANTEN telescope has been revealing new views of molecular gas distribution of the southern sky.
The new sensitive survey of giant molecular clouds (GMCs) in the LMC tripled the number of the
GMCs from 55 to 168 [Fukui et al. 2001]. Catalog of GMCs in the LMC for the first survey waspresented [Mizuno et al. 2001] and the result of the GMC survey toward the SMC was presented[Mizuno et al. 2001]. The effect of supergiant shells on the formation of molecular clouds and stellar
clusters was studied [Yamaguchi et al. 2001] and the evolutional sequence of GMCs was elucidated byusing the NANTEN LMC data [Yamaguchi et al. 2001]. Eight molecular supershells were detectedfrom the NANTEN galactic plane survey [Matsunaga et al. 2001] and the effect of supernova tomolecular clouds were studied toward the Vela supernova remnant [Moriguchi et al. 2001]. The most
massive C18O molecular complex was found in Centaurus region [Saito et al. 2001], and a large scalestudy of H13CO+ and C18O (J=1-0) was carried out toward a GMC Orion B [Aoyama et al. 2001].
Star formation in IC 2218 in the Orion-Eridunus Bubble was investigate to reveal the effect of massive
stars to the star formation in it [Kun et al. 2001]. Large scale 12CO(J=1-0) surveys toward nearby
low-mass star forming regions were carried out toward Chamaeleon [Mizuno et al. 2001] and Lupus[Tachihara et al. 2001]. Molecular clouds at Galactic high-latitude were surveyed extensively toward
Aquila [Kawamura et al. 2001] and toward the infrared excess clouds [Onishi et al. 2001]. The
correlation between CO column density and extinction was investigated for molecular clouds in
Chamaeleon II-III complex.
CO molecular outflows are searched toward the cloud A and B2 of the Rho-Ophiuchi star-forming
region and all the newly discovered outflows are likely to be driven by Class II sources ornear-infrared sources, and none of them is associated with the cold submillimeter-millimeter sources
without infrared counter parts [Kamasaki et al. 2003]. High-resolution millimeter imaging was
carried out toward the R Coronae Australis IRS 7 region, and three compact objects located within 4"(700 AU) of IRS 7A [Choi and Tatematsu 2004]. Millimeter wavelength observations are presented
toward NGC 1333 IRAS 4, a group of highly embedded young stellar objects in Perseus, that reveal
motions of infall, outflow, rotation, and turbulence in the dense gas around its two brightest continuum
objects, 4A and 4B [Di Francesco et al. 2001]. Result of multiepoch 22 GHz H2O maser survey mainly
toward 142 low-mass young stellar objects using the Nobeyama 45 m telescope and the Very Large
Array was compiled together with their H2O maser activity [Furuya et al. 2003]. Molecular gas
toward the supernova remnant (SNR) W44 (G34.7-0.4) was extensively mapped in CO J=1-0
emission with the 17" beam of the Nobeyama 45 m radio telescope, detecting high-velocity (> 25 kms-1) CO line wings [Seta et al. 2004]. (T. Onishi)
J5.3 Circumstellar Disks
Low- and intermediate-mass pre-main-sequence (PMS) stars are usually found to be accompaniedby circumstellar disks of gas and dust. Our solar system and the exoplanets being discovered since1995 are believed to form in the disks, and thus, the disks are called protoplanetary ones. The
physical and chemical properties of the disks are theoretically thought to determine the key
characteristic of a newborn planetary system. One of the major causes of the diversity of the
exoplanets is the radial distribution of the disk surface density. An extensive imaging survey of thedisks around T Tauri stars with the Nobeyama Millimeter Array (NMA) has revealed the diversity ofthe surface density distribution [Kitamura et al. 2002]: the power-law index of the distribution is 0-1 inmost cases, smaller than 1.5 in the Hayashi model, the standard one for the origin of our solar system.
Furthermore, the survey has discovered the radial expansion of the disks as an accretion disk, whichmeans that the physical properties of a disk just at the end of the accretion stage are the initialconditions for planet building.
Another important factor for understanding the exoplanet diversity is the chemical nature of thedisks. However, there exist only a few sources for which interferometer images were obtained with

various molecular lines. For the disk around LkCa 15, the NMA has marginally resolved the spatial
distribution of formaldehyde [Aikawa et al. 2003].

It is found that the column density offormaldehyde is one order of magnitude larger than that predicted by theoretical models of disk
chemistry, while the formaldehyde intensity is less centrally peaked than that of CO, consistent withthe models.
The observational studies of the protoplanetary disks have been performed mainly for young stellar
objects (YSOs) in the Taurus molecular cloud, a typical site for low-mass star formation. To
understand the diversity of planetary systems, however, it is crucial to study the disk properties inother clouds and to reveal region-to-region variations. Another sample of the nearest star-forming
regions is MBM 12, whose distance is considered to be 65-360 pc. The NMA has succeeded in
detecting the dust thermal emission from three YSO disks [Itoh et al. 2003]. The conclusion of thisstudy is that the disks in MBM 12 have masses and IR excesses similar to those in Taurus. (Y.
Kitamura)J5.4 Stars
Masers in evolved stars have extensively been studied with Nobeyama 45-m telescope. The J=2-1
v=1 and 2 transitions of SiO around 43 GHz are easily detectable with this telescope with the SiS
mixer receiver using acousto-opto spectrometers. The high sensitivity due to large aperture of thistelescope enables us to detect the objects at 10 kpc away. Deguchi et al. (2001) detected a number of
new SiO maser sources within a few pc of the Galactic center. Furthermore, a targetted survey of the~400 large-amplitude variables within 30 pc of the Galactic center (Imai et al. 2002b; Deguchi et al.
2003a) yielded about 200 detections in the SiO maser lines. With these systematic surveys by SiO
maser lines, dynamics of the intermidiate-mass stars around the Galactic center black hole wasrevealed. Furthermore, surveys of about 400 IRAS sources in the Galactic disk were performed by
SiO maser lines (Nakashima & Deguchi 2003ab), resulting 250 new detections in SiO. Some of themwere turned out to be very interesting objects (Nakashima et al. 2004; Deguchi et al. 2004) from theview point of stellar evolution.

High-spatial resolution observations with millimeter-wave

interferometers (BIMA & NMA) of these objects were also performed, clarifying the bipolar outflow
structure (Nakashima & Deguchi 2004). The radial velocities of stars, which were accumulated withthese SiO survyes, can be used to obtain the pattern speed of the Galaxy (Deguchi et al. 2004b). (S.
Deguchi)
J5.5 Interstellar Chemistry
Deuterium fractionation is an important problem in astrochemistry. It is deeply related to thechemical evolution and the depletion of molecules onto dust grains. Saito et al. (2002) proposed thatthe deuterium fractionation ratio can be used as an indicator of the chemical evolution of dense coreson the basis of the DCO+/H13CO+ data toward TMC-1 and chemical model calculations. Hirota etal. (2003) mapped the DNC (J=1-0) and HN13C (J=1-0) lines toward several dense cores, and foundthat the chemical fractionation ratio does not vary within each cloud even in L1544, where heavydepletion of molecules has been reported. This means that the DNC/HN13C ratio is not very
sensitive to the depletion factor unlike the DCO+/HCO+ ratio. Since the time scales of chemical
evolution, depletion, and physical evolution are comparable to one another, these three factors should
be considered for detailed interpretation of deuterium fractionation data.

In this relation, an

important contribution from the laboratory microwave spectroscopy has been made by Hirao andAmano (2003). They measured the accurate transition frequency of the 1{10}-1{01} transition of
D2H+ at 691 GHz in the laboratory. Immediately after the laboratory study, Vastel et al. (2004)
detected this line toward IRAS16293-2422, where various deuterated molecules have been detected.
According to the model of deuterium fractionation, D2H+ is expected to be abundant in a cloud withhigh depletion. The detection of D2H+ clearly confirms this effect.
In relation to the chemical evolution of dark cloud cores, Aikawa et al. (2003) studied the
distribution of CCS and other molecules in L1544, considering the effects of the chemical evolution
and the depletion. It is confirmed that the CCS distribution shows a hole at the central part of the corein the late stage, where HN2+ becomes abundant. On the other hand, Hirota et al. (2002) found aunique core, L1521E. In this source, the carbon-chain molecules like CCS are very abundant,
whereas NH3 and HN2+ are deficient. Furthermore it shows a very low deuterium fractionation ratio.
On the basis of these results, they concluded that L1521E should be in a very early stage of chemical
evolution.

Later Tafalla and Santiago (2004) reported that this cloud shows little depletion,

confirming its youth. Hirota et al. (2004) further reported two more clouds which are similar to
L1521E.

These young clouds would be important to understand the initial conditions of starformation.
A big progress has been achieved in the field of grain surface chemistry.

It is well known that thehighly saturated molecules like CH3OH cannot be produced in the gas phase efficiently. Although
the formation of CH3OH on dust grains due to reactions of CO and H is proposed, its detailed
mechanism and reaction rates has still been controversial. Watanabe and Kouchi (2002) succeeded incharacterizing these surface reactions by using the H atom source with calibrated intensity. This andrelated beautiful experiments (Watanebe et al. 2003, Hidaka et al. 2004) have opened a new window
on laboratory studies of grain surface reactions, and they would provide more sound basis of the ratesof the reactions to chemical model calculations of molecular clouds and protoplanetary disks.
As for the extragalactic sources, Takano et al. (2002) reported observations of NH3 toward NGC253
and M82, and discussed the origin of the source-to-source variation of the NH3 abundance. On theother hand, Oike et al. (2004) studied the abundances of C3H2 toward the same sources. (S.
Yamamoto)
J5.6 Pulsars
There are many progresses in theoretical researches.

Following results are obtained on theemission mechanism. The outer gap electrodynamics of the pulsar magnetosphere is solved intwo-dimension for the first time by Takata, Shibata and Hirotani (2004). Contradicting the previous
picture, it has been shown that the magnetic field in pulsar wind nebulae is turbulent (disordered)significantly, requiring a change in the theoretical model [Shibata et al. 2003]. Other studies on thisissue are; the screening of the electric field in the pulsar polar cap [Asano et al. 2004], the estimation of
the fluxes of neutrinos and gamma rays [Nagataki, 2004], the model to the PSR1259-63/Be starsystem [Murata et al. 2003], the propagation and transmission of Alfven waves [Kojima 2004], and thecounterstreaming instability in magnetized pair plasma [Saito 2004]. In addition, there are some
papers on other issues such as simulations on the core collapses [Kotake et al. 2004 and Takiwaki et al.
2004] and acceleration analyses by using magnetohydrodynamic process [Okamoto 2002, 2003].
The investigation on the gravitational delay of pulsar TOA is conducted in NICT, NAOJ and Nagano
NCT. Some presentations on this subject have been done in Japan Applied Physics Society Meetingsin 2004.
As for the observation activities, a 30-m spherical dish has been built in Nasu Pulsar Observatory of
Waseda University. Tracking observation is possible with Az-El Feed Horn system synchronized to
Gregorian subreflector. RF frequency is 1.4GHz and a 2bit 400 MHz/1 bit 800 MHz complex
Nyquist sampler is tested for dispersion removing in voltages. Kashima 34-m telescope in CRL(renamed to NICT since 2004) has been observing the timing of millisecond pulsars almost every
week since 1997 [Hanado et al. 2002]. The observation results at Kashima show good agreementwith other reports [Hanado et al. 2004]. From the simultaneous timing observation with Kalyazin
64-m telescope at in Russia, a long-term DM variation of PSR1937+21 is found [Ilyasov et al. 2004].
The collaboration between Kalyazin 64-m telescope and Kashima 34-m telescope has been continued
in pulsar VLBI [Rodin et al. 2002]. (Y. Hanado)

J6 Extragalactic Radio Astronomy
J6.1 Galaxies
The distribution and dynamics of molecular gas in galactic disks have been studied with the 45-m
telescope and the Nobeyama Millimeter Array of the Nobeyama Radio Observatory: NGC 3079
shows central massive core of the molecular gas (Koda et al. 2002). The molecular gas in the central
regions of the non-barred Seyfert galaxies, NGC 4501 (Onodera et al. 2004) and NGC 5033 (Kohno etal. 2003a), were mapped in CO. Properties of molecular clouds were examined in the spiral arm ofM51 (Tosaki et al. 2002) and in the interarm of NGC 5055 (Tosaki et al. 2003). The dense molecular
gas traced by HCN was well studied in many galaxies, NGC 253 (Paglione et al. 2004), NGC 1097
(Kohno et al. 2003b), NGC 4527 (Shibatsuka et al. 2003), NGC 5195 (Kohno et al. 2002), lenticulargalaxies (Kuno et al. 2002), and CO bright galaxies (Sorai et al. 2002), in relating to star formation and
Seyfert activity. Multitransitions of CO in the Antennae, archetypical interacting galaxy pair, were
fully mapped for their disks to know the relation to starbursts (Zhu et al. 2003), while observations ofammonia (Takano et al. 2002) and cyclopropenylidene (Cyclic-C3H2) (Oike et al. 2004) in M82 andNGC 253 quantitatively revealed physical and chemical properties of the archetypical starburst
galaxies. Rotation curves in the inner disks of Virgo galaxies were determined from the highresolution CO mapping (Koda and Wada 2002, Sofue and Rubin 2001, Sofue et al. 2003a, 2003b,
2003c).
High-resolution observations of CO emission from the z = 4.7 QSO BRI 1202-0725 and the z = 4.4
QSO BRI 1335-0417 using the Very Large Array show that CO is spatially resolved into two
components separated by 1" and 4", with substructure on scales ~0.2"-0.5" (Carilli et al. 2002). The
Sunyaev-Zel'dovich (SZ) effect was successfully detected on a distant galaxy cluster, RX J2228+2037,
at z = 0.421 (Pointecouteau et al. 2002) and on eight galaxy clusters from z = 0.18 to 0.55 (Tsuboi et al.
2004) at 21 GHz and 43 GHz, respectively, and the physical state of the cluster or the Hubble constantis determined. A gamma-ray burst, GRB 030329, was detected at 23 GHz, 43GHz, and 90 GHz withthe 45-m telescope, and time variations of the flux densities were consistent with the expectation fromthe fireball model (Kuno et al. 2004). (N. Nakai)
J6.2 Quasars and Active Galactic Nuclei
Active Galactic Nuclei (AGNs) are considered to consist of a super massive black hole (SMBH) andan accretion disk rotating around it. Relativistic jets often emanate from the disk.
The footpoint of the jet was monitored in the radio galaxy 3C 66B and an orbital motion of the
SMBH-disk system was discovered, implying a SMBH binary. The discovery gives a clue to the
SMBH formation mechanism [Sudou et al. 2003].
Various observations have unveiled fuel reservoirs around the central engine of AGN. NMA
imaged CO (J=1-0) gas associated with a dust disk of 1 kpc in the radio galaxy 3C 31 [Okuda et al.
2005]. HCN (J=1-0) and CO (J=3-2) lines trace denser gas concentrated in the 100-pc region in AGNs
such as NGC 1097 [Kohno et al. 2003a] and M 51 [Matsushita et al. 2004]. Starburst sometimes
happens in such reservoirs and may cause mass accretion into the central engine. An imaging surveyof molecular lines was conducted for 20 nearby Seyfert galaxies using the NMA and proposed adiagnostics of starburst. Seyfert galaxies without starburst show significantly higher HCN-to-COand HCN-to-HCO+ intensity ratios than those with starburst does [Kohno et al. 2003b]. In the central
sub-pc region, these matters are partially ionized to be probed via free-free absorption [Kameno et al.
2003] and polarization properties [Mutoh et al. 2002].
VLBI polarimetry of 3C 273 has revealed a gradient of Faraday rotation measure across the jet,which infers a helical magnetic structure winding up the jet [Asada et al. 2002], predicted by a MHD(Magneto-Hydro Dynamics) collimation and acceleration mechanism. (S. Kameno)Acknowledgements
The editor thanks T. Daishido, S. Deguchi, P.G. Edwards, H. Ezawa, Y. Hanado, T. Handa, T.
Hasegawa, S. Kameno, N. Kawano, Y. Kitamura, H. Kobayashi, M. Kojima, A. Morioka, N. Nakai, T.
Onishi, K. Shibasaki, M. Tsuboi, and S. Yamamoto for their collaboration in preparing this review
article.
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