COMMISSION J : 99

COMMISSION J : RADIO ASTRONOMY (Nov. '95 - Oct. '98)

Edited by Makoto Inoue

J1. Introduction

The Nobeyama Radio Observatory (NRO), a radio astronomy facility of the National Astronomical Observatory of Japan (NAOJ), runs the 45-m telescope and Nobeyama Millimeter Array (NMA) for various fields of radio astronomy. NRO also runs the Nobeyama Radioheliograph for solar observations. All these are operated under the open-use scheme. NAOJ runs the 10-m telescope in Mizusawa and the 6-m telescope in Kagoshima, the latter in collaboration with Kagoshima University.

The Institute of Space and Astronautical Science (ISAS) and NAOJ operate the VLBI Space Observatory Programme (VSOP), which is the first space VLBI project run by international collaboration of radio observatories and space agencies. Three NAOJ telescopes, i.e. the 45-m, 10-m and the 6-m telescopes, are sometimes combined to perform the Japanese VLBI network (JNET), which often includes the 34-m telescope of the Communications Research Laboratory (CRL), the Ministry of Post and Tele-communications in Kashima. CRL also operates a four station VLBI network around Tokyo metropolitan area.

Nagoya University and the Institute of Astronomy, University of Tokyo, run the 4-m and the 60-cm telescopes, respectively, to make large-scale CO survey observations of molecular clouds. They both built the second telescopes to observe the Southern Hemisphere sources, and brought them to Chile. Waseda University has completed the 64-element interferometer for monitoring transient radio sources. The Department of Physics, University of Tokyo, has started the Mt. Fuji Submillimeter Telescope Project in collaboration with the Institute of Molecular Science and NRO. Radio observations on the Solar System have been conducted at the Solar Terrestrial Environment Laboratory in Nagoya University, CRL, and Hyogo College of Medicine.

NAOJ has been proposing the Large Millimeter and Submillimeter Array (LMSA), and conducting its feasibility study and site testing in Chile. International collaboration to merge the similar projects proposed by US and Europe is under discussion. NAOJ has been promoting the VERA (VLBI Exploration of Radio Astrometry) project, a dedicated VLBI array for radio astrometry.

J2. New Instrumentation

J2.1. NRO 45-m Telescope and NMA

It was found in 1995 that the antenna efficiencies of the 45-m telescope at 3 mm had dropped by 25% due to a large-scale deformation of the surface. The efficiencies were recovered in summer 1996 after tightening of loose bolts of the backup structure. A 25 multi-beam receiver for 80-115 GHz was installed on the 45-m telescope in April 1998, and preliminary test observations were successfully made using existing AOS's. A digital backend system for this array has been under construction. Design of LSI and trial manufacture of a 1-GHz sampler were made in 1995, and a trial system was assembled in 1997. The system was successfully tested in May 1998.

A series of radio holography measurements and readjustments of the surface panels of NMA antennas has improved the surface accuracy; 46 micron rms for the new 6th antenna in 1996 and 80 micron rms for the other five antennas in 1997. In order to make wide-band observations, the first intermediate frequency of NMA has been changed from L-band to 5-7 GHz band. The receiver and IF transmission system was renewed accordingly in 1996. A new digital ultra wide-band correlator (1 GHz) and an FX-type correlator (32 MHz) have been routinely used for NMA observations since December 1996. Receivers at 230 GHz were installed on NMA antennas and have been used for observations since January 1998. A new experimental array, named as Rainbow Array with the 45-m and six NMA antennas, has been used to make high sensitivity mapping observations at both 3- and 2-mm bands.

J2.2. Nobeyama Radioheliograph

The Nobeyama Radioheliograph (NoRH) has been operating since 1992. Initially, observing frequency was single at 17 GHz. In 1995, dual frequency capability was added by introducing the frequency selective sub-reflector (FSS). Data acquisition is in time-sharing basis; 17 GHz RCP, LCP then 34 GHz with the duty cycle of 100 ms. After the solar minimum in 1996, the number of energetic events detected by NoRH has been increasing toward the maximum in the year 2000. Software development of the image synthesis of NoRH data made it possible to study quiet features and low-contrast features on the Sun such as dark filaments and polar cap brightening. Speedup of image synthesis made it possible to study dynamical features with high cadence.

J2.3. VSOP

The satellite HALCA was launched on February 12, 1997 from the Kagoshima Space Center of ISAS to have apogee and perigee heights of 21,000 km and 550 km, respectively. The 8-m onboard antenna was deployed on February 27, 1997. The satellite is dedicated for the space VLBI engineering test and scientific observations with L, C, and K band receivers. HALCA is linked by Usuda, Goldstone, Greenbank, Madrid, and Canberra stations at Ku band. They send a reference signal locked on a hydrogen maser and receive HALCA 128-Mbps VLBI data. After the successive satellite system checks, the first fringe from HALCA was detected on May 7 toward the Usuda 64-m telescope using the Mitaka correlator of NAOJ. The FX correlator at Mitaka is operated as a VSOP correlator, and correlators of VLBA (NRAO) and S2 (DRAO) are also used. Scientific observations have been conducted since September 1997, by close collaboration with VLBI networks and ground radio telescopes throughout the world. By the end of 1998, about 150 open-use observations were done together with about 100 survey observations which are led by the mission group. VSOP has been producing high-resolution images of AGNs, pulsars, and maser sources with good quality [Hirabayashi et al. 1998]. On March 1998, VSOP detected K-band fringes of the burst water maser in Orion KL.

J2.4. Ground-Based VLBI JNET

JNET consists of the Nobeyama 45-m telescope (NRO), Mizusawa 10-m telescope (NAOJ), Kagoshima 6-m telescope (NRO), and Kashima 34-m telescope of CRL. Open-use observations started in 1994 at 22 GHz, and receivers at 43 GHz have been installed. The VSOP recording system, which is based on the K4 recording system with one or two channels of 16-MHz bandwidth, is used. The recorded data are correlated at Mitaka of NAOJ. Distribution of the water maser spots has been monitored in several star forming regions and late type stars by JNET. An outburst of Orion KL water maser has been discovered with Kagoshima 6-m telescope, and the VLBI monitoring observations are now undergoing. Compact water masers around late type stars were found by the JNET [Imai et al. 1997a], and velocity shifts were found in several water masers of RT Vir [Imai et al. 1997b].

CRL started the Key Stone Project (KSP) since 1995. The project is to monitor local crustal deformation in the Tokyo metropolitan area using a four-station VLBI, LLR, and GPS networks. The VLBI data are transferred to the correlator by optical fiber and processed in real time manner. Geographical Survey Institute (GSI) has built and been operating a five-station VLBI network for geodetic aims. CRL and NAOJ have developed a Giga-bit bandwidth VLBI recording system, and first fringes were detected. Real time VLBI system using 256-Mbps optical fiber network has been developed by CRL, NAOJ, and ISAS.

J2.5. The 60-cm Telescopes of the University of Tokyo

The radio astronomy group at the Institute of Astronomy of the University of Tokyo has run two 60-cm radio telescopes, called the VST1 and VST2. The VST1 is located at Nobeyama and the VST2 is at La Silla in Chile. They are twin and have the same 9-arcmin beamwidth. These telescopes are used for survey observations of the Galactic plane and nearby molecular clouds in CO J=2-1 line. The beamsize of 9 arcmin enables us to make direct comparison with the Columbia Survey in CO J=1-0 line, which gives density and temperature of molecular gas. An SIS receiver and a 2048-ch AOS with 500-MHz bandwidth were installed at VST1. A cooled Schotkey diode mixer receiver and a 2048-ch AOS with 1-GHz bandwidth were installed at VST2.

Using the twin telescope the Galactic plane survey has been made for the first and forth quadrants. Both of the two halves of the Galactic plane survey show systematic decreasing with the galacto-centric radius in the CO J=2-1/J=1-0 line intensity ratio. Several molecular clouds, such as the Rosetta nebula, eta Car, Taurus, and Cepheus regions, were observed. Molecular clouds in Pereus arm and the Galactic center region were also observed. The results for these regions show variety of physical states of molecular gas in the Galaxy. Several positions in the LMC were also observed.

J2.6. The 4-m Telescope of Nagoya University

Nagoya University has constructed a new 4-m telescope to establish a mm and sub-mm radio observatory in the Las Campanas Observatory in Chile. This is based on a collaborative effort between Nagoya University and the Carnegie Institution of Washington. The facility consists of the 4-m radio telescope with a superconducting Nb mixer receiver of 50 K (SSB) receiver temperature at 110 GHz. The beamsize of about 3 arcmin allows us to survey the CO distribution efficiently without losing details.

The astronomical observations have been carried out since September 1996. A CO J=1-0 survey of Large Magellanic Cloud (LMC) has been made. This survey first revealed the existence of more than 100 Giant Molecular Clouds with a linear spatial resolution of ~40 pc. The CO survey observations of the Galactic objects have been also carried out. These observations include southern dark clouds (Lupus, Ophiuchus, Chamaeleon, Southern Coalsack, Aquila, etc.), Giant Molecular Clouds (Carina, Vela, S35, S37, etc.), and High Latitude Clouds. We also found what we call the "Carina Super Shell," which is the first detected super shell in the Galaxy with Giant Molecular Clouds and the induced star formation. The operation frequency will be extended to the sub-mm region in a few years.

J2.7. Arrays of Waseda University

The array of the Nishiwaseda Astrophysical Observatory, Waseda University, is a Nyquist rate direct imaging radio interferometer of 8 x 8 elements with each 2.4-m diameter operating at 10.6 GHz. The HEMT receiver temperature is 50-60 K at normal temperature. Digital lens (2D FFT processor) is used for Nyquist rate imaging with a 20-MHz bandwidth each. Transmission coaxial cables at present are being replaced to bit-parallel optical fibers to reduce phase fluctuations.

First five spherical dish antennas of 20 m in diameter are under construction for Huge Pulsar Array project in Nasu Pulsar Observatory at Nasu (160 km north of Tokyo). Observing frequency is at 1.4 GHz with the HEMT receiver temperature of 40 K at normal temperature. A (2+1+2)D FFT processor has been developed for pulsar survey and timing observation [Daishido et al. 1996]. A (2+1)D FFT processor, spatial-temporal FFT processing, is a conceptual extension of above Digital lens. The total 16 x 16 x 256 complex data in spatial and temporal space could be Fourier transformed to (16 x 16)-pixel x 256-ch momentum and frequency space at Nyquist rate of 50 nano sec.

J2.8. Mt. Fuji Submillimeter Telescope

A joint group, consisting of the Department of Physics and Research Center for Early Universe in the University of Tokyo, the Institute for Molecular Science, and NRO, is operating a 1.2-m submillimeter telescope at the summit of Mt. Fuji (Elevation 3700 m). This project aims at survey observations of the neutral carbon atom to understand formation processes and structure of molecular clouds. Taking an advantage of good observing conditions from Mt. Fuji, areas of more than 20 square degrees mostly toward nearby molecular clouds have already been observed with the CI J=1-0 (492 GHz) and CO J=3-2 lines. Observations of the CI J=2-1 (809 GHz) line will start from the end of 1999.

J2.9. LMSA Project

NAOJ is planning a project to construct a large interferometric array at millimeter and submillimeter wavelengths which will be located on a high, dry site in the eastern Atacama Desert of Northern Chile. The project called the Large Millimeter and Submillimeter Array (LMSA) is a high priority project for the future large-scale ground-based astronomical facility of Japan [Ishiguro 1997, Ishiguro et al. 1998]. The LMSA is an array consisting of fifty 10-m antennas covering wide frequency range from 80 GHz to 890 GHz. In addition to the measurements using 220-GHz tipping radiometer and 11-GHz radio seeing monitor in the Pampa la Bola area, opacities at submillimeter wavelengths have been measured with a Fourier transform spectrometer [Matsuo et al. 1998] and 492-GHz tipping radiometer [Hirota et al. 1998]. The main scientific targets of LMSA are to reveal the fundamental process of star and planet formation, and the formation and evolution of galaxies. With a 10-km maximum baseline at 350 GHz the LMSA will provide 10 milli-arcsecond resolution which is crucial to resolve a proto-planetary disk. The design and development are underway especially for antenna [Ishiguro et al. 1996], submillimeter mixers [Shi et al. 1997], and correlator system. A new 10-m submillimeter telescope is under construction at Nobeyama as an LMSA prototype antenna, which is expected to achieve very high surface accuracy with lightweight machined aluminum panels and a CFRP backup structure. It is proposed to realize more powerful array and cost saving by merging the LMSA with European LSA and US MMA projects.

J2.10. VERA Project

A group of scientists in the fields of VLBI research, high-precision astrometry, and Galactic dynamics is jointly promoting the VERA (VLBI Exploration of Radio Astrometry) project proposed by NAOJ. A dedicated differential VLBI array aiming at very high precision radio astrometry of 10 micro-arcsecond level will be constructed with four stations spread over the islands of Japan. Each station will be equipped with a 20-m class antenna capable of observing almost simultaneously two closely spaced radio sources to facilitate effective compensation of the degrading atmospheric phase fluctuations. Receiving frequency bands will be 43, 22, 8 and 2 GHz. VERA will measure annual trigonometric parallax and proper motion of thousands of astronomical masers across the Milky Way Galaxy by the phase-referenced VLBI observations with adjacent quasars. Scientific objectives include accurate determination of the dynamical mass of the Galaxy and hence the amount of the Galactic dark gravitating matter, construction of the three-dimensional dynamical map of the Galaxy, distance determinations to the star-forming regions, direct calibration of the period-luminosity relation of Mira variables, phase-referenced VLBI imaging of faint radio sources, ground support observations for future space VLBI missions, and some applications to geodetic and selenodetic observations.

J3. Solar Radio Astronomy

Almost all works on solar radio astronomy in Japan during the period 1995-1998 were based on the observations with the NoRH (see J2.4). By the software development of fast and deep CLEAN with the help of Steer's algorithm [Koshiishi 1996], weak features are now one of the major subjects using the NoRH. The radio synoptic maps and a radio butterfly diagram for 7 years were synthesized [Shibasaki 1998]. Polar cap brightening is the most prominent feature in the butterfly diagram. Based on its annual variation, it is interpreted as the result of the combined effect of limb brightening and intrinsic brightening. Coronal holes were studied by NoRH [Gopalswamy et al. 1998]. Some parts of coronal holes, where magnetic field is stronger, are brighter, although no EUV enhancements were detected. It is interpreted that higher temperature and density at upper chromosphere are due to the brightening. Prominence eruptions associated with CMEs were studied extensively, combined with SOHO and YOHKOH satellite observations [Gopalswamy et al. 1996, 1997 and 1998]. It was shown that NoRH is one of the best instruments for such studies, because of continuous observations of the whole Sun with high cadence. Magnetic field configurations in impulsive microwave bursts were studied [Nishio et al. 1997, Hanaoka 1997]. Both studies showed that at least two loops are involved in flares. They consist of small and long loops with 3-legged configuration. Particle acceleration is interpreted as the result of the interaction of two loops.

Interplanetary scintillation (IPS) has been employed for solar wind studies at the Solar-Terrestrial Environment Laboratory, Nagoya University. A computer assisted tomography (CAT) technique has been developed to obtain unbiased solar wind parameters from the IPS measurements [Asai et al., 1998, Kojima et al. 1998]. Using the CAT analysis technique, the origin of low-speed solar wind and latitudinal velocity structure [Kojima et al. 1998] have been studied. Electron density profile in solar wind acceleration regions has been investigated using the IPS CAT technique [Yokobe et al. 1998] and theoretical simulation [Yamauchi et al. 1998].

J4. Solar System Radio Astronomy

The long-term variation of the solar wind structure near the sun was investigated using the interplanetary scintillation data taken at 2 and 8 GHz in the period 1990 to 1994 [Tokumaru et al. 1996]. Shishov and Tokumaru [1996] theoretically studied the power spectrum and two-frequency co-spectrum of interplanetary scintillation in the near-Sun region and pointed out importance of the effect of MHD waves. Polarization measurements in the frequency range from 20.5 to 25.5 MHz were made for 20 storms of Jovian Io-related sources A and B. A significant difference in axial ratio between the two sources was found [Misawa et al. 1997]. Worldwide cooperative observations over a wide frequency range were made during the comet SL9/Jupiter impact period. No detectable effects of the comet collision on the Jovian decametric radiation were reported [Maeda et al. 1995, Reyes et al. 1997].

J5. Galactic Radio Astronomy

J5.1. Galactic Center Region

Wide-area mapping observations in CO J=1-0 [Oka et al. 1998] and CS J=1-0 [Tsuboi et al. 1999] were made in the central few-degree region with the 45-m telescope. Many expanding shells were founded in the region, which is probably due to the powerful star-forming activity of the Galactic center region earlier [Tsuboi et al. 1998, Hasegawa et al. 1998]. A wider-area CO J=2-1 mapping was performed with the 60-cm telescope of University of Tokyo [Oka et al. 1997]. A compact cloud with a very large velocity width over 100 km/s was found near the center [Oka et al. 1998b]. An expanding shell was found to interact with the radio arc, which probably activates the radio arc [Tsuboi et al. 1997b]. A mass spectrum of the molecular clouds was derived [Miyazaki and Tsuboi 1998, Oka et al. 1998c]. Intensity monitoring at 100 and 150 GHz of Sgr A* was performed with NMA [Tsutsumi et al. 1998b]. A spectrum of Sgr A* in near-millimeter wavelength was obtained with the 45-m telescope [Falcke et al. 1998]. Polarimetry at 40 GHz revealed poloidal magnetic field and strong Faraday rotation in the radio arc [Tsuboi et al. 1995].

J5.2. Star Forming Regions

Properties of molecular gas in the first quadrant of the Galaxy are examined through a galactic CO J=2-1 survey with Univ. Tokyo 60 cm telescope [Sakamoto et al. 1997]. Large-scale mm-wave observations of molecular clouds provided implication regarding the fragmentation of clouds and star formation in Taurus [Mizuno et al. 1995, Onishi et al. 1996], Cepheus and Cassiopeia [Yonekura et al. 1997, 1998], and Orion [Nagahama et al. 1998]. The distribution of the low-density and high-density gas of the archetypal GMC, Orion A, was studied in detail by Sakamoto et al. [1997] and Tatematsu et al. [1998]. TMC-1C was studied in H¹³CO⁺ and CH₃OH with the Nobeyama 45-m telescope and the chemical evolution of the low-mass cores was revealed [Takakuwa et al. 1998]. The cometary globule in IC1396 was studied with the NMA, and evidence for radiation-driven implosion was obtained [Sugitani et al. 1997]. X-ray emitting protostars in Ophiuchus were observed in CO J=1-0 and CO J=2-1, and the detected outflows are found to be pole-on [Sekimoto et al. 1997]. Molecular outflows associated with Barnard 1 and L723 were studied in single-dish and interferometric observations [Hirano et al. 1997, 1998]. A very massive molecular outflow was discovered toward IRAS 22142+5206 with the Nobeyama 45-m telescope [Dobashi et al. 1998].

An increasing number of studies toward the IRAS sources embedded in the molecular clouds have been performed at Nobeyama. Ramesh et al. [1997] calculated the self-reversed line profiles of HCO⁺ and CS, and their isotopic species in IRAS 18507+0121. They concluded the presence of cold intervening screen in front of the hot core. Yonekura et al. [1998] studied the Head-Tail structure and outflow associated with IRAS 22103+5828 in the molecular cloud S134. Chen et al. [1996] mapped the CS and continuum emission with NMA and identified the structure within 0.1 pc of the IRAS 05338-0624 in the dark cloud L164N. Yang et al. [1995] mapped the CS J=2-1 line and found an elongated structure of the 0.14 pc x 0.08 pc at the position of IRAS 00338+6312 in the dark cloud L1287. Yonekura et al. [1997] studied a large scale structure at the Cepheus and Cassiopeia regions with Nagoya 4-m telescope and found a mass spectrum with power index of 1.7 and a relation of maximum luminosity of IRAS sources with cloud mass.

J5.3. Circumstellar Disks

Saito et al. [1996] and Momose et al. [1998] observed L1551 IRS5, and made clear the detailed kinematics of the rotating/infalling motion of the circumstellar gas disk. Disks around DM Tau [Saito et al. 1995], DG Tau [Kitamura et al. 1996a, 1996b], and HH 111 [Yang et al. 1997] were studied with the NMA. Kitamura et al. [1996a] found a dust disk around DG Tau with a size of 218 AU x 76 AU with NMA at 147 GHz.

J5.4. Stars

Thermal and maser emissions from stars and their environments have been studied extensively with the 45-m telescopes and NMA. The spectral line survey at frequencies between 28 and 50 GHz has been performed for the late-type star, IRC+10216 [Kawaguchi et al. 1995]. About 150 lines out of 180 detected lines were assigned to the transitions of 22 known molecules, 38 still unidentified. The protoplanetary nebula, CRL2688, has been studied extensively by the ¹³CO and CS lines with NMA [Yamamura et al. 1997, Kasuga et al. 1997]. The emission from CO was found almost circular but that from CS aligned on the bipolar axis. These studies have shown the molecular distributions are unexpectedly complex and different from molecule to molecule in the circumstellar envelopes.

Masers by vibrationally excited SiO have been used for studying the circumstellar environment as well as the structure of the Galaxy. Jiang et al. [1996a] detected 56 new SiO sources in 181 observed sources located at the outer part of the Galaxy. Izumiura et al. [1998] detected 14 SiO maser sources towards the Galactic center. Shiki et al. [1997] detected 6 new SiO sources (late-type stars) toward the Sgr B2 cloud. Cho et al. [1996] have made multiple line studies of ²⁸SiO and ²⁹SiO in 102 stars. Some of these stars have been studied in the optical and near infrared bands by Jiang et al. [1996b], Jiang et al. [1997], Deguchi et al. [1997]. Fine structure of masers has been studied with VLBI. Imai et al. [1997ab] observed water masers at 22 GHz and found evidence of acceleration (linear drift) of radial velocity of maser spots in RT Vir. The radio continuum emission from four X-ray stars was monitored by Tsutsumi et al. [1996] with NMA and a physical constraint of the inverse-Compton model was considered.

J5.5. Interstellar Chemistry

Four new molecules H₂CHO⁺ [Ohishi et al. 1996], c-C₂H₄O [Dickens et al. 1997], HDCS [Minowa et al. 1997], and C₇H [Guelin et al. 1997] have been detected. The c-C₂H₄O molecule and the structural isomer acetaldehyde were searched by Nummelin et al. [1998] toward many molecular clouds and detected in the hot cores NGC 6334F, G327.3-0.6, G31.41+0.31, and G34.3+0.2. Takano et al. [1998] have reported the observations of the ¹³C substituted HC₃N (H¹³CCCN, HC¹³CCN, and HCC¹³CN) rotational lines in TMC-1 and derived the abundance ratios of 1.0:1.0:1.4 for [H¹³CCCN]:[HC¹³CCN]:[HCC¹³CN]. The enriched abundance of HCC¹³CN was explained by the production mechanism of HC₃N through a neutral-neutral reaction of CN with C₂H₂. The same conclusion was obtained by analyzing the potential energy surface [Fukuzawa et al. 1997], and it was confirmed that the reaction is exothermic and has no energy barrier. These studies gave important results for explaining the formation mechanism of carbon-chain molecules.

Metal compounds FeCO, NaSH, MgH, MgO, MgOH, CaH, CaOH, and CaO were studied in laboratory and searched for in interstellar space and/or circumstellar envelopes by Kagi et al. [1997] and Sakamoto et al. [1998]. However, none of them have been detected. In a series of papers, Aikawa et al. [1996, 1997] reported theoretical studies on the evolution of the molecular abundance in protoplanetary disks, where adsorption of molecules onto grains as well as the reactions in the gas phase was taken into account.

J5.6. Pulsars

ASCA group investigated the difference of observed pulse phases in radio and X-ray region. They determined the phase lag between the radio and X-ray pulses for PSR1821-24 (millisecond pulsar) and for PSR1509-58, setting a strong constraint on the emission mechanism [Rots et al. 1998]. Pulsar VLBI observations are carried out several times per year between the 34-m antenna of CRL and the 64-m antenna of Lebedev Physical Institute in Russia [Sekido et al. 1996]. They determined the coordinate of PSR0329+54 with milli-arcsecond precision in International Celestial Reference Frame (ICRF). CRL group developed the timing observation system with 200-MHz pass-band for Kashima 34-m antenna [Hanado et al. 1998] and started the weekly observation of PSR1937+21 (millisecond pulsar) since November 1997. This observation of the fastest pulsar (P = 1.56 msec) should provide a significant contribution on the highest precision timing measurement and on the magnetopsheric theory when it is compared with observations in other frequency bands.

J6. Extragalactic Radio Astronomy

J6.1. Galaxies

Large scale distribution and dynamics of molecular gas in galaxies have been investigated by CO mapping observations with the NRO 45-m telescope. Kuno and Nakai [1997] derived the gas motion in the galactic disk of M51 from CO data. The motion and distribution of the molecular gas are consistent with the density wave theory. Kuno et al. [1997] showed that the flocculent spiral galaxy NGC5055 has a two-arm spiral structure of molecular gas.

The physical conditions of molecular gas in galaxies have been investigated by multi-line observations. Matsushita et al. [1998] derived the physical condition of the circumnuclear dense molecular gas from the HCN/¹³CO ratio. Sakamoto et al. [1997] found the systematic gradient of the ¹³CO/¹²CO ratio as a function of the galacto-centric distance in NGC891, and interpreted it in terms of the variation of the dense molecular gas fraction. The relation between the surface density of molecular gas and star forming activity was examined in post-starburst galaxies [Tosaki and Shioya 1997, Shioya et al. 1998] and a flocculent galaxy [Sakamoto 1996].

J6.2. Quasars and Active Galactic Nuclei

H₂O megamaser is a powerful probe for gas dynamics in the central region of AGNs with a sub-pc resolution. A series of the observations towards the archetype of the megamaser source NGC 4258 revealed a sub-pc jet at the dynamical center of the maser spots [Herrnstein et al. 1997], and gave constraints on the models of accretion disks [Herrnstein et al. 1998]. Hagiwara et al. [1997] detected the maser emission from a rotating disk in the active galaxy NGC 5793. Satoh et al. [1998] suggested a thick molecular torus with the radius of about 1 pc around the center of NGC 3079. Nakai et al. [1998] also found a rotating disk in the center of a Seyfert 2 galaxy IC 2560. All these results support the presence of a massive black hole at the center of the rotating disk.

The NMA has detected thermal molecular emission from AGNs as a probe for a physical condition. The conspicuous work is the detection of CO J=5-4 emission line at millimeter region towards a high redshift quasar BR1202-0725 at z = 4.69 [Ohta et al.1996], followed by CO J=2-1 observations [Ohta et al. 1998]. These results indicate a high-density (10^3.5-10^5.5 cm^-3) and high kinetic-temperature (50-100 K) of the molecular gas in the early universe. Inoue et al. [1996] found a molecular torus in the center of the active galaxy NGC 1275 (3C 84) with a huge amount (3 x 10¹¹ solar mass) of molecular gas.

Space VLBI observations with VSOP have provided extremely high-resolution (0.5 mas) studies of AGNs [Hirabayashi et al. 1998]. Observations towards a gamma-ray source 1156+295 showed that the brightness temperature exceeds the Compton limit of 10¹² K, and proved that the Doppler boosting is working. VSOP images of high-redshift quasars 0014+813 at z = 3.366 identified the core and bending jets.

Acknowledgements

The editor thanks T. Daishido, S. Deguchi, T. Handa, Y. Hanado, M. Ishiguro, S. Kameno, O. Kameya, K. Kawaguchi, H. Kobayashi, M. Kojima, N. Kuno, T. Ohnishi, K. Maeda, T. Sasao, K. Shibasaki, K. Tatematsu, M. Tsuboi, N. Ukita and S. Yamamoto for their collaboration in preparing this review article.

Commission H ('99)

Commission K ('99)

Commission J ('93)

Commission J ('96)

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COMMISSION J : RADIO ASTRONOMY (Nov. '95 - Oct. '98)

Edited by Makoto Inoue

J1. Introduction

J2. New Instrumentation

J2.1. NRO 45-m Telescope and NMA

J2.2. Nobeyama Radioheliograph

J2.3. VSOP

J2.4. Ground-Based VLBI JNET

J2.5. The 60-cm Telescopes of the University of Tokyo

J2.6. The 4-m Telescope of Nagoya University

J2.7. Arrays of Waseda University

J2.8. Mt. Fuji Submillimeter Telescope

J2.9. LMSA Project

J2.10. VERA Project

J3. Solar Radio Astronomy

J4. Solar System Radio Astronomy

J5. Galactic Radio Astronomy

J5.1. Galactic Center Region

J5.2. Star Forming Regions

J5.3. Circumstellar Disks

J5.4. Stars

J5.5. Interstellar Chemistry

J5.6. Pulsars

J6. Extragalactic Radio Astronomy

J6.1. Galaxies

J6.2. Quasars and Active Galactic Nuclei

Acknowledgements

Contents

Commission H ('99)

Commission K ('99)

Commission J ('93)

Commission J ('96)

References

Contents

Commission H ('99)

Commission K ('99)

Commission J ('93)

Commission J ('96)