With Kagoshima 6 Meter Radio Telescope

Takumi Nagayama1, Toshihiro Omodaka1, Toshihiro Handa2, Tsuyoshi Sawada3, Hayati Bebe Iahak1 and Naohito Matsuyama1 1 Faculty of Science, Kagoshima University, 1-21-30 Korimoto, Kagoshima 890-0065 2 Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015 handa ioa.s.u-tokyo.ac.jp 3 Nobeyama Radio Observatory, National Astronomical Observatory of Japan, Minamimaki, Minamisaku, Nagano 384-1305 sawada ioa.s.u-tokyo.ac.jp NH3 lines are useful to estimate the temperature of...

List of Participants

Amram Philipe, Laboratoire d'Astrophysique de Marseille, OAMP, Universite de Provence, CNRS, France Philippe.Amram oamp.fr Arimoto, Nobuo, NAOJ, arimoto optik.mtk.nao.ac.jp Athanassoula, Evangelia, Observatoire de Marseille, lia oamp.fr Azzollini, Ruyman, Instituto de Astrof sica de Canarias, ruyman iac.es Baker, Andrew, NRAO University of Maryland, ajb astro.umd.edu Beckman, John, Insitituto de Astrof sica de Canarias, jeb iac.es Beletsky, Yuri, ESO, ybialets eso.org Benjamin, Robert, U of...

High Latitude Clouds

We have carried out high galactic latitude molecular clouds observations with the NANTEN telescope in order to reveal the molecular gas distribution around the solar system and the physical properties of low-density molecular clouds. Three types of observations have been made at the region. A survey for high galactic latitude molecular clouds was carried out toward the 68 of far-infrared excess clouds of 12 by using 12CO (J 1-0) line 11 . The CO emissions were detected in the 32 infrared excess...

Feeding of Nuclear Clusters

2.1 The Late Type Spiral Galaxy IC 342 IC 342 is a prime example of a late-type spiral galaxy with a young luminous nuclear cluster that formed in a short-lived burst about 60 Myr ago (Boker et al. 1997, 1999b). The central region of IC 342 has been mapped in the past in several molecular transitions on scales of a few arcseconds (e.g. Meier & Turner 2001). These maps show that the molecular gas is located in two spiral arms that show strong streaming motions. The spiral arms join to form a...

VERA Project

Mareki Honma, Takeshi Bushimata, Yoon Kyung Choi, Tomoya Hirota, Hiroshi Imai, Kenzaburo Iwadate, Takaaki Jike, Osamu Kameya, Ryuichi Kamohara, Yukitoshi Kan-ya, Noriyuki Kawaguchi, Masachika Kijima, Hideyuki Kobayashi, Seisuke Kuji, Tomoharu Kurayama, Seiji Manabe, Takeshi Miyaji, Takumi Nagayama, Akiharu Nakagawa, Chung Sik Oh, Toshihiro Omodaka, Tomoaki Oyama, Satoshi Sakai, Katsuhisa Sato, Tetsuo Sasao, Katsunori M. Shibata, Motonobu Shintani, Hiroshi Suda, Yoshiaki Tamura, Miyuki Tsushima,...

Possible Detection of Outer Plasma Around AGN Jets

Asada1, H. Nagai1, Y. Murata2, and P. Edwards2 1 National Astronomical Observatory of Japan 2 Institute of Space and Astronautical Science We point out a possible way to investigate a plasma cocoon which has been revealed recent Faraday rotation studies of AGN jets. A high spatial resolution observation of VSOP suggests a sharp absorption feature which suggests free-free absorption by the plasma cocoon. The spiral jet configuration could provide, in general, an...

Molecular Gas in NGC 1068

As the cornerstone of AGN unification models, NGC 1068 is one of the most studied objects in the night sky, yet many aspects of its nuclear region remain poorly understood, despite its proximity. In particular, the peculiar gas kinematics revealed in 0.7 CO(2-1) mapping were modelled as a warped disk 13 . It is now apparent from our 2.12 m H2 1-0 S(1) maps of the distribution (Fig. 1) and kinematics (Fig. 2), which have a spatial resolution nearly 10 times better, that this picture is too...

Ram Pressure Models

Several groups have investigated the effects of ram pressure on a gas-rich spiral galaxy. These groups have employed different ways to describe the ISM continuous description Eulerian hydrodynamics in 2D 17 and 3D 18 , 19 , 11 discrete-continuous hybrid description smoothed particles hydrodynamics 1 , 20 discrete description sticky particles 26 . These groups studied galaxies with different rotation velocities and different initial gas surface density profiles. In addition, most of the authors...

Ngc 2146

Kawabe2, K. Nakanishi2, B. Vila-Vilaro2, K. Kohno3, T. Inui4, H. Matsumoto4, T. G. Tsuru4, and A. B. Peck5 1 Academia Sinica, Institute of Astronomy and Astrophysics 2 National Astronomical Observatory of Japan 5 Harvard-Smithsonian Center for Astrophysics We performed deep CO(1-0) mapping of the central 60 regions of nearby edge-on starburst galaxies M82 and NGC 2146 with the Nobeyama Millimeter Array. Both galaxies show kpc-scale Ha and or soft X-ray...

Kinematics of Molecular Gas in the Bar of Maffei

Kazuo Sorai1, Nario Kuno2, Naomasa Nakai3, Hidenori Matsui1 and Asao Habe1 1 Institute of Fundamental Physics, Department of Cosmosciences, Graduate School of Science, Hokkaido University sorai astroi.sci.hokudai.ac.jp 3 Institute of Physics, The University of Tsukuba We made 12CO J 1 0 observations of nearby barred spiral galaxy Maffei 2 with Nobeyama 45-m telescope and Nobeyama Millimeter Array. Molecular gas concentrates on the central region and the bar, which is seen in the 2MASS K-band...

Molecular Gas in the Andromeda Galaxy Properties of the Molecular Clouds

Ungerechts3, L. Loinard4, R. Lucas2, and R. Wielebinski5 1 Academia Sinica Institute of Astronomy and Astrophysics P.O. Box 23-141, Taipei, 106 Taiwan 2 Institut de Radioastronomie Millimetrique, St Martin d'Heres, France 3 Instituto de Radioastronomia Millimetrica, Granada, Spain 4 Centro de Radioastronomia y Astrof sica, UNAM, Morelia, Mexico 5 Max-Planck-Institut f r Radioastronomie, Bonn, Germany The closest spiral galaxy, M31, is certainly a key target to...

Mass of the GMCs

There are different methods to derive the mass of the molecular gas in the interstellar medium, but the easiest one is to apply a CO to H2 conversion factor N(H2) X Ico(1-o), where N(H2) is the column density of molecular gas and ICo(1-o) the integrated intensity of the CO(1-0) emission. In the Milky Way, a standard value X 1 - 4 1020 cm-2K-1km-1s is observed (e.g. Solomon et al. 1987, Strong & Mattox 1996). In the following, we compare the molecular mass derived from the CO luminosity to...

And Near Infrared Interstellar Extinction

Shogo Nishiyama1, Tetsuya Nagata2 and Koji Sugitani3 1 National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, Japan shogo optik.mtk.nao.ac.jp 2 Kyoto University, Kyoto 606-8502, Japan 3 Nagoya City University, Nagoya 467-8501, Japan The IRSF SIRIUS Galactic center survey project is a deep near-infrared (J, H, KS) survey of the central region of our Galaxy with the 1.4 m telescope IRSF and the infrared camera SIRIUS 1, 2 . The pixel scale of SIRIUS is 0'.'45, and the limiting...

The Angstrom Project

Eamonn Kerins, on behalf of The Angstrom Project Team Astrophysics Research Institute, Liverpool JMU, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK ejk astro.livjm.ac.uk The Andromeda Galaxy Stellar Robotic Microlensing (Angstrom) Project is a long-term microlensing survey of the bulge of the Andromeda Galaxy (M31). Microlensing describes the transient magnification of starlight by the gravitational field of a foreground compact object passing close by the line of sight. The...

The Latest from the VLA

In the following, we present some new observations that we recently obtained at the VLA in B array configuration (D. Riechers, PhD Thesis, MPIA Heidelberg). APM0827+5255 (z 3.9) The presence of extended C0(1-0) emission in APM0827+5255 was reported by Papadopoulus et al. (2001). Additional C0(2-1) Fig. 2. Image of C0(1-0) towards APM 08729+5255 obtained with the VLA covering a bandwidth of 43.75MHz, or 560km s-1 (Riechers et al. 2006, in prep.). Contours are shown at -3, -2, 2, 3, 4, 5, 6, 7,...