Commission J: Radio Astronomy (Novebber 2007 – October 2010)
Edited by H. Kobayashi
J1

Overview of Japanese radio astronomy activity

One of most important activities in Japanese radio astronomy is ALMA project, which is amillimeter and submillimeter large array with 80 telescopes at Atacama Desert of Chili. Japan
shares quarter burden for the construction and operation. In concrete terms, Japan has constructed
ACA (Atacama Compact Array), which consists of four 12-m telescopes and twelve 7-m
telescopes, and 3 band receiver cartridges for whole ALMA telescopes. The construction of
ALMA is succeeding and science observations have been started.
In the field of millimeter and submillimeter radio astronomy, ASTE telescope, which is a 10-m
submillimeter telescope at Atacama Desert, has started science observations. A large TES
bolometer array is used for simultaneously imaging the sky in the two bands (1100 and
850 micron). It discovered a cluster of galaxies, which show ultra star burst formation.
And Nobeyama 45-m telescope is continued for science observations and Nobeyama
millimeter array was closed for common use.
At the field of VLBI (Very Long Baseline Interferometer) researches, VERA (VLBI
Exploration of Radio Astrometry) was started to carry out a precise astrometry project to measure
the distance of galactic maser objects by using trigonometric parallax measurement technique. It
has revealed the structure of nearby spiral arm structure around the Sun. And a new VLBI
correlator is developed under the collaboration with NAOJ (National Astronomical Observatory ofJapan) and KASI (Korean Astronomy and Space Science Institute), which will be used for the East
Asian VLBI network observations.
Also Japanese VLBI network have started scienceobservations with 6, 8 and 22 GHz bands.
And NANTEN telescope, which is a 4-m submillimeter telescope at Chili, has made wide field
mapping observations of southern hemisphere sky.
On September 2007, SELENE satellite was launched, which is a lunar probe vehicle. In orderto make precise hypsographic map and gravity map of whole lunar globe, Japanese VLBI network
has used for the satellite tracking. It revealed the accurate gravitational field of the whole of themoon.
J2. ALMA
The Atacama Large Millimeter/submillimeter Array (ALMA) is most important project forJapanese radio astronomy. It is constructed and operated by Europe, Japan, and North America, in
cooperation with the Republic of Chile. ALMA is funded in Europe by the European Organization
for Astronomical Research in the Southern Hemisphere，in Japan by the National lnstitutes of
Natural Sciences(NINS) in cooperation with the Academia Sinica in Taiwan, and in North America
by the U.S. National Science Foundation (NSF) in cooperation with the National Research Councilof Canada (NRC). ALMA construction and operations are led on behalf of Europe by ESO，onbehalf of Japan by the National Astronomical 0bservatory of Japan (NAOJ), and on behalf of North
America by the National Radio Astronomy Observatory (NRAO). ALMA will have 54 12-m
telescopes and 12 7-m telescopes with 3-0.3 mm wavelength receivers.
East Asia shares the construction of Atacama Compact Array (ACA), which is a part of ALMAfor wide field and extended structure imagings. ACA consists of four 12-m telescopes and twelve

7-m telescopes. Also East Asia has been developing three bands receivers, which are 125-163GHz,
385-500GHz, and 780-950 GHz, and a correlator. Operation and data analysis software isdeveloping with international collaborations.
ALMA was succeded test observations at 230, 345, and 690 GHz with more than 10 telescopes.
They already showed the higest feasibilities of sensitivity and spatial resolution in millimeter andsubmillimeter arrays. And first science program with common use will start within 2011.
J3 .ASTEASTE is 12-m single dish telescope for millimeter and submillimeter observations. It has four
receivers, which are 350GHz/450GHz heterodyne receivers and the 270GHz/350GHz bolometer
camera. It made important scientific results for star busrt galaxies, galactic star forming regions
and others. ASTE discovered very active star burst galaxy at 11.5 Giga light-year distances,which shows 1000 time star formation than Milkyway galaxy. Also other star burst galaxies are
discovered. These results are important for understanding of the revolution of galaxies.
J4. VLBI
In the field of VLBI, Japan has mainly two activities. One is ground-based arrays, such as
VERA, JVN and EAVN. The other is a space-based project, which is VSOP-2. VERA aims tomeasure the trigonometric parallaxes for galactic maser sources and reveal real structure of the
Milkyway galaxy. VERA has started to observe more than 200 sources and determine the distanceand proper motions for around 50 sources. And neaby arm structure around Sun is decided. Also
JVN (Japanese VLBI Network) has started science observations, which consists of 12 VLBI
stations in Japan. Fine structure of jets and disks in star forming regions are revealed by 6.7GHz
methanol maser observations. And other high sentivity VLBI observations have been carried out.
Moreover EAVN (East Asian VLBI network) is started. Some test observations were done andfeasibility is checked between Japan, Korea and China. EAVN has around 20 VLBI stations,which is the biggest in the world. And new VLBI correlator is constructed by the interbational
collaborations between Japan and Korea. It has 16 stations correlations with 8Gbps data rate perstation, which is the biggest capability in the world. Space VLBI project, which is used space
radio telescope as a VLBI station, is started the project. 9-m deployment antenna, which is a key
instrument, met some difficulties. It is under the review of project by ISAS/JAXA.
J5. Others
Japan has many activities of radio astronomy. Hokakido University has a 11-m telescope for 22
GHz observations. NH3 observations for galactic sources are published. Ibaraki University is
operating two 32-m telescopes at Takahagi under the collaboration with NAOJ. They have 6, 8,
and 22 GHz receivers for single dish and VLBI observations.
National Institute ofCommunication and Trasmission (NICT) has a 32-m telescope at Kashima for VLBI. And NICT
has developed VLBI sampler, recorder and software correlator for geodesy VLBI. Geo-Survey
Institute (GSI) of Japan has a 32-m telescope at Tsukuba for geodesy VLBI, which is to keep theoriginal point in Japan. GSI has three 11-m telescopes for geodesy VLBI in Shitotsugawa, Aira,and Chichijima. Moreover Tsukuba University uses GSI 32-m telescope for astonomy usage at
22GHz. Institute of Space and Astronaitics Science (ISAS) has a 64-m telescope at Usuda, which
is mainly used for satellite tracking. It is used for VLBI. Waseda University has an 8-element
array with 20-m fixed telescopes at 1.4 GHz, which is mainly used for pulsar and transient sources.
Naogoya University has a 4-m submillimeter telescope at Atacama, which is called as NANTEN.

It made large survey of some star forming regions. Gifu University has a 11-m telescope at 8 and
22GHz, which is used for geodey VLBI and optical fiber VLBI experiments. Osaka Prefecture
University has a 1.85-m telescope at Nobeyama and an activity to develop new receivers. 6GHz
and 8GHz common polarized and receiver is developed and used at Takahagi and Shanghai
telescopes. Yamaguchi University is operating 32-m telescope at Yamaguchi with NAOJ, whichhas 6GHz and 8GHz receivers. It is used for single dish and VLBI obserbations and made someresults of methanol masers and active galactic nuclei sources. Kagoshima Univeristy iscollaborating with NAOJ for VERA. Period luminosity relation of Mira variables is deteming.
References and Abstracts

Abdo, A.A., M. Ackermann, M. Ajello, A. Axelsson, L. Baldini, J. Ballet, G. Barbielline, D.
Bastieri, B. M. Baughman, K. Bechtol, R. Bekkazzini, B. Berenji, E. D. Bloom, E. Bonamente,
A. W. Borgland, J. Bregeon, A. Brez, M. Brigida, P. Bruel, T. H. Burnett, G. A. Caliandro, R. A.
Cameron, P. A. Caraveo, J. M. Casandjian, E. Cavazzuti, C. Cecchi, Ö. Celik, A. Celotti, A.
Chekhtman, J. Chiang, S. Ciprini, R. Claus, J. Cohen-Tanugi, W. Collmar, J. Conrad, L.
Costamante, S. Cutini, A. de Angelis, F. de Palma, E. do Couto e Silva, P. S. Frell, D. Dumora,
C. Farnier, C. Favuzzi, S. J. Fegan, W. B. Focke, P. Fortin, L. Foschini, M. Frailis, L.
Fuhrmann, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, N. Gehrels, S. Germani, N. Giglietto,
F. Giordano, M. Giroletti, T. Glanzman, G. Godfrey, I. A. Grenier, IJ. E. Grove, L. Guillemot,
S. Guiriec, Y. Hanabata, E. Hays, R. E. Hughes, M. S. Jackson, G. Johannesson, A. S. Johnson,
W. N. Johnson, M. Kadler, T. Kamae, H. Katagiri, J. Kataoka, N. Kawai, M. Kerr, J.
Knodlseder, M. L. Kocian, M. Kuss, J. Lander, L. Latronico, F. Longo, F. Loparco, B. Lott, M.
N. Lovelette, P. Lubrano, G. M. Madejski, A. Makeev, W. Max-Moerbeck, M. N. Mazziotta, W.
McConville, J. E. McEnery, S. McGlynn, C. Meurer, P. F. Michelson, W. Mitthumsiri, T.
Mizuno, A. A. Moiseev, C. Monte, M. E. Monzani, A. Morselli, I. V. Moskalenko, I. Nestoras,
P. L. Nolan, J. P. Norris, E. Nuss, T. Ohsugi, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque,
D. Parent, V. Pavlidou, V. Pelassa, M. Pepe, M. Persc-Rollins, F. Piron, T. A. Porter, S. Raino,
R. Rando, M. Razzano, A. Readhead, O. Reimer, T. Reposeur, J. L. Richards, A. Y. Rodriguez,
M. Roth, F. Ryde, H. F. -W. Sadrozinski, D. Sanchez, A. Sander, P. M. Saz Parkinson, J. D.
Scargle, C. Sgro, M. S. Shaw, P. D. Smith, G. Spandre, P. Spinelli, M. S. Strickman, D. J.
Suson, G. Tagliaferri, H. Tajima, H. Takahashi, T. Tanaka, J. B. Thayer, J. G. Thayer, D. J.
Tho,pson, L. Tibaldo, O. Tibolla, D. F. Torres, G. Tosti, A. Tramacere, Y. Uchiyama, T. L.
Usher, V. Vasileiou, N. Vilchez, V. Vitale, A. P. Waite, P. Wang, A. E. Wehrle, B. L. Winer, K. S.
Wood, T. Ylinen, J. A. Zensus, M. Ziegler, M. (The Fermi/LAT Coolab.), E. Angelakis, C.
Bailyn, H. Bignall, J. Blanchard, E. W. Bonning, M. Buxton, R. Canterna, A. Carraminana, L.
Carrasco, F. Colomer, A. Doi, G. Ghisellini, M. Hauser, X. Hong, J. Isler, M. Kino, Y. Y.
Kovalev, Yu. A. Kovalev, T. P. Krichbaum, A. Kutyrev, A. Lahteenmaki, J. J. van Langevelde,
M. L. Lister, D. Macomb, L. Maraschi, N. Marchili, H. Nagai, Z. Paragi, C. Phillips, A. B.
Pushkarev, E. Recillas, P. Roming, M. Sekido, M. A. Stark, A. Szomoru, J. Tammi, F.
Tavecchio, M. Tornikoski, A. K. Tzioumis, C. M. Urry, and S. Wagner [2009],"Multiwavelength Monitoring of the Engimatic Narrow-Line Seyfert 1 PMN J0948+0022 inMarch-July 2009," Astrophys. J., vol.707, pp.727-737.
Following the recent discovery of γ-rays from the radio-loud narrow-line Seyfert 1 galaxy
PMN J0948+0022 (z = 0.5846), we started a multiwavelength campaign from radio toγ-rays,
which was carried out between the end of 2009 March and the beginning of July. The source
displayed activity at all the observed wavelengths: a general decreasing trend from optical
toγ-ray frequencies was followed by an increase of radio emission after less than two months
from the peak of theγ-ray emission. The largest flux change, about a factor of about 4,

occurred in the X-ray band. The smallest was at ultraviolet and near-infrared frequencies,
where the rate of the detected photons dropped by a factor 1.6-1.9. At optical wavelengths,
where the sampling rate was the highest, it was possible to observe day scale variability, withflux variations up to a factor of about 3. The behavior of PMN J0948+0022 observed in thiscampaign and the calculated power carried out by its jet in the form of protons, electrons,
radiation, and magnetic field are quite similar to that of blazars, specifically of flat-spectrum
radio quasars. These results confirm the idea that radio-loud narrow-line Seyfert 1 galaxies
host relativistic jets with power similar to that of average blazars.
Abdo, A. A., M. Ackermann, M. Ajello, M. Axelsson, L. Baldini, J. Ballet, G. Barbiellini, D.
Bastieri, B. M. Baughman, K. Bechtol, R. Bellazzini, B. Berenji, R. D. Blandford, E. D.
Bloom, D. C.-J. Bock, J. R. Bogart, E. Bonamente, A. W. Borgland, A. Bouvier, J. Bregeon, A.
Brez, M. Brigida, P. Bruel, T. H. Burnett, S. Buson, G. A. Caliandro, R. A. Cameron, P. A.
Caraveo, J. M. Casandjian, E. Cavazzuti, C. Cecchi, O. Celik, A. Chekhtman, C. C. Cheung, J.
Chiang, S. Ciprini, R. Claus, I. Cognard, J. Cohen-Tanugi, W. Collmar, L. R. Cominsky, J.
Conrad, S. Corbel, R. Corbet, L. Costamante, S. Cutini, C. D. Dermer, A. de Angelis, F. dePalma, S. W. Digel, E. E. Silva Do Couto, P. S. Drell, R. Dubois, D. Dumora, C. Farnier, C.
Favuzzi, S. J. Fegan, E. C. Ferrara, W. B. Focke, P. Fortin, M. Frailis, L. Fuhrmann, Y.
Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Gehrels, S. Germani, B. Giebels,
N. Giglietto, P. Giommi, F. Giordano, M. Giroletti, T. Glanzman, G. Godfrey, I. A. Grenier, J.
E. Grove, L. Guillemot, S. Guiriec, Y. Hanabata, A. K. Harding, M. Hayashida, E. Hays, D.
Horan, R. E. Hughes, G. Iafrate, R. Itoh, M. S. Jackson, G. Johannesson, A. S. Johnson, R. P.
Johnson, W. N. Johnson, M. Kadler, T. Kamae, H. Katagiri, J. Kataoka, N. Kawai, M. Kerr, J.
Knodlseder, M. L. Kocian, M. Kuss, J. Lande, S. Larsson, L. Latronico, M. Lemoine-Goumard,
F. Longo, F. Loparco, B. Lott, M. N. Lovellette, P. Lubrano, J. Macquart, G. M. Madejski, A.
Makeev, W. Max-Moerbeck, M. N. Mazziotta, W. McConville, J. E. McEnery, S. McGlynn, C.
Meurer, P. F. Michelson, W. Mitthumsiri, T. Mizuno, A. A. Moiseev, C. Monte, M. E. Monzani,
A. Morselli, I. V. Moskalenko, S. Murgia, I. Nestoras, P. L. Nolan, J. P. Norris, E. Nuss, T.
Ohsugi, A. Okumura, N. Omodei, E. Orlando, J. F. Ormes, D. Paneque, J. H. Panetta, D.
Parent, V. Pavlidou, T. J. Pearson, V. Pelassa, M. Pepe, M. Pesce-Rollins, F. Piron, T. A. Porter,
S. Raino, R. Rando, A. Readhead, M. Razzano, A. Reimer, O. Reimer, T. Reposeur, L. C.
Reyes, J. L. Richards, L. S. Rochester, A. Y. Rodriguez, M. Roth, F. Ryde, H. F.-W.
Sadrozinski, D. Sanchez, A. Sander, P. M. Saz Parkinson, D. Scargle, C. Sgro, M. S. Shaw, C.
Shrader, E. J. Siskind, D. A. Smith, P. D. Smith, G. Spandre, P. Spinelli, L. Stawarz, M.
Stevenson, M. S. Strickman, D. J. Suson, H. Tajima, H. Takahashi, T. Takahashi, T. Tanaka, G.
B. Taylor, J. B. Thayer, J. G. Thayer, D. J. Thompson, L. Tibaldo, D. F. Torres, G. Tosti, A.
Tramacere, Y. Uchiyama, T. L. Usher, V. Vasileiou, N. Vilchez, V. Vitale, A. P. Waite, P. Wang,
A. E. Wehrle, B. L. Winer, K. S. Wood, T. Ylinen, J. A. Zensus, M. Ziegler, M., (TheFermi-Lat Collaboration), M. Uemura, Y. Ikejiri, K. S. Kawabata, M. Kino, K. Sakimoto, M.
Sasada, S. Sato, M. Yamanaka, M. Villata, C. M. Raiteri, I. Agudo, H. D. Aller, M. F. Aller, E.
Angelakis, A. A. Arkharov, U. Bach, E. Benitez, A. Berdyugin, D. A. Blinov, M. Boettcher, C.
S. Buemi, W. P. Chen, M. Dolci, D. Dultzin, N. V. Efimova, M. A. Gurwell, C. Gusbar, J. L.
Gomez, J. Heidt, D. Hiriart, T. Hovatta, S. G. Jorstad, T. S. Konstantinova, E. N. Kopatskaya,
E. Koptelova, O. M. Kurtanidze, A. Lahteenmaki, V. M. Larionov, E. G. Larionova, P. Leto, H.
C. Lin, E. Lindfors, A. P. Marscher, I. M. McHardy, D. A. Melnichuk, M. Mommert, K.
Nilsson, A. Paola, di, R. Reinthal, G. M. Richter, M. Roca-Sogorb, P. Roustazadeh, L. A. Sigua,
L. O. Takalo, M. Tornikoski, C. Trigiglio, I. S. Troitsky, G. Umana, C. Villforth, K. Grainge, R.
Moderski, K. Nalewajko, and M. A. Sikora [2010], "A Change in the Optical Polarization
Associated with a -Ray Flare in the Blazar 3C 279," Nature, vol.463, pp.919-923.
It is widely accepted that strong and variable radiation detected over all accessible energy

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bands in a number of active galaxies arises froma relativistic, Doppler-boosted jet pointing
close to our line of sight1. The size of the emitting zone and the location of this region relative
to the central supermassive black hole are, however, poorly known, with estimates ranging
from light-hours to a light-year or more. Here we report the coincidence of a gamma (c)-rayflare with a dramatic change of optical polarization angle. This provides evidence forco-spatiality of optical and c-ray emission regions and indicates a highly ordered jet magnetic
field. The results also require a non-axisymmetric structure of the emission zone, implying a
curved trajectory for the emitting material within the jet, with the dissipation region located at
a considerable distance from the black hole, at about 105 gravitational radii.
Abramov-Maximov, V. E., G. B. Gelfreikh, N. I. Kobanov, and K. Shibasaki [2009], "A
Comparison of Parameters of 3-minute and 5-minute Oscillations in Sunspots From
Synchronous Microwave and Optical Observations," Proc. of the IAU Symp. 257, "Universal
Heliophysical Processes", eds. N. Gopalswamy and David F. Webb, pp.95-99.
The observations of 3 and 5 minute oscillations in sunspots present information on propagationof MHD waves in the magnetic tubes of sunspots. We present a comparison of wavelet spectraof radio flux oscillations at= 1.76 cm and oscillations of longitudinal component of thevelocity at the chromosphere in sunspot umbra and penumbra in AR 10661 (2004, Aug 18).
The radio maps of the Sun obtained with the Nobeyama Radioheliograph were used. The
spatial resolution of the radio data was about 10-15 arcsec, and 10 sec cadence was used. On
the radio maps sunspot-associated sources were identified and time profiles of their maximum
brightness temperatures for each radio source were calculated. Radio data consists of
information of oscillations of plasma parameters (in the regions with magnetic field B = 2000G) at the level of the chromosphere-corona transition region. The optical observations werecarried out at Sayan observatory. These data included information on longitude component of
the magnetic field at the photosphere (line Fe I 6569Å and longitudinal component of thevelocity at the chromosphere (line Hα was used). Comparing the wavelet diagrams covering
the same periods of observations at radio and optics showed that some wave trains of time
profiles are very similar in both kinds of observations (similar oscillation frequencies and theirdrifts, variations of amplitudes), however, some significant differences were also registered.
The best similarity in optical and radio oscillations was found when the active region (AR) wasnear the center of the solar disk. The phase shifts between the two kinds of observations
reflecting the propagation of MHD waves were also analyzed.
Adams, M., H. J. Boffin, W. Garnier, and D. Iono [2008], "The Global ALMA EPO
Programme: Communicating Astronomy with the Public at Millimetre and Submillimetre
Wavelengths," Commnicating astronomy with the public 2007 : Proceedings from the
IAU/National Observatory of Athens/ESA/ESO Conference, eds. Christensen, L. L., Zoulias,
M., and Robson, I., pp.288-293.
The Atacama Large Millimeter/submillimeter Array (ALMA) is a major 21st century
international science research facility that will open new windows on celestial origins. ALMA
construction is underway in the high-elevation Atacama Desert of northern Chile. Science
operations will begin in 2010, and full science operations will start in 2013. The ALMA
Education and Public Outreach (EPO) programme is a global collaboration that seeks tocommunicate the excitement and value of the ALMA mission, science, and technology tointernational audiences effectively. The ALMA EPO programme is the responsibility of the
Joint ALMA Observatory (JAO), the National Radio Astronomy Observatory (NRAO), theEuropean Organisation for Astronomical Research in the Southern Hemisphere (ESO), and the
National Astronomical Observatory of Japan (NAOJ). This contribution provides an overview
of the ALMA Project and the global ALMA EPO programme.
Araki, H., S. T. Tazawa, H. Noda, Y. Ishihara, E. M. Migita, S. Sasaki, N. K. Kawano, I. K.

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Kamiya, and J. Oberst [2008a], "Present Status and Preliminary Results of the Lunar
Topography by Kaguya-LALT Mission," 39th Lunar and Planetary Science Conference,(Lunar and Planetary Science XXXIX), held March 10-14, 2008 in League City, Texas. LPI
Contribution No. 1391., p.1510.
We report present status and the first results from the laser altimeter (LALT) on Kaguya(SELENE) lunar explorer. LALT started its observations on December 30, 2007. New, but
preliminary, lunar topography will be obtained after two months observation by LALT.
Araki, H., S. Tazawa, H. Noda, T. Tsubokawa, N. Kawano, and S. Sasaki [2008b],"Observation of the Lunar Topography by the Laser Altimeter LALT on Board Japanese Lunar
Explorer SELENE," Adv. Sp. Res., vol.42, pp.317-322.
The SELENE Laser Altimeter (LALT) is designed to map the Moon’s topography and will belaunched in summer 2007. LALT incorporates Q-switched Cr doped Nd:YAG laser (1064 nm)with an output energy of 100 mJ and 1 Hz repetition frequency for about one year mission
period. The laser pulse travels to the Moon's surface and reflections from the surface aredetected by a silicon avalanche photo-diode. The ranging distance is 50-150 km with about 5
m accuracy. Several corrections for accurate ranging data are investigated. The flight hardware
has been qualified and passed all the integration tests. A principal goal of the LALT instrument
is to obtain a much more detailed lunar topographic map which is superior in global coverage,measurement accuracy and number of data points to previous observations and models. The
overall science objectives of LALT are (1) determination of lunar global figure, (2) internal
structure and surface processes, (3) exploration of the lunar pole regions, and (4) reduction oflunar occultation data.
Araki, H., S. Sasaki, H. Noda, S. Tazawa, Y. Ishihara, E. Migita, N. Kawano, I. Kamiya, and J.
Oberst [2008c], "Global Lunar Topography by LALT (Laser Altimeter) on Board Kaguya,"
Meteoritics and Planetary Sci. Suppl., vol.43, paper id. 5230.
Not Available
Araki, H., Y. Ishihara, H. Noda, S. Goossens, S. Tazawa, N. Kawano, S. Sasaki, and J. Oberst[2008d], "A New Lunar Topographic Map of the Moon by KAGUYA-LALT: The First Precise
Topography of the Polar Regions," American Geophysical Union, Fall Meeting 2008, abstract#P13E-04.
The Japanese lunar explorer KAGUYA (SELENE) was launched successfully on September
14th, 2007. A laser altimeter (LALT) is on board the main orbiter of KAGUYA. The objectivesof LALT are (1) determination of lunar global figure, (2) studies in internal structure andsurface processes, (3) exploration of the lunar pole regions, and (4) reduction of lunar
occultation data. LALT transmits laser pulses whose time width is about 20 nano-seconds andpulse interval is 1 second. Range accuracy is up to 5m. The range data are transformed to the
topography of the moon with the aid of position and attitude data of the main orbiter. From theend of December 2007, LALT started continuous operation and a global topography map with
unprecedented resolution was produced. Lunar mean radius is estimated as 1737.15±0.01 km
and the COM-COF offset is 1.94 km based on the spherical harmonic model STM359_grid-02
derived from LALT topography. The amplitude of the power spectrum of STM359_grid-02 islarger than that of the previous model at L>30 degrees, which may reflect the process of basinformation and/or crustal evolution. In the polar regions where previous CLEMENTINE
altimeter did not cover, many topographic features that were difficult to see on the imagery
from spacecraft or ground based radar are discovered. The sunlit rate in the lunar polar regions
is estimated by using the polar topographic map made from LALT topography. We found thati) the highest sunlit rate is 93~96 % in both polar regions and ii) the eternal shadow area issmaller than previous estimations. These results will be of great use for the planning of thelunar polar exploration in near future.

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Araki, H., S. Tazawa, H. Noda, Y. Ishihara, S. Goossens, S. Sasaki, N. Kawano, I. Kamiya, H.
Otake, J. Oberst, and C. Shum [2009a], "Lunar Global Shape and Polar Topography Derived
from Kaguya-LALT Laser Altimetry," Science, vol.323, pp.897-900.
A global lunar topographic map with a spatial resolution of finer than 0.5 degree has been
derived using data from the laser altimeter (LALT) on board the Japanese lunar explorer
Selenological and Engineering Explorer (SELENE or Kaguya). In comparison with theprevious Unified Lunar Control Network (ULCN 2005) model, the new map reveals unbiased
lunar topography for scales finer than a few hundred kilometers. Spherical harmonic analysisof global topographic data for the Moon, Earth, Mars, and Venus suggests that isostaticcompensation is the prevailing lithospheric support mechanism at large scales. However,
simple rigid support is suggested to dominate for the Moon, Venus, and Mars for smaller scales,
which may indicate a drier lithosphere than on Earth, especially for the Moon and Venus.
Araki, H., S. Tazawa, H. Noda, Y. Ishihara, S. Goossens, N. Kawano, S. Sasaki, I. Kamiya, H.
Otake, J. Oberst, and C. K. Shum [2009b], "The Lunar Global Topography by the Laser
Altimeter (LALT) Onboard Kaguya (SELENE): Results from the One Year Observation," 40th
Lunar and Planetary Science Conference, (Lunar and Planetary Science XL), held March
23-27, 2009 in The Woodlands, Texas, id.1432.
A global and precise topographic map of the Moon has been derived by the laser altimeter(LALT) onboard the Japanese lunar explorer Kaguya (SELENE). Results of the one year
observation and implications from the LALT topography will be presented.
Araki, H., S. Tazawa, H. Noda, E. Migita, I. Kamiya, N. Kawano, and S. Sasaki [2010],"Preliminary Results of Lunar Topography by KAGUYA-LALT Mission," Trans. of Sp. Tech.
Japan, vol.7, pp.Tk23-Tk25.
The Laser Altimeter (LALT) on board the main orbiter of KAGUYA (SELENE) started
nominal observation on December 30, 2007 for mapping the lunar topography. As of March 31,
2008, LALT has obtained about 6.7 million topographic data and the return rate is 97%.
Several qualifications of the data to produce reliable topography are now in progress. The
present status and preliminary results are reported in this article.
Asada, K., A. Doi, M. Kino, H. Nagai, M. Nakamura, S. Kameno, and VSOP-2 Science
Working Group [2009a], "VSOP-2 Observations of M 87: A Proposal for a VSOP-2 Key
Science Program," Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y.,
ASP Conf. Ser. vol.402, pp.262-265.
We report the advantages and potentials of VSOP-2 observations for studying the central
engine of M 87. Extremely high angular resolution of VSOP-2 of 38μ-arcsecond will provide
us the unique opportunity to observe M 87 with spatial resolution of 0.0031 pc. This
corresponds to around 10 times the Schwarzschild radius so that VSOP-2 can be a powerfultool to reveal the accretion disk and jet launching site, and investigate the formation,
acceleration and collimation of the jet in connection with the physics of the accretion disk. A
polished plan based on these studies will be proposed as one of the Key Science Programs of
VSOP-2 mission in the category of Active Galactic Nuclei.
Asada, K., S. Kameno, Z.-Q. Shen, H. Shinji, D. C. Gabuzda, and M. Inoue [2009b], "3C 84
Expanding Radio Lobe Revealed by VSOP Observations," Proc. of the "Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara,
Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.91-95.
We report the detection of the expansion and inner proper motions of a young radio lobe
associated with the bright radio source 3C 84 in the Seyfert galaxy NGC 1275 using
multi-epoch VSOP observation. The observed inner proper motions are consistent with theevolution scenario of classical double radio sources. The apparent expansion velocity is

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0.50±0.09 c, and the age of radio lobe is estimated to be 45.7±8.9 years in 2001. The total flux
density at 5 GHz increased at the end of the 1950’s, with several peaks in the middle of the
1980’s, and is in a decay phase now. The decay of total flux density can be naturally explainedby an adiabatic cooling due to the expansion of the radio lobe, and previously measured
spectral indices suggest that the emission comes from the surface of the radio lobe.
Asai, A., K. Shibata, H. Hara, and N. Nitta [2008a], "Characteristics of Anemone Active
Regions Appearing in Coronal Holes Observed with the Yohkoh Soft X-Ray Telescope,"
Astrophys. J., vol.673, pp.1188-1193.
Coronal structure of active regions appearing in coronal holes is studied, using data that wereobtained with the Soft X-Ray Telescope (SXT) aboard Yohkoh between 1991 November and1993 March. The following characteristics are found. Many of the active regions (ARs)appearing in coronal holes show a structure that looks like a sea anemone. Such active regions
are called anemone ARs. About one-fourth of all active regions that were observed with SXT
from their births showed the anemone structure. For almost all the anemone ARs, the order ofthe magnetic polarities is consistent with the Hale-Nicholson polarity law. These anemone ARsalso showed, to a greater or lesser extent, an east-west asymmetry in the X-ray intensity
distribution, such that the following (eastern) part of the AR was brighter than its preceding(western) part. This, as well as the anemone shape itself, is consistent with the magnetic
polarity distribution around the anemone ARs. These observations also suggest that an active
region appearing in coronal holes has a simpler (less sheared) and morepreceding-spot-dominant magnetic structure than those appearing in other regions.
Asai, A., H. Hara, T. Watanabe, S. Imada, T. Sakao, N. Narukage, J. L. Culhane, and G. A.
Doschek [2008b], "Strongly Blueshifted Phenomena Observed with {¥it Hinode}/EIS in the2006 December 13 Solar Flare," Astrophys. J., vol.685, pp.622-628.
We present a detailed examination of strongly blueshifted emission lines observed with the
EUV Imaging Spectrometer on board the Hinode satellite. We found two kinds of blueshifted
phenomenon associated with the X3.4 flare that occurred on 2006 December 13. One wasrelated to a plasmoid ejection seen in soft X-rays. It was very bright in all the lines used for theobservations. The other was associated with the faint arc-shaped ejection seen in soft X-rays.
The soft X-ray ejection is thought to be a magnetohydrodynamic (MHD) fast-mode shock
wave. This is therefore the first spectroscopic observation of an MHD fast-mode shock wave
associated with a flare.
Asai, A., H. Nakajima, M. Shimojo, T. Yokoyama, S. Masuda, and S. Krucker [2009],"Imaging Spectroscopy on Preflare Coronal Nonthermal Sources Associated with the 2002
July 23 Flare," Astrophys. J., vol.695, pp.1623-1630.
We present a detailed examination on the coronal nonthermal emissions during the preflarephase of the X4.8 flare that occurred on 2002 July 23. The microwave (17 GHz and 34 GHz)
data obtained with Nobeyama Radioheliograph, at Nobeyama Solar Radio Observatory and thehard X-ray (HXR) data taken with RHESSI obviously showed nonthermal sources that arelocated above the flare loops during the preflare phase. We performed imaging spectroscopic
analyses on the nonthermal emission sources both in microwaves and in HXRs, and confirmedthat electrons are accelerated from several tens of keV to more than 1 MeV even in this phase.
If we assume the thin-target model for the HXR emission source, the derived electron spectral
indices (~4.7) is the same value as that from microwaves (~4.7) within the observational
uncertainties, which implies that the distribution of the accelerated electrons follows a single
power law. The number density of the microwave-emitting electrons is, however, larger thanthat of the HXR-emitting electrons, unless we assume low-ambient plasma density of about
1.0x109 cm-3 for the HXR-emitting region. If we adopt the thick-target model for the HXR
emission source, on the other hand, the electron spectral index (~6.7) is much different, while

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the gap of the number density of the accelerated electrons is somewhat reduced.
Asaki, Y., S. Deguchi, H. Imai, K. Hachisuka, M. Miyoshi, and M. Honma [2008],"Measurements of Annual Parallaxes and Proper Motions of the Red Supergiant S Per," Proc.
of the IAU Symp. 242, "Astrophysical Masers and their Environments", eds. Jessica Chapman
and Willem Baan, pp.378-380.
VLBI phase-referencing monitoring of water vapor masers around the red supergiant, S Per,
was conducted over four years. We successfully obtained proper motions and an annual
parallax of the masers and determined the distance to S Per of 2.51±0.09 kpc. The propermotion of the star itself was inferred from the maser proper motions, and it was -0.38 and -1.54
mas/yr for right ascension and declination, respectively. Assuming the distance from the sun to
the Galactic center, R0, of 8.5 kpc and the rotation velocity around the sun, θ0, of 220 km/s, theGalactic rotation velocity around S Per is 200 km/s.
Asaki, Y., and Y. Kono [2009a], "VSOP-2 Astrometric Accuracy with Phase Referencing,"
Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser.
vol.402, pp.435-440.
The VSOP-2 mission is expected to conduct phase referencing observations with theunprecedented spatial resolutions at 8.4, 22, and 43 GHz together with the ASTRO-G satellite.
In this report, VSOP-2 astrometry with phase referencing is examined in detail based on asimulation tool, ARIS.
Asaki, Y., and M. Miyoshi [2009b], "A Future Submillimeter-Wave Space VLBI," Proc. of the"Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies",
eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402,
pp.431-434.
Submillimeter-wave VLBI is a very attractive idea for future radio astronomy. We discuss asubmillimeter space VLBI based on the simulation of (u, v) coverage. We assume observations
using three terrestrial submillimeter telescopes and one telescope in a sun-synchronous
low-Earth orbit. The simulated array gives a well-filled (u, v) coverage for a specified source.
However, the (u, v) coverage becomes much poorer if real-time VLBI data transfer from thesatellite to the ground is needed even with a telemetry network with seven ground stations.
Alternative methods for the VLBI data acquisition from the space telescope will be required
for the proposed space VLBI.
Asayama, S., S. Kawashima, H. Iwashita, T. Takahashi, M. Inata, Y. Obuchi, T. Suzuki, and T.
Wada [2008], "Design and Development of ALMA Band 4 Cartridge Receiver," Proc. of the
19th International Symposium on Space THz Technology, ed. Wolfgang Wild, pp.244-249.
This paper describes the design and development of the ALMA Band 4 cartridge receiver.
Band 4 is one of the ten bands that will form the ALMA Front End Receiver. It receives
radiation in the 125-163 GHz frequency range in two orthogonal polarizations anddown-converts the sideband separated signals to intermediate frequencies between 4 and 8
GHz.
Asayama, S., and M. Kamikura [2009], "Development of Double-Ridged Waveguide
Orthomode Transducer for the 2 MM Band," J. IR., Millimeter, and Terahertz Waves, vol.30,
pp.573-579.
This paper describes the design and development of the 2 mm band orthomode transducer(OMT) for the Band 4 cartridge receivers of the Atacama Large Millimeter/Submillimeter
Array (ALMA). The OMT consists of a double-ridged waveguide followed by a B ifot typejunction with a main arm and two side arms. The main arm output is a multi-section steptransformer followed by an E-plane bend and an oval waveguide to be realized the OMT witha two-split block using conventional Computer Numerical Control (CNC) milling techniques.

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The prototype OMT shows return loss of better than 20 dB, cross polarization coupling of
better than 30 dB and insertion loss of less than 0.4 dB across 125 - 163 GHz. Furthermore,production feasibility was demonstrated through the evaluation of seven OMTs with aproduction design. The design of the developed OMT is so simple that it is easily scaled tosubmillimeter frequencies.
Baba, J., Y. Asaki, J. Makino, M. Miyoshi, R. Takahashi, T. R. Saitoh, and K. Wada [2009],"The Origin of Large Reculiar Motions of Star-Forming Regions and Spiral Structures of Our
Galaxy," Astrophys. J., vol.706, pp.471-481.
Recent Very Long Baseline Interferometer (VLBI) observations determined the distances andproper motions of star-forming regions in spiral arms directly. They showed that star-forming
regions and young stars have large peculiar motions as large as 30 km s-1 with complex
structures. Such a large peculiar motion is incompatible with the prediction of the standard
theory of quasi-stationary spiral arms. We use a high-resolution, self-consistentN-body+hydrodynamical simulation to explore how the spiral arms are formed and maintained,
and how star-forming regions move. We found that arms are not quasi-stationary but transientand recurrent, as suggested in alternative theories of spiral structures. Because of this transient
nature of the spiral arms, star-forming regions exhibit a trend of large and complex
non-circular motions, which is qualitatively consistent with the VLBI observations. Owing tothis large non-circular motion, a kinematically estimated gas map of our Galaxy has large
systematic errors of ~2-3 kpc in the distance from the Sun.
Bakunina, I. A., V. E. Abramov-Maximov, S. V. Lesovoy, K. Shibasaki, A. A. Solov'ev, and Yu.
V. Tikhomirov, [2009], "Long Period Oscillations of Microwave Emission of Solar Active
Regions: Observations with NoRH and SSRT," Proc. of the IAU Symp. 257, "Universal
Heliophysical Processes", eds. N. Gopalswamy and David F. Webb, pp.155-157.
In this work we present the first results of study and comparison of the parameters ofquasi-periodic long-term oscillations of microwave emission of large (>0.7 arcmin) sunspots
as a result of simultaneous observations with two radioheliographs ﾐ NoRH (17 GHz) and
Siberian Solar Radio Telescope (SSRT) (5.7 GHz) with 1 minute cadence. Radioheliographs
have been working with quite large time overlap (about 5 hours) and have the high spatial
resolution: 10 arcsec (NoRH) and 20 arcsec (SSRT). We have found that quasi-periodic
long-term oscillations are surely observed at both frequencies with the periods in the range of
20–150 min. We detected common periods for common time of observations with two
radioheliographs and interpret this as the consequence of the vertical-radial quasi-periodic
displacements of sunspot as a whole structure.
Barnes, P. J., Y. Yonekura, S. D. Ryder, A. M. Hopkins, Y. Miyamoto, N. Furukawa, and Y.
Fukui [2010], "Discovery of Large-Scale Gravitational Infall in a Massive Protostellar
Cluster," Mon. Not. Roy. Astron. Soc., vol.402, pp.73-86.
We report Mopra Australia Telescope National Facility (ATNF), Anglo-Australian Telescopeand Atacama Submillimeter Telescope Experiment observations of a molecular clump in
Carina, BYF73 = G286.21+0.17, which give evidence of large-scale gravitational infall in thedense gas. From the millimetre and far-infrared data, the clump has a mass of ∼2 × 104 M∼,
luminosity of ∼2–3 × 104 L∼ and diameter of ∼0.9 pc. From radiative transfer modelling, wederive a mass infall rate of ∼3.4 × 10−2 M∼ yr−1. If confirmed, this rate for gravitational infall
in a molecular core or clump may be the highest yet seen. The near-infrared K-band imaging
shows an adjacent compact H ii region and IR cluster surrounded by a shell-likephotodissociation region showing H2 emission. At the molecular infall peak, the K imaging
also reveals a deeply embedded group of stars with associated H2 emission. The combinationof these features is very unusual, and we suggest that they indicate the ongoing formation of a
massive star cluster. We discuss the implications of these data for competing theories of

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massive star formation.
Bridger, A., D. Clarke, N. P. F. Lorente, H. Yatagai, M. Scgilling, L. Testi, and R. H. Warmels[2008], "ALMA Observing Tool," Proc. of the SPIE, vol.7019, pp.70190R-1-12.
We present a report on the current development status of the ALMA Observing Tool,
describing how the tool operates as an integrated environment for proposal and program
preparation. The paper also covers the science-oriented graphical tools for both spatial andspectral setup, their system-oriented equivalents, local oscillator and correlator setup assistants
as well as program validation.
Bronfman, L. [2008a], "Massive Star Formation in the Southern Milky Way. From Large Scale
Surveys to High Resolution Observations," Asttrophys. and Sp. Sci., vol.313, pp.81-85.
During the past decade we have compiled a large molecular line data base of massive star
forming regions in the southern Milky Way. These regions are confined into giant molecular
clouds that trace the galactic spiral arms. Their radial distribution has a pronounced peak
midway between the Sun and the galactic center, which in the IV quadrant corresponds to thelocation of the Norma Spiral arm. We study in some detail one of the foremost regions ofmassive star formation in the Norma arm, using millimeter continuum and line emission maps
obtained with the SEST, APEX, and ASTE telescopes. It is a multiple system evolving along acomplete GMC core, candidate for future ALMA observations.
Bronfman, L., G. Garay, M. Merello, D. Mardones, J. May, K. J. Brooks, L.-A. Nyman, and R.
Gusten [2008b], "Discovery of an Extremely High Velocity, Massive, and Compact Molecular
Outflow in Norma," Astrophys. J., vol.672, pp.391-397.
G331.5-0.1 in the Norma spiral arm is one of the most luminous and extended cores of a giant
molecular cloud (GMC), containing at least six massive and dense dust condensations. Here
we report the discovery, from observations of several submillimeter molecular lines that weremade using the Atacama Submillimeter Telescope (ASTE) and the Atacama Pathfinder
Experiment Telescope (APEX), of an unresolved, extremely high velocity molecular outflow
toward the brightest and most massive dust condensation. The outflow is massive andenergetic (flow mass of ~55 Msolar momentum of ~2.4x103 Msolar km s-1 kinetic energy of~1.4x1048 ergs). These values are characteristic of flows driven by young massive stellar
objects with Lbol~1x105 Lsolar. We also report the detection, using the Australia Telescope
Compact Array (ATCA), of a compact radio continuum source that is located at the center ofthe outflow and therefore likely to be its driving energy source. It has an spectral index
between 4.8 and 8.6 GHz of 1.1±0.2, suggesting that it might correspond to a collimated jet.
Bussey, D. B. J., J. A. McGovern, P. D. Spudis, C. Neish, S. Sorensen, H. Noda, and Y.
Ishihara [2010], "Lunar Polar Illumination Conditions Derived Using Kaguya Laser Data," LPI
Contribution No. 1533, p.2293.
We have used the Kaguya laser-derived topography data to fully characterize the lunar polar
illumination conditions. We have generated illumination profiles for the areas that receive themost illumination.
Choi, M., and K. Tatematsu [2009], "Protostellar Accretion Disks for the NGC 1333 IRAS 4A
Binary System," Proc. of the "Exoplanets and disks: their formation and diversity", eds. Usuda,T., Tamura, M., and Ishii, M., AIP Conf. Proc., vol.1158, pp.117-118.
We present the results of radio imaging observations of the NGC 1333 IRAS 4A protobinary in
the ammonia (2, 2) and (3, 3) lines and in the 1.3 cm continuum. Both ammonia andcontinuum maps show two compact sources, accretion disks of Al and A2. Interestingly, the A2
disk is brighter in the ammonia lines but dimmer in the dust continuum than its sibling disk.
This difference suggests that the disks have surprisingly dissimilar characters, one gas-rich andthe other dusty. If such a condition can persist until the planet-forming phase of the disk
evolution, planetary systems produced in such disks may look very different from each other.

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Choi, Y. K., T. Hirota, M. Honma, and H. Kobayashi [2008a], "Astrometry of Red Supergiant
VY Canis Majoris with VERA," Proc. of the IAU Symp. 248, "A Giant Step: from Milli- to
Micro-arcsecond Astrometry", eds. Wenjing Jin, Imants Platais, Michael A. C. Perryman,
pp.192-193.
We present observational results on the red supergiant VY Canis Majoris with VERA. We haveobserved 22 GHz H2O masers and 43 GHz SiO masers (v=1 and 2 J=1-0) around VY CMa for
13 months. We succesfully detected a parallax of 0.87±0.08 mas, corresponding to the distanceof 1.15 +0.10-0.09 kpc using H2O masers. As the result of phase-referencing analyses, we havemeasured absolute positions for both H2O masers and SiO masers. The H2O maser features
show rapid expansion off the central star.
Choi, Y. K., T. Hirota, M. Honma, H. Kobayashi, T. Bushimata, H. Imai, K. Iwadate, T. Jike, S.
Kameno, O. Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, M. K. Kim, S. Kuji,
T. Kurayama, S. Manabe, K. Maruyama, M. Matsui, N. Matsumoto, T. Miyaji, T. Nagayama, A.
Nakagawa, K. Nakamura, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, T. Sasao, K. Sato, M.
Sato, K. M. Shibata, Y. Tamura, M. Tsushima, and K. Yamashita [2008b], "Distance to VY
Canis Majoris with VERA," Publ. Astron. Soc. Japan, vol.60, pp.1007-1012.
We report on astrometric observations of H2O masers around the red supergiant VY Canis
Majoris carried out with VLBI Exploration of Radio Astrometry (VERA). Based on
astrometric monitoring for 13 months, we successfully measured a trigonometric parallax of
0.88±0.08 mas, corresponding to a distance of 1.14 +0.11-0.09 kpc. This is the most accurate
determined distance to VY CMa and the first one based on an annual parallax measurement.
The luminosity of VY CMa has been overestimated due to a previously accepted distance.
With our result, we re-estimate the luminosity of VY CMa to be (3±0.5) x 105 Lsun using thebolometric flux integrated over optical and IR wavelengths. This improved luminosity value
makes the location of VY CMa on the Hertzsprung-Russel (HR) diagram much closer to thetheoretically allowable zone (i.e. the left side of the Hayashi track) than previous ones, though
the uncertainty in the effective temperature of the stellar surface still does not permit us tomake a final conclusion.
Choi, Y. K., T. Hirota, M. Honma, and H. Kobayashi [2008c], "Distance to VY Canis Majoris
with VERA," Proc. of the 9th European VLBI Network Symposium on The role of VLBI in
the Golden Age for Radio Astronomy and EVN Users Meeting, September 23-16, 2008,
Bologna, Italy, pp.57-62.
We report on observational results of H2O and SiO (J=1 0, v=1 and v=2) masers around VY
Canis Majoris (VYCMa) carried out with VERA for 13 months. Our astrometric monitoringmeasured a parallax of 0.88±0.08 mas, and it corresponds to a distance of 1.14+0.11-0.09 kpc.
This is the first trigonometric parallax measurement for VY CMa. Using our newly obtained
distance with a high accuracy, the luminosity of VY CMa was re-estimated to be (3±0.5) × 105
L∼. This improved luminosity is more consistent with the theoretical evolutionary model thanprevious values. Moreover, we considered 3-dimensional structure and kinematics of thecircumstellar envelopes around VY CMa with propermotions and absolute positions of the
H2O and SiO masers. The 3-dimensional structures and kinematics suggest a bipolar out ﾟ ow
around VY CMa along the line of sight.
Choi, Y. K., T. Hirota, M. Honma, and H. Kobayashi [2009], "Astrometry of the Red
Supergiant Star VY Canis Majoris with VERA," Proc. of the "Approaching Micro-Arcsecond
Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed.,
Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.363-365.
We present observational results on the red supergiant VY Canis Majoris with VERA. We haveobserved 22 GHz H2O masers and 43 GHz SiO masers (v = 1 and 2 J = 1-0) around VY CMa
for 13 months. We successfully detected a parallax of 0.87±0.08 mas, corresponding to

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1.15+0.10-0.09 kpc of distance using H2O masers. As results of phase ﾐ referencing analyses, wehave measured absolute positions for both the H2O masers and SiO masers. The propermotions of the H2O masers show the tendency of expansion.
Cirtain, J. W., L. Golub, L. Lundquist, A. van Ballegooijen, A. Savcheva, M. Shimojo, E.
DeLuca, S. Tsuneta, T. Sakao, K. Reeves, M. Weber, R. Kano, N. Narukage, and K. Shibasaki[2007], "Evidence for Alfvén Waves in Solar X-ray Jets," Science, vol.318, pp.1580-1582.
Coronal magnetic fields are dynamic, and field lines may misalign, reassemble, and releaseenergy by means of magnetic reconnection. Giant releases may generate solar flares andcoronal mass ejections and, on a smaller scale, produce x-ray jets. Hinode observations ofpolar coronal holes reveal that x-ray jets have two distinct velocities: one near the Alfvén
speed (~800 kilometers per second) and another near the sound speed (200 kilometers per
second). Many more jets were seen than have been reported previously; we detected anaverage of 10 events per hour up to these speeds, whereas previous observations documented
only a handful per day with lower average speeds of 200 kilometers per second. The x-ray jets
are about 2 × 103 to 2 × 104 kilometers wide and 1 × 105 kilometers long and last from 100 to2500 seconds. The large number of events, coupled with the high velocities of the apparent
outflows, indicates that the jets may contribute to the high-speed solar wind.
Deguchi, S., T. Fujii, Y. Ita, H. Izumiura, O. Kameya, A. Miyazaki, Y. Nakada, and M. Ideta[2008a], "Dynamics of Stars in the Inner Galactic Bulge Revealed from SiO Maser Surveys,"Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F.,
pp.33-38.
We surveyed ~300 MSX/2MASS infrared objects in the 7°×2° area of the Galactic center inthe ~43 GHz SiO maser lines, obtaining accurate radial velocities of ~160 detected objects.
The longitude-velocity diagram of these objects reveals two conspicuous features: one
indicating a linear velocity increase with longitude with |l| < 1.5°, which is likely to be
associated with the inner bar, and the other having eccentric velocities with |Vlsr| >250 km s-1.
Based on numerical simulations of stellar orbits in the Galactic bulge, we conclude that thelatter feature is created as a result of a past star formation in the bulge, when the intersecting
point of the x1 and x2 orbits was considerably outside of the present position.
Deguchi, S. [2008b], "SiO Maser Survey of Evolved Stars in the Galaxy: Various
Environments of Maser Sources," Proc. of the IAU Symp. 242, "Astrophysical Masers andtheir Environments", eds. Jessica Chapman and Willem Baan, pp.200-207.
Using the SiO J=1-0 v=1 and v=2 lines near 43 GHz, we have detected about 2000 of 3600
sources observed with the Nobeyama 45-m radio telescope. The sources were chosen from
IRAS/MSX/2MASS catalogs using color-selection criteria to pick up mass-losing oxygen-rich
AGB stars and some post-AGB objects. A number of interesting sources were also found:supergiants in a massive star cluster, a nova with light echo (V838 Mon), AGB stars inglobular clusters, and AGB candidates associated with dwarf galaxies. With the exception of
the stars in the massive open star cluster, these 'unusual' objects are associated with metal poor
environments where mass losing oxygen-rich AGB stars are unexpected. It is inferred thatthese objects were created by stellar merging which can occur in dense star clusters.
Deguchi, S. [2009a], "Study of Red Supergiants in Embedded Star Clusters by Radio Lines,"
Proc. of the "AGB stars and related phenomena", eds. Toshiya Ueta, Noriyuki Matsunaga, andYoshifusa Ita, p.74.
Not Available
Deguchi, S., N. Matsunaga, H. Fukushi, and T. Kaminski [2009b], "Detection of the SiO J=2-1,
v=1 Maser Emission at 86.2 GHz in V838 Mon, an Unusual Nova-Like Variable," ATel,#1996.
We report on a new detection of the SiO J=2-1 v=1 maser line at 86.243 GHz in V838 Mon.

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The observations were obtained on 2009 March 21-23 using the 45m telescope at Nobeyama
with a newly built sensitive dual- polarization receiver. The maser line has a peak intensity of
0.39 Jy at Vlsr=53.7 km/s and exhibits a complex asymmetric pedestal with a stronger
contribution at the lower velocity side; the total integrated intensity of the emission feature isof 2.8 Jy km/s.
Deguchi, S., N. Matsunaga, S. Takahashi, N. Kuno, and J. Nakashima [2010a], "Dying SiO
Maser in the V407 Cyg System," Atel, #2519.
The symbiotic nova, V407 Cyg, is a system having a Mira-type cool stellar component withcircumstellar SiO maser emission (Deguchi et al. 2005; PASJ 57, 939). The nova outburst
occurred in the V407 Cyg system can significantly influence the structure of the circumstellar
shell of the cool star in a short time scale. We have been monitoring the time variation of SiO
maser emission in the V407 Cyg system with the Nobeyama 45m telescope every few days
since March 16, 2010.
Deguchi, S., J. Nakashima, Y. Zhang, S. S. N. Chong, K. Koike, and S. Kwok [2010b], "SiO
and H2O Maser Observations of Red Supergiants in Star Clusters Embedded in the Galactic
Disk," Publ. Astron. Soc. Japan, vol.62, pp.391-407.
We present the results of radio observations of red supergiants in a star cluster, Stephenson(1990, AJ, 99, 1867)’s #2, and of candidates for red supergiants in three star clusters, Mercer etal. (2005, ApJ, 635, 560)’s #4, #8, and #13, in the SiO and H2O maser lines. The Stephenson’s#2 cluster and nearby aggregation at the southwest contain more than 15 red supergiants. We
detected one red supergiant at the center of Stephenson’s #2 and three in a southwest
aggregation in the SiO maser line; three out of these four were also detected in the H2O maserline. The average radial velocity of the four detected objects is 97 kms-1, giving a kinematic
distance of 5.5 kpc, which locates this cluster near the base of the Scutum-Crux spiral arm. We
also detected six SiO emitting objects associated with other star clusters. In addition, mapping
observations in the CO J = 1-0 line toward these clusters revealed that an appreciable amountof molecular gas still remains around the Stephenson’s #2 cluster in contrast to the prototypical
red-supergiant cluster, Bica et al. (2003, A&A, 404, 223)’s #122. This indicates that the timescale of gas expulsion differs considerably in individual clusters.
Deguchi, S., T. Shimoikura, and K. Koike [2010c], "SiO Maser Survey off the Galactic Plane:
A Signature of Streaming Motion," Publ. Astron. Soc. Japan, vol.62, 5pp.25-546.
A group of Mira variables in the solar neighborhood shows unusual spatial motion in the
Galaxy. To study this motion on a much larger scale in the Galaxy, we newly surveyed 134
evolved stars off the Galactic plane by SiO maser lines, obtaining accurate radial velocities of
84 detected stars. Together with the past data of SiO maser sources, we analyzed theradial-velocity data of a large sample of sources distributed in a distance range of about 0.3-6
kpc in the first Galactic quadrant. At Galactic longitudes between 20° and 40°, we found agroup of stars with large negative radial velocities, which deviate by more than 100 km s-1
from the Galactic rotation. We show that these deviant motions of maser stars are created byperiodic gravitational perturbation of the Bulge bar, and that the effect appears most strongly atradii between corotation and outer Lindblad resonances The resonance effect can explain thedisplacement of positions from the Galactic plane as well.
Doi, A., K. Fujisawa, M. Honma, K. Sugiyama, Y. Murata, N. Mochizuki, and Y. Isono[2008a], "Japanese VLBI Network Observations of 6.7-GHz Methanol Masers 1. Array," Proc.
of the IAU Symp. 242, "Astrophysical Masers and their Environments", eds. Jessica Chapman
and Willem Baan, pp.148-149.
The Japanese VLBI network (JVN) has begun observations of 6.7-GHz methanol masers
associated with massive star-forming regions. The JVN is a newly-established VLBI array withbaselines ranging from 50 to 2560 km spread across the Japanese islands. Three observing

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bands of 6.7, 8.4, and 22 GHz are now available. The array consists of ten antennas: VERA
Mizusawa 20 m, VERA Ishigaki 20 m, VERA Iriki 20 m, Usuda 64 m, Yamaguchi 32 m,
Tomakomai 11 m, Tsukuba 32 m, Kashima 34 m, VERA Ogasawara 20 m, and Gifu 11 m, thefirst five of which have 6.7-GHz receiving systems. In summer 2005, we obtained the first
fringes at 6.7 GHz, and VLBI images of 12 methanol maser sites including seven that had notpreviously been imaged with VLBI at this band. In 2006 summer, we obtained phase-reference
observations toward several methanol maser sites.
Doi, A., K. Asada, H. Nagai, K. Fujisawa, and N. Kawaguchi [2008b], "JVN Observataions of
NLS1 Galaxies and BAL Quasars," Proc. of the 9th European VLBI Network Symposium on
The role of VLBI in the Golden Age for Radio Astronomy and EVN Users Meeting,
September 23-16, 2008, Bologna, Italy, pp.73-75.
We are conducting VLBI observations for Narrow-Line Seyfert 1 galaxies (NLS1s) and Broad
Absorption Line (BAL) quasars, which are thought to be driven by highly accreting central
engines, in order to understand accretion phenomena on such central engines. Because these
AGN subclasses are generally very weak radio sources, phase-referencing VLBI observations
are being carried out using Japanese VLBI Network (JVN), together with VLBA, EVN, and an
optical-ﬁbre-linked JVN subarray “OCTAVE.” For NLS1s, 12 out of 14 sources have beensuccessfully imaged in milli-arcsecond resolutions. For BAL quasars, 21 out of 23 sources
have been successfully detected with OCTAVE baselines at 8.4 GHz. Several NLS1 sand BAL
quasars are investigated in images at multi-frequency. Some evidence of Doppler-boosting on
relativistic jets were seen in several radio-loud objects, which is inconsistent with the edge-on
view paradigm of BAL quasars.
Doi, A., M. Tsuboi, Y. Kono, H. Takeuchi, N. Mochizuki, Y. Murata, and ASTRO-G Group[2009a], "ASTRO-G Observing Systems," Proc. of the "Approaching Micro-Arcsecond
Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed.,
Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.46-50.
ASTRO-G for the VSOP-2 project is a radio telescope satellite for a next-generation space
very-long-baseline interferometry (VLBI) following HALCA for the VSOP project. It will belaunched in 2012. We present the overview of ASTRO-G observing systems and available
observing modes.
Doi, A., N. Kawaguchi, Y. Kono, T. Oyama, K. Fujisawa, H. Takaba, H. Sudou, K. Wakamatsu,
A. Yamauchi, Y. Murata, N. Mochizuki, K. Wajima, T. Omodaka, T. Nagayama, N. Nakai, K.
Sorai, E. Kawai, M. Sekido, Y. Koyama, S. Asano, and H. Uose, [2009b], "VLBI Detections ofParsec-Scale Nonthermal Jets in Radio-Loud Absorption Line Quasars," Publ. Astron. Soc.
Japan, vol.61, pp.1389-1398.
We conducted radio detection observations at 8.4 GHz for 22 radio-loud broad absorption line
(BAL) quasars, selected from the Sloan Digital Sky Survey Third Data Release, by avery-long-baseline interferometry (VLBI) technique. The VLBI instrument we used wasdeveloped by the Optically ConnecTed Array for VLBI Exploration project (OCTAVE), which
is operated as a subarray of the Japanese VLBI Network. We aimed to select BAL quasars withnonthermal jets suitable for measuring their orientation angles and ages by subsequent detailed
VLBI imaging studies to evaluate two controversial issues of whether BAL quasars are viewed
nearly edge-on, and of whether BAL quasars are in a short-lived evolutionary phase of thequasar population. We detected 20 out of 22 sources using the OCTAVE baselines, implying
brightness temperatures greater than 105 K, which presumably come from nonthermal jets.
Hence, BAL outflows and nonthermal jets can be generated simultaneously in these central
engines. We also found four inverted-spectrum sources, which are interpreted as
Doppler-beamed, pole-on-viewed relativistic jet sources, or young radio sources: single
edge-on geometry cannot describe all BAL quasars. We discuss the implications of the

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OCTAVE observations for investigations for the orientation and evolutionary stage of BAL
quasars.
Egusa, F., Y. Sofue, H. Nakanishi, and S. Komugi [2008a], "Determination of Pattern Speedand Star Formation Timescale in Nearby Spiral Galaxies," Proc. of the "Mapping the Galaxy
and Nearby Galaxies", eds. Wada, K., and Combes, F., p.320.
Without abstract
Egusa, F., Y. Sofue, S. Komugi, and H. Nakanishi [2008b], "Determination of Star Formation
Timescale and Pattern Speed of Spiral Galaxies", Proc. of the "Pathways Through an Eclectic
Universe", eds. J. H. Knapen, T. J. Mahoney, and A. Vazdekis, ASP Conf. Ser., vol.390,
pp.180-181.
We propose a method to determine the star formation timescale and pattern speed
simultaneously in spiral galaxies. Though they are important and fundamental parameters ingalactic dynamics and star formation scenarios, it has hitherto been difficult to derive theirvalues directly from observations. Our method utilizes azimuthal offsets between arms of HII
regions and molecular clouds, and has been successfully applied to three nearby galaxies so far
through the use of CO and Hα images. As derived star formation timescales fall into thenarrow range of 4-13Myr, which is consistent with typical timescales for molecular clouds tocollapse gravitationally, a dominant mechanism of global star formation in spiral arms might
be the gravitational collapse of molecular clouds.
Egusa, F., Y. Sofue, K. Kohno, H. Nakanishi, and S. Komugi [2009], "Determining Star
Formation Timescale and Pattern Speed in Nearby Spiral Galaxies," Astrophys, J., vol.697,
pp.1870-1891.
We present a revised method for simultaneous determination of the pattern speed (ΩP) and starformation timescale (tSF) of spiral galaxies, which is originally proposed in our previous work.
As this method utilizes offsets between molecular and young-stellar arms, we refer to it as the"Offset Method." Details of the method, its application, and results for CO and Hα images of
13 nearby spiral galaxies are described here. CO data are from our observations with theNobeyama Millimeter Array for two galaxies, and from the BIMA SONG for the rest. Out of
13 galaxies, we were able to derive ｽ P and tSF for five galaxies. We categorize them as "C"galaxies as their offsets are clear. Our findings from these galaxies are as follows. (1) The
corotation radius calculated by the derived ΩP is close to the edge of the CO data, and is about
half of the optical radius for three galaxies. (2) The derived tSF is roughly consistent with thefree-fall time of typical molecular clouds, which indicates that the gravitational instability is
the dominant mechanism triggering star formation in spiral arms. (3) The tSF is found to bealmost independent of the surface density of molecular gas, metallicity, or spiral arm strengths.
The number of "C" galaxies and the quality of CO data, however, are not enough to confirm
these relationships. We also find that two other galaxies show no offsets between CO and H ,although their arms are clearly traced, and categorize them as "N" galaxies. The presence of abar could account for this feature, since these two galaxies are both barred. With one galaxy
excluded from our analysis due to its poor rotation curve, offsets of the remaining five galaxies
are found to be ambiguous. Either their dependence on the rotational frequency cannot be
explained by our picture, or the number or quality of data is not sufficient for the analysis. We
categorize them as "A" galaxies. The possible reasons for this ambiguity are (1) the density
wave is weaker, and/or (2) observational resolution and sensitivity are not enough to detect the
spiral arms and their offsets clearly. The former is supported by our finding that the arm
strengths of "A" galaxies are slightly weaker than that of "C" galaxies.
Ezawa, H., K. Kohno, R. Kawabe, S. Yamamoto, H. Inoue, H. Iwashita, H. Matsuo, T. Okuda,
T. Oshima, T. Sakai, K. Tanaka, N. Yamaguchi, G. W. Wilson, M. S. Yun, I. Aretxaga, D.
Hughes, J. Austermann, T. A. Perera, K. S. Scott, L. Bronfman, and J. R. Cortes [2008], "New

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Archevements of ASTE: the Atacama Submillimeter Telescope Experiment." Proc. of the SPIE,
vol.7012, pp.101208-1-9.
ASTE is a 10-m submillimeter telescope operating in Atacama desert in northern Chile since
2002 by NAOJ and collaborators. Thanks to the excellent observing condition at the telescopesite, ASTE has been producing numerous astronomical results from star forming regions,
Galactic center, Magellanic clouds, nearby galaxies, and galaxy clusters. There has been threemajor improvements during the years 2007-2008: continuum camera "AzTEC", new SIS
receiver "CATS345", and a wide-band spectrometer "WHSF". AzTEC is a 144 element
bolometer array at 270 GHz, developed by University of Massachusetts and collaborators. The
mapping speed reaches 10-30 arcmin2/hr/mJy2. CATS345 is a side-band separation (2SB) SIS
receiver developed by University of Tokyo and NAOJ. The IF bandwidth is 4 GHz withside-band rejection ratio better than 10 dB. We have achieved the typical system noise
temperature of 200-400 K (SSB) within 330-360 GHz, the best value being 150 K (SSB) at thefrequency of 12CO(J=3-2) at 345 GHz under a typical weather condition. The newspectrometer WHSF employs of an FX type auto-correlator, ultra-high speed sampler, anddigital signal transmitter. It can be operated in two modes; 4096 MHz band-width ×2 IFs or
2048 MHz band-width ×4 IFs, both with 4096 channels in spectral resolution.
Fomalont, E. B., S. Kopeikin, O. Titov, and M. Honma [2009], "VLBA/VERA Test of General
Relativity," AAS#15.03/BAAS, vol.41, p.890.
We report on VLBA/VERA/geodetic observational tests of General Relativity. First, we willsummarize the results from recent VLBA experiments which measured gamma from thebending of radio waves of quasars by the solar gravitational field, and the experiment thatmeasured the the aberration of gravity using the Jovian gravitational field. We will thendescribe tentative results from several recent experiments that continue the measurements of
the aberration of gravity from Jupiter and Saturn using the VLBA, VERA and the geodetic
network. Finally, we discuss the limits of precision that can be obtained with VLBI now and in
the future.
Fomalont, Ed., S. Kopeikin, D. Jones, M. Honma, and O. Titov [2010], "Recent
VLBA/VERA/IVS Tests of General Relativity,” Proc. of the IAU symp. vol.261, "Relativity infundamental astronomy: dynamics, reference frames, and data analysis", pp.291-295.
We report on recent VLBA/VERA/IVS observational tests of General Relativity. First, we willsummarize the results from the 2005 VLBA experiment that determined gamma with anaccuracy of 0.0003 by measuring the deflection of four compact radio sources by the solar
gravitational field. We discuss the limits of precision that can be obtained with VLBA
experiments in the future. We describe recent experiments using the three global arrays tomeasure the aberration of gravity when Jupiter and Saturn passed within a few arcmin of brightradio sources. These reductions are still in progress, but the anticipated positional accuracy of
the VLBA experiment may be about 0.01 mas.
Friesen, R. K., J. Di Franesco, Y. Shimajiri, and S. Takakuwa [2010], "The Initial Conditionsof Clusteres Star Formation II: N2H+ Observations of the Ophiuchus B Core," Astrophys. J.,
vol.708, pp.1002-1024.
We present a Nobeyama 45 m Radio Telescope map and Australia Telescope Compact Array
pointed observations of N2H+ 1-0 emission toward the clustered, low-mass star-forming Oph B
Core within the Ophiuchus molecular cloud. We compare these data with previously publishedresults of high-resolution NH3 (1,1) and (2,2) observations in Oph B. We use 3D
CLUMPFIND to identify emission features in the single-dish N2H+ map, and find that theN2H+ "clumps" match well similar features previously identified in NH3 (1,1) emission, but
are frequently offset to clumps identified at similar resolution in 850μm continuum emission.
Wide line widths in the Oph B2 sub-Core indicate that non-thermal motions dominate the Core

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kinematics, and remain transonic at densities n ~ 3 × 105 cm–3 with large scatter and no trendwith N(H2). In contrast, non-thermal motions in Oph B1 and B3 are subsonic with little
variation, but also show no trend with H2 column density. Over all of Oph B, non-thermal
N2H+ line widths are substantially narrower than those traced by NH3, making it unlikely NH3
and N2H+ trace the same material, but the vLSR of both species agree well. We find evidence
for accretion in Oph B1 from the surrounding ambient gas. The NH3/N2H+ abundance ratio islarger toward starless Oph B1 than toward protostellar Oph B2, similar to recent observational
results in other star-forming regions. The interferometer observations reveal small-scale
structure in N2H+ 1-0 emission, which are again offset from continuum emission. No
interferometric N2H+ emission peaks were found to be coincident with continuum clumps. In
particular, the ~1 Msun B2-MM8 clump is associated with an N2H+ emission minimum andsurrounded by a broken ring-like N2H+ emission structure, suggestive of N2H+ depletion. We
find a strong general trend of decreasing N2H+ abundance with increasing N(H2) in Oph B
which matches that found for NH3.
Fujishita, M., K. Torii, N. Kudo, T. Kawase, H. Yamamoto, A. Kawamura, N. Mizuno, T.
Onishi, A. Mizuno, M. Machida, K. Takahashi, S. Nozawa, R. Matsumoto, and Y. Fukui [2009],"Discovery of Molecular Loop 3 in the Galactic Center: Evidence for a Positive-Velocity
Magnetically Floated Loop towards L=355°-359°, " Publ. Astron. Soc. Japan, vol.61,
pp.1039-1053.
We have discovered a molecular dome-like feature towards 355° ≤ l ≤ 359° and 0° ≤ b ≤ 2°.
The large velocity dispersions of 50-100 km s-1 of this feature are much larger than those in the
Galactic disk, and indicate that the feature is located in the Galactic center, probably within ~1
kpc of Sgr A*. The distribution has a projected length of ~600 pc and a height of ~300 pc fromthe Galactic disk, and shows a large-scale monotonic velocity gradient of ~130 km s-1 per~600 pc. The feature is also associated with HI gas having a more continuous spatial andvelocity distribution than that of 12CO. We interpret the feature as being a magnetically floatedloop similar to loops 1 and 2, and name it "loop 3''. Loop 3 is similar to loops 1 and 2 in its
height and length, but is different from loops 1 and 2 in that the inner part of loop 3 is filledwith molecular emission. We have identified two foot points at both ends of loop 3. HI, 12CO,
and 13CO datasets were used to estimate the total mass and the kinetic energy of loop 3 to be~3.0 × 106 M⦿ and ~1.7 × 1052 erg. The huge size, velocity dispersions, and energy are
consistent with the magnetic origin of the Parker instability, as in the case of loops 1 and 2, but
is difficult to be explained by multiple stellar explosions. We argue that loop 3 is in an earlier
evolutionary phase than loops 1 and 2 based on the inner-filled morphology and the relative
weakness of the foot points. This discovery indicates that the western part of the nuclear gas
disk of ~1 kpc radius is dominated by the three well-developed magnetically floated loops, andsuggests that the dynamics of the nuclear gas disk is strongly affected by magnetic instabilities.
Fukui, Y., N. Furukawa, T. M. Dame, J. R. Dawson, H. Yamamoto, G. P. Rowell, F. Aharonian,
W. Hofmann, E. de Oña Wilhelmi, T. Minamidani, A. Kawamura, N. Mizuno, T. Onishi, A.
Mizuno, and S. Nagataki [2009a], "A Peculiar Jet and Arc of Molecular Gas toward the Rich
and Young Stellar Cluster Westerlund 2 and a TeV Gamma Ray Source," Publ. Astron. Soc.
Japan, vol.61, pp.L23-L27.
We have discovered remarkable jet- and arc-like molecular features toward the rich and youngstellar cluster Westerlund 2. The jet has a length of ~ 100 pc and a width of ~ 10 pc, while thearc shows a crescent shape with a radius of ~30 pc. These molecular features each have massesof ~104 M⦿, and show spatial correlations with the surrounding lower density HI gas. The jetalso shows an intriguing positional alignment with the core of the TeV gamma-ray source
HESS J1023-575 and with the MeV/GeV gamma-ray source recently reported by the Fermi
collaboration. We argue that the jet and arc are caused by an energetic event in Westerlund 2,

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presumably due to an anisotropic supernova explosion of one of the most massive member
stars. While the origin of the TeV and GeV gamma-ray sources is uncertain, one may speculatethat they are related to the same event via relativistic particle acceleration by strong shockwaves produced at the explosion or by remnant objects, such as a pulsar wind nebula or a
microquasar.
Fukui, Y., A. Kawamura, T. Wong, M. Murai, H. Iritani, N. Mizuno, Y. Mizuno, T. Onishi, A.
Hughes, J. Ott, E. Muller, L. Staveley-Smith, and S. Kim [2009b], "Molecular and Atomic Gas
in the Large Magellanic Cloud II. Three-Dimensional Correlation between CO and HI,"Astrophys. J., vol.705, pp.144-155.
We compare the CO (J = 1-0) and H I emission in the Large Magellanic Cloud in three
dimensions, i.e., including a velocity axis in addition to the two spatial axes, with the aim ofelucidating the physical connection between giant molecular clouds (GMCs) and theirsurrounding H I gas. The CO J = 1-0 data set is from the second NANTEN CO survey and the
H I data set is from the merged Australia Telescope Compact Array (ATCA) and Parkes
Telescope surveys. The major findings of our analysis are as follows: (1) GMCs are associatedwith an envelope of H I emission, (2) in GMCs [average CO intensity] ∼ [average H I
intensity]1.1±0.1, and (3) the H I intensity tends to increase with the star formation activity
within GMCs, from Type I to Type III. An analysis of the H I envelopes associated with GMCs
shows that their average line width is 14 km s-1 and the mean density in the envelope is 10 cm-3.
We argue that the H I envelopes are gravitationally bound by GMCs. These findings are
consistent with a continual increase in the mass of GMCs via H I accretion at an accretion rateof 0.05 Msun yr-1 over a timescale of 10 Myr. The growth of GMCs is terminated via
dissipative ionization and/or stellar-wind disruption in the final stage of GMC evolution.
Fukui, Y., and A. Kawamura [2010], "Molecular Clouds in Nearby Galaxies," Ann. Rev.
Astron. Astrophys., vol.48, pp.547-580.
We present a review of spatially resolved giant molecular clouds (GMCs) in nearby galaxies,
aiming at providing a template of GMC properties, which may be extrapolated to distantgalaxies. We focus on the Magellanic system including the Large and Small Magellanic
Clouds (LMC, SMC), M33, and a few dwarfs as observed in the J = 1-0 12CO transition at
2.6-mm wavelength. The X factor, a conversion factor of the 12CO intensity to total molecularcolumn density, and the GMC mass distribution, dN/dM, are similar among these galaxies,
suggesting that GMCs share similar properties in the Local Group. The GMCs are classified
into three types according to their level of star-formation activity and the types are interpreted
in terms of evolution in 20-30 Myr rather than as three different generic types. A
three-dimensional comparison including the velocity axis has revealed that GMCs in the LMC
are associated with Hi envelopes. The Hi envelopes are probably gravitationally bound andmay be infalling to increase the GMC mass via Hi-H2 conversion. Recent submillimeter
observations are revealing dense and warm clumps in GMCs, suggesting that the interior of a
GMC also follows contraction leading to star formation on a similar timescale. Finally, we
present an attempt to place these GMC properties among more distant galaxies and discuss
future observational prospects.
Furuya, R. S., R. Cesaroni, S. Takahashi, C. Codella, M. Momose, and M. T. Beltran [2008a],"Candidate Rotating Toroids around High-Mass (Proto)Stars," Astrophys. J., vol.673,
pp.363-381.
Using the OVRO, Nobeyama, and IRAM millimeter arrays, we searched for "disk"-outflow
systems in three high-mass (proto)star-forming regions: G16.59-0.05, G23.01-0.41, andG28.87+0.07. These were selected from a sample of NH3 cores (Codella, Testi, & Cesaroni)
associated with OH and H2O maser emission (Foster & Caswell) and with no or very faintcontinuum emission. Our imaging of molecular line (including rotational transitions of

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CH3CN) and 3 mm dust continuum emission revealed that these are compact (<~0.06-0.13 pc),
massive (~100-400 Msolar), and hot (~100 K) molecular cores (HMCs) that are likely sites ofhigh-mass star formation prior to the appearance of ultracompact HII regions. All three sources
turn out to be associated with molecular outflows from 12CO and/or HCO+ J=1-0 line imaging.
In addition, velocity gradients of 10-100 km s-1 pc-1 in the innermost, densest regions of theG23.01-0.41 and G28.87+0.07 HMCs are identified along directions roughly perpendicular to
the axes of the corresponding outflows. All the results suggest that these cores might berotating about the outflow axis, although the contribution of rotation to gravitational
equilibrium of the HMCs appears to be negligible. Our analysis indicates that the three HMCs
are close to virial equilibrium due to turbulent pressure support. Comparison with other similar
objects where rotating toroids have been identified so far shows that in our case rotation
appears to be much less prominent; this can be explained by the combined effect of
unfavorable projection, large distance, and limited angular resolution with the current
interferometers.
Furuya, R. S., Y. Kitamura, and H. Shinnnaga [2008b], "Low-Mass Star-Forming Cores in the
GF9 Filament," Publ. Astron. Soc. Japan, vol.60, pp.421-428.
We carried out an unbiased mapping survey of dense molecular cloud cores traced by the NH3(1,1) and (2,2) inversion lines in the GF9 filament which contains an extremely young
low-mass protostar GF9-2 (Furuya et al. 2006, ApJ, 653, 1369). The survey was conductedusing the Nobeyama 45m telescope over a region of ~1.5°x1° with an angular resolution of 73".
The large-scale map revealed that the filament contains at least 7 dense cores, as well as 3
possible ones, located at regular intervals of ~0.9 pc. Our analysis shows that these cores havekinetic temperatures of ∼10 K and LTE-masses of 1.8 - 8.2 Msun, making them typical sites of
low-mass star formation. All the identified cores are likely to be gravitationally unstablebecause their LTE-masses are larger than their virial masses. Since the LTE-masses andseparations of the cores are consistent with the Jeans masses and lengths, respectively, for the
low-density ambient gas, we argue that the identified cores have formed via the gravitational
fragmentation of the natal filamentary cloud.
Furuya, R. S., Y. Kitamura, and H. Shinnaga [2009], "Spectroscopic Evidence for Gas Infall in
GF 9-2," Astrophys. J. (Letters), vol.692, pp.L96-L99.
We present spectroscopic evidence for the infall motion of gas in the natal cloud coreharboring an extremely young low-mass protostar GF 9-2. We previously discussed that theongoing collapse of the GF 9-2 core has agreement with the Larson-Penston-Hunter (LPH)
theoretical solution for the gravitational collapse of a core. To discuss the gas infall on firmer
ground, we have carried out on-the-fly mapping observations of the HCO+ (1-0) line using theNobeyama 45 m telescope equipped with the 25 Beam Array Receiver System. Furthermore,
we observed the HCN (1-0) line with the 45 m telescope, and the HCO+ (3-2) line with theCaltech Submillimeter Observatory 10.4 m telescope. The optically thick HCO+ and HCNlines show blueskewed profiles whose deepest absorptions are seen at the peak velocity of
optically thin lines, i.e., the systemic velocity of the cloud, indicating the presence of gas infall
toward the central protostar. We compared the observed HCO+ line profiles with model ones
by solving the radiative transfer in the core under LTE assumption. We found that the core gas
has a constant infall velocity of ~0.5 km s-1 in the central region, leading to a mass accretion
rate of 2.5 x 10-5 M⦿ yr-1. Consequently, we confirm that the gas infall in the GF 9-2 core isconsistent with the LPH solution.
Glendenning, B. E., J. Ibsen, G. Kosugi, and G. Raffi [2010], "ALMA Software Management
and Deployment," Proc. of the SPIE, vol.7740, pp.77401L-77401L-6.
The ALMA Software (~ 80% completed) is in daily use at the ALMA Observatory and has
been developed as an end-toend system including: proposal preparation, dynamic scheduling,

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instrument control, data handling and formatting, data archiving and retrieval, automatic andmanual data processing, and support for observatory operations. This presentation will expand
on some software management aspects, procedures for releases, integrated system testing anddeployment in Chile. The need for a realistic validation environment, now achieved with a twoantenna interferometer at the observatory, and the balance between incremental development
and stability of the software (a challenge at the moment) will be explained.
Gomez, Y., D. Tafoya, G. Anglada, L. Loinard, J. M. Torrelles, L. F. Miranda, M. Osorio, R.
Franco-Hernandez, L. Nyman, J. Nakashima, and S. Deguchi [2008], "HCO+ Emission
Possibly Related with a Shielding Mechanism that Protects Water Molecules in the Young PN
K 3-35," Proc. of the IAU Symp. 251, "Organic Matter in Space", eds. S. Kwok, and S.
Sandford, pp.173-174.
Water maser emission has been detected only toward three planetary nebulae (PNe). In
particular, in K3-35, the first PN where water vapor maser emission was detected, thecomponents are located in a torus-like structure with a radius of 85 AU and also at the
surprisingly large distance of 5000 AU from the star, in the tips of the bipolar lobes. The
existence of these water molecules in PNe is puzzling, probably related to some unknown
mechanism shielding them against the ionizing radiation. We report the detection of HCO+ (J =1 - 0) emission toward K 3-35, that not only suggests that dense molecular gas (~105 cm-3) ispresent in this PN, but also that this kind of PN can enrich their surroundings with organic
molecules.
Goossens, S., and K. Matsumoto [2008a], "Determination of the Lunar k2 Love Number from
Satellite Tracking Data," 39th Lunar and Planetary Science Conference, (Lunar and Planetary
Science XXXIX), held March 10-14, 2008 in League City, Texas. LPI Contribution No. 1391.,
p.1536.
The lunar potential Love number k2 has been determined from available satellite tracking data.
The best estimate in this research yields k2 = 0.0213 ± 0.0075 (ten sigma), which is closer toresults based on lunar laser ranging than a previous satellite-based estimate.
Goossens, S., K. Matsumoto, Y. Ishihara, Q. Liu, F. Kikuchi, H. Noda, N. Namiki, and T. Iwata[2008b], "Orbit Determination and Quality Assessment Using SELENE Tracking Data andResults," 37th COSPAR Scientific Assembly, held 13-20 July 2008, in Montreal, Canada,p.1055.
On September 14, 2007, the SELENE (KAGUYA) spacecraft were launched from
Tanegashima Space Center in Japan. SELENE consists of three satellites: a main orbiter in a
100 km by 100 km circular, polar orbit, and two small subsatellites in 100 km by 2400 km(Rstar) and 100 km by 800 km (Vstar) elliptical, polar orbits. Until now, tracking of lunar
satellites consisted of 2-way (or 3-way, where the upand downlink stations are different)
tracking, leaving a gap in the tracking coverage over the far side of the Moon as the satellite
cannot be tracked there from Earth. This severely hampers the determination of the global
lunar gravity field, and, consequently, this also puts limits on the precision of orbits of lunar
satellites. By employing 4-way Doppler tracking between the main orbiter and Rstar, the first
direct tracking data of a satellite over the far side have been obtained, resulting in a newly
determined global lunar gravity field. The existing 2-way tracking data set is furthermore
complemented by differential VLBI tracking between Rstar and Vstar, providing a sensitivity
perpendicular to the line-ofsight from station to satellite. This work focuses on aspects of orbit
determination for the SELENE satellites, including the processing strategies for data types
using multiple satellites. Orbit determination quality is described in terms of data fit and,
where possible, orbit overlap statistics. For the main satellite, the on-board altimeter provides
an independent check of orbit quality through crossovers, although they are not yet
systematically included in the orbit determination process. The performance of the VLBI data

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in the orbit determination of the small subsatellites is also discussed. The newly determined
global lunar gravity field models from SELENE are evaluated in several ways: theirperformance when used in orbit determination of previous lunar satellites, and their ability inorbit prediction. Covariance analysis shows the expected orbit quality. The results presented
here are thought to be of importance for oncoming lunar spacecraft, such as LRO, GRAIL andother future missions.
Goossens, S., K. Matsumoto, Y. Ishihara, Q. Liu, F. Kikuchi, H. Noda, T. Iwata, N. Namiki,and H. Hanada [2008c], "Analysis of Tracking Data and Results from Kaguya (SELENE)
Satellites for Lunar Gravity Field Estimation," American Geophysical Union, Fall Meeting
2008, abstract #P31B-1400.
On September 14, 2007, the KAGUYA (SELENE) spacecraft were launched from
Tanegashima Space Center in Japan. KAGUYA consists of three satellites: a main orbiter in a
100 km by 100 km circular, polar orbit, and two small subsatellites in 100 km by 2400 km(Rstar) and 100 km by 800 km (Vstar) elliptical, polar orbits. By employing 4-way Doppler
tracking between the main orbiter and Rstar, the first direct tracking data of a satellite over thefar side have been obtained, resulting in a newly determined global lunar gravity field. The
existing 2-way tracking data set is furthermore complemented by precise differential VLBI
tracking between Rstar and Vstar, providing a sensitivity perpendicular to the line-of-sightfrom station to satellite. This work focuses on various aspects of processing and analysing the
tracking data from the Kaguya satellites for the main purpose of lunar gravity field estimation.
This includes particulars of the data processing strategies, multi-satellite analysis and data
weighting. Gravity models from Kaguya data are evaluated in terms of data fit andperformance in orbit determination. The performance of the differential VLBI data in the orbit
determination of the small subsatellites is also discussed, as well as their contribution to thegravity solutions. Results for the polar moment of inertia C/MR2 from the degree 2
coefficients, and for the lunar k2 Love number are also included.
Goossens, S., K. Matsumoto, Y. Ishihara, Q. Liu, F. Kikuchi, H. Noda, N. Namiki, T. Iwata,and H. Hanada [2009], "Updated Lunar Gravity Results from Kaguya (SELENE) andHistorical Tracking Data," American Geophysical Union, Fall Meeting 2009, abstract#P23C-1274.
The Kaguya spacecraft were launched from Tanegashima Space Center on September 14, 2007.
Kaguya consists of three orbiters: a main orbiter in a low-altitude (100 km) circular polar orbit,
and two sub-satellites (Rstar and Vstar) in elliptical orbits. By taking tracking data between
Rstar and the main orbiter while the main orbiter was over the farside of the Moon (called
4-way Doppler), Kaguya has obtained the first direct tracking data over the farside. Tracking
data were further complemented by differential VLBI tracking between Rstar and Vstar andstations on Earth, with a sensitivity perpendicular to the line-of-sight, thus offering further
improvement in three-dimensional positioning of the relay satellites. On February 12, 2009,
Rstar crashed into the Moon because of its natural orbital evolution, finishing the opportunities
for 4-way data. On June 10, the main orbiter finished its lifetime by a controlled crash into theMoon, and tracking for Vstar was ended on June 29, comprising the end of data collection
from Kaguya. Here, results from incorporating all Kaguya Doppler tracking (including allcollected 4-way data over the farside) are presented. Spherical harmonics expansions up todegree and order 100 have been determined, and they will be evaluated in terms of geophysicalcontent, correlations with topography, and orbit determination performance. It is shown that
unconstrained solutions can be obtained up to degree and order 70 without loss of correlations
with topography. A preliminary high-resolution 150 degrees and order model for low-lunar
orbit determination is also presented. Furthermore, preliminary results from the analysis ofsame-beam differential VLBI data are also included, showing how these data can especially

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help to improve orbit determination for the sub-satellites. The VLBI data will also contributeto a precise determination of the lower-degree gravity coefficients.
Gopalswamy, N., S. Yashiro, and K. Shibasaki [2008], "Heating and Kinematics of an Eruptive
Prominence Associated with a Fast Coronal Mass Ejection," American Geophysical Union,
Fall Meeting 2007, abstract #SH31C-07.
The fast (1800 km/s) coronal mass ejection (CME) on 2005 July 27 had a bright bubble-shaped
prominence core observed by the Nobeyama Radioheliograph (NoRH) in microwaves (17 and
34 GHz), TRACE at 171 A, and the Extreme-ultraviolet Imaging Telescope (EIT) on board
SOHO. NoRH has the largest field of view among the non- white light instruments, so theprominence could be tracked until it reached a height of about 0.75 solar radii from the limb.
The prominence remained optically thick at both 17 and GHz, even though it was significantly
heated. Comparison with TRACE observations suggest that the prominence was heated inindividual fibers within the prominence, making it multi-thermal plasma.
The prominence maintained its overall shape as it entered into the field of view of
SOHO/LASCO coronagraphs with a speed of about 1400 km/s, so the height-time history
could be studied over a distance of more than 20 solar radii from the Sun. NoRH data indicatedthat the initial acceleration was extremely high (about1.4 km/s/s). During the slow-rise phaseof the prominence, EUV loops overlying the prominence also moved out, which whencombines with CME leading-edge measurements from LASCO/C2 yielded an acceleration of
about 300 m/s/s. This was comparable to the average acceleration of the prominence over thesame height range. When we consider the just the LASCO field of view, both the prominencecore and the CME leading edge showed deceleration, but to vastly different extents (-32 m/s/s
for the CME leading edge compared to -3 m/s/s for the prominence core). Our preliminary
conclusion is that the prominence was insulated from interacting with the non-CME ambient
medium, which might explain the weaker slowing down of the prominence.
Gopalswamy, N., S. Yashiro, K. Shibasaki, and D. Hathaway [2010], "Polar ChromosphericSignatures of the Subdued Cycle 23/24 Solar Minimum," American. Astron. Soc., AAS
Meeting #216, #401.03.
Coronal holes appear brighter than the quiet Sun in microwave images, with a brightness
enhancement of 500 to 2000 K. The brightness enhancement corresponds to the upper
chromosphere, where the plasma temperature is about 10000 K. We constructed a microwave
butterfly diagram using the synoptic images obtained by the Nobeyama radioheliograph(NoRH) showing the evolution of the polar and low latitude brightness temperature. While thepolar brightness reveals the chromospheric conditions, the low latitude brightness is attributed
to active regions in the corona. When we compared the microwave butterfly diagram with themagnetic butterfly diagram, we found a good correlation between the microwave brightness
enhancement and the polar field strength. The microwave butterfly diagram covers part ofsolar cycle 22, whole of cycle 23, and part of cycle 24, thus enabling comparison between thecycle 23/24 and cycle 22/23 minima. The microwave brightness during the cycle 23/24
minimum was found to be lower than that during the cycle 22/23 minimum by 250 K. The
reduced brightness temperature is consistent with the reduced polar field strength during thecycle 23/24 minimum seen in the magnetic butterfly diagram. We suggest that the microwave
brightness at the solar poles is a good indicator of the speed of the solar wind sampled by
Ulysses at high latitudes.
Grechnev, V. V., V. G. Kurt, I. M. Chertok, A. M. Iralov, H. Nakajima, A. T. Altyntsev, A. V.
Belov, B. Yu. Yushkov, S. N. Kuznetsov, L. K. Kashapova, N. S. Meshalkona, and N. P.
Prestage [2008a], "An Extreme Solar Events of 20 January 2005: Properties of the Flare andthe Origon of Energetic Particles," Solar Phys., vol.252, pp.149-177.
The famous extreme solar and particle event of 20 January 2005 is analyzed from two

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perspectives. Firstly, using multi-spectral data, we study temporal, spectral, and spatial featuresof the main phase of the flare, when the strongest emissions from microwaves up to 200 MeV
gamma-rays were observed. Secondly, we relate our results to a long-standing controversy on
the origin of solar energetic particles (SEP) arriving at Earth, i.e., acceleration in flares, orshocks ahead of coronal mass ejections (CMEs). Our analysis shows that all electromagnetic
emissions from microwaves up to 2.22 MeV line gamma-rays during the main flare phaseoriginated within a compact structure located just above sunspot umbrae. In particular, a huge(≈105 sfu) radio burst with a high frequency maximum at 30 GHz was observed, indicating thepresence of a large number of energetic electrons in very strong magnetic fields. Thus,
protons and electrons responsible for various flare emissions during its main phase wereaccelerated within the magnetic field of the active region. The leading, impulsive parts of theground-level enhancement (GLE), and highest-energy gamma-rays identified withπ0-decayemission, are similar and closely correspond in time. The origin of theπ 0-decay
gamma-rays is argued to be the same as that of lower-energy emissions, although this is notproven. On the other hand, we estimate the sky-plane speed of the CME to be 2000-2600km s-1,
i.e., high, but of the same order as preceding non-GLE-related CMEs from the same active
region. Hence, the flare itself rather than the CME appears to determine the extreme nature ofthis event. We therefore conclude that the acceleration, at least, to sub-relativistic energies, ofelectrons and protons, responsible for both the major flare emissions and the leading spike of
SEP/GLE by 07 UT, are likely to have occurred nearly simultaneously within the flare region.
However, our analysis does not rule out a probable contribution from particles accelerated in
the CME-driven shock for the leading GLE spike, which seemed to dominate at later stagesof the SEP event.
Grechnev, V. V., A. M. Uralov, V. A. Slemzin, I. M. Chertok, I. V. Kuzmenko, and K. Shibasaki[2008b], "Absorption Phenomena and a Probable Blast Wave in the 13 July 2004 Eruptive
Event," Solar Phys., vol.253, pp.263-290.
We present a case study of the 13 July 2004 solar event, in which disturbances caused byeruption of a filament from an active region embraced a quarter of the visible solar surface.
Remarkable are the absorption phenomena observed in the SOHO/EIT 304 Å channel, whichwere also visible in the EIT 195 Å channel, in the H line, and even in total radio flux records.
Coronal and Moreton waves were also observed. Multispectral data allowed reconstructing an
overall picture of the event. An explosive filament eruption and related impulsive flare
produced a CME and blast shock, both of which decelerated and propagated independently.
Coronal and Moreton waves were kinematically close and both decelerated in accordance withan expected motion of a coronal blast shock. The CME did not resemble a classicalthree-component structure, probably because some part of the ejected mass fell back onto theSun. Quantitative evaluations from different observations provide close estimates of the falling
mass, ~3x1015 g, which is close to the estimated mass of the CME. The falling material was
responsible for the observed large-scale absorption phenomena, in particular, shallow
widespread moving dimmings observed at 195 Å. By contrast, deep quasi-stationary dimmings
observed in this band near the eruption center were due to plasma density decrease in coronal
structures.
Greenhill, L., E. Humphreys, W. Hu, L. Macri, D. Murphy, K. Masters, Y. Hagiwara, H.
Kobayashi, and Y. Murata [2009], "Estimation of the Hubble Constant and Constraint on
Descriptions of Dark Energy," Astro2010: The Astronomy and Astrophysics Decadal Survey,
Science White Papers, no. 103-0-7.
Joint analysis of Cosmic Microwave Background, Baryon Acoustic Oscillation, and supernova
data has enabled precision estimation of cosmological parameters. New programs will push to
1% uncertainty in the dark energy equation of state and tightened constraint on curvature,

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requiring close attention to systematics. Direct 1% measurement of the Hubble constant (H0)would provide a new constraint. It can be obtained without overlapping systematics directlyfrom recessional velocities and geometric distance estimates for galaxies via the mapping ofwater maser emission that traces the accretion disks of nuclear black holes. We identify
redshifts 0.02<z<0.06 as best for small samples, e.g., 10 widely distributed galaxies, each with
3% distance uncertainty. Knowledge of peculiar radial motion is also required. Mapping
requires very long baseline interferometry (VLBI) with the finest angular resolution,
sensitivity to individual lines of a few mJy-km/s, and baselines that can detect a complex of~10 mJy lines (peak) in < 1 min. For 2010-2020, large ground apertures (50-100m diameter)
augmenting the VLBA are critical, such as EVLA, GBT, Effelsberg, and the Large Millimeter
Telescope, for which we propose a 22 GHz receiver and VLBI instrumentation. A space-VLBI
aperture may be required, thus motivating US participation in the Japanese VSOP-2 mission(launch c.2013). This will provide 3-4x longer baselines and ~5x improvement in distanceuncertainty. There are now 5 good targets at z>0.02, out of ~100 known masers. A single-dishdiscovery survey of >10,000 nuclei (>2500 hours on the GBT) would build a sample of tens ofpotential distance anchors. Beyond 2020, a high-frequency SKA could provide larger maser
samples, enabling estimation of H0 from individually less accurate distances, and possibly
without the need for peculiar motion corrections.
Hagiwara, Y., and VSOP-2 Science Working Group [2009], "Extragalactic Water Maser
Observations with VSOP-2," Proc. of the "Approaching Micro-Arcsecond Resolution with
VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and
Murata, Y., ASP Conf. Ser. vol.402, pp.266-269.
Space-VLBI is known to achieve greatly increased angular resolution compared withground-based VLBI observations. VSOP-2 will offer 75μ arcsec angular resolution at 22 GHz.
With this improved angular resolution, VSOP-2 observations of H2O megamaser will refine
the measurements of proper motions, accelerations, distances to galaxies, and other physicalparameters of galactic nuclei. In this presentation, the prospects of VSOP-2 observations of
extragalactic H2O maser with strong emphasis on H2O megamaser are presented.
Hanada, H., T. Iwata, N. Namiki, N. Kawano, K. Asari, T. Ishikawa, F. Kikuchi, Q. Liu, K.
Matsumoto, H. Noda, S. Tsuruta, S. Goossens, K. Iwadate, O. Kameya, Y. Tamura, X. Hong, J.
Ping, Y. Aili, S. Ellingsen, and W. Schlüter [2008a], "VLBI for Better Gravimetry in
SELENE," Adv. Sp. Res., vol.42, pp.341-346.
The Japanese lunar explorer SELENE (SElenological and Engineering Explorer), to belaunched in 2007, will for the first time utilize VLBI observations in lunar gravimetry
investigations. This will particularly improve the accuracy to which the low degree
gravitational harmonics and the gravity field near the limb can be measured, and whencombined with Doppler measurements will enable three-dimensional information to be
extracted. Differential VLBI Radio sources called VRAD experiment involves two on-board
sub-satellites, Rstar and Vstar. These will be observed using differential VLBI to measure thetrajectories of the satellites with the Japanese network named VERA (VLBI Exploration ofRadio Astrometry) and an international VLBI network. We will use a multi-frequency VLBI
method to measure the angular distance between the two sub-satellite radio sources Rstar andVstar. The observations will be at three frequencies in S-band, 2212, 2218 and 2287 MHz, andone in X-band, 8456 MHz. This method uses low power consumption carrier waves, and issuitable for the positioning of spacecraft. The Japanese domestic VLBI network, VERA, willconduct VLBI observations for the whole mission period of one year. In addition, we willconduct two periods of intensive observations, each one month in duration, which will also
include the international stations, Shanghai, Urumqi (China), Hobart (Australia) and Wettzell(Germany). These observations will measure the phase delay to an accuracy of better than 0.17

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rad (10 deg) in X-band. For a baseline length of 2000 km this is equivalent to a positioning
accuracy of about 20 cm on the Moon. Combining the data from the tracking of the 3 SELENE
satellites (main orbiter, Rstar and Vstar) at different altitudes and from four-way Doppler
measurements, and by making long term observations of the sub-satellites (in excess of one
year without any maneuvering), we will be able to improve the accuracy to which the lunar
gravitational field is known by an order of magnitude. We have completed the development of
on-board instruments, and are carrying out pre-flight tests under a variety of conditions. We
have also undertaken test VLBI observations of orbiters such as Geotail, Nozomi and Smart-1
with the international network.
Hanada, H. [2008b], "VLBI Observation of Okina and Ouna in Kaguya (SELENE) for
Improvement of Orbit Determination and Lunar Gravity Field Model," 37th COSPAR
Scientific Assembly, held 13-20 July 2008, in Montreal, Canada, p.1168.
KAGUYA consists of the main orbiter, and two small free-flying sub-satellites, called Rstar(OKINA) and Vstar (OUNA). We are observing OKINA and OUNA using differential VLBI
observa-tions with the aim of improving the lunar gravity field model. Our observations will
particularly improve the accuracy to which the low degree gravitational harmonics and thegravity field near the limb can be measured, and when combined with Doppler measurements
will enable three-dimensional information to be extracted. Differential VLBI will be used toaccurately measure the trajectories of the satellites, both with the Japanese VERA (VLBI
Exploration of Radio Astrometry) telescopes and an array including the international VLBI
stations, Shanghai, Urumqi (China), Hobart (Australia), and Wettzell (Germany). We are using
multi-frequency VLBI to determine the angular distance between OKINA and OUNA using
three frequencies in S-band, (2212, 2218 and 2287 MHz), and one in X-band, (8456MHz).
Two periods of international observations, each of one month in duration, with theparticipation of VERA and the international stations, (in addition to the normal observations by
VERA only) are planned for the one year mission period. VLBI observation was started on
Nov.5, 2007 and the first international VLBI observation was per-formed in Jan, 2008. We
have succeeded in obtaining phase delays with an accuracy of several pico-seconds in S-band.
Hanada, H., T. Iwata, N. Namiki, N. Kawnao, S. Sasaki, K. Matsumoto, H. Noda, S. Tsuruta, K.
Asari, T. Ishikawa, F. Kikuchi, Q. Liu, S. Goossens, K. M. Shibata, K. Iwadate, O. Kameya, Y.
Tamura, X. Hong, J. Ping, Y. Aili, S. Ellingsen, and W. Schluter [2009], "The Explorations of
Lunar Gravity by VLBI Observations of SELENE (Kaguya)," Trans. of Sp. Tech. Japan, vol.7,
pp.Tk1-Tk5.
SELENE (Kaguya), which was successfully launched on Sep. 14, 2007, consists of the main
orbiter, and two small free-flying sub-satellites, called Rstar (OKINA) and Vstar (OUNA). We
use multi-frequency VLBI to measure the angular distance between the two sub-satellite radiosources Okina and Ouna in order to improve the accuracy of the low degree gravitational
harmonics and the gravity field near the limb. The observations are made at three frequencies
in S-band, (2212, 2218 and 2287 MHz), and one in X-band, (8456MHz) with carrier waves.
The Japanese domestic VLBI network, VERA, will conduct VLBI observations for the whole
mission period of one year. In addition, we will conduct two periods of international
observations, each one month in duration, which will also include the international stations,
Shanghai, Urumqi, Hobart, and Wettzell. We have succeeded in making VLBI observations of
Okina/Ouna with VERA and the international network, and have also succeeded in correlatingof signals from Okina/Ouna. We obtained phase delays with an accuracy of several
pico-seconds in S-band.
Haruyama, J., M. Ohtake, T. Matsunaga, T. Morota, C. Honda, Y. Yokota, M. Abe, Y. Ogawa,H. Miyamoto, A. Iwasaki, C. M. Pieters, N. Asada, H. Demura, N. Hirata, J. Terazono, S.
Sasaki, K. Saiki, A. Yamaji, M. Torii, and J.-L. Josset [2009], "Long-Lived Volcanism on the

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Lunar Farside Revealed by SELENE Terrain Camera," Science, vol.323, pp.905-908.
We determined model ages of mare deposits on the farside of the Moon on the basis of thecrater frequency distributions in 10-meter-resolution images obtained by the Terrain Camera
on SELENE (Selenological and Engineering Explorer) (Kaguya). Most mare volcanism thatformed mare deposits on the lunar farside ceased at ~3.0 billion years ago, suggesting thatmare volcanism on the Moon was markedly reduced globally during this period. However,
several mare deposits at various locations on the lunar farside also show a much younger age,clustering at ~2.5 billion years ago. These young ages indicate that mare volcanism on the
lunar farside lasted longer than was previously considered and may have occurred episodically.
Hasegawa, T., T. Arai, N. Yamaguchi, and F. Sato [2008], "ASTE Observations of theMassive-Star Forming Region Sgr B2: a Giant Impact Scenario," Astrophys. and Sp. Sci.,
vol.313, pp.91-94.
We report mapping observations of a 35 pc x 35 pc region covering the Sgr B2 molecular
cloud complex in the 13CO (3-2) and the CS (7-6) lines using the ASTE 10 m telescope withhigh angular resolution. The central region was mapped also in the C18O (3-2) line. The images
not only reproduce the characteristic structures noted in the preceding millimeter observations,but also highlight the interface of the molecular clouds with a large velocity jump of a few tensof km s-1. These new results further support the scenario that a cloud-cloud collision has
triggered the formation of massive cloud cores, which form massive stars of Sgr B2. Prospectsof exciting science enabled by ALMA are discussed in relation to these observations.
Hatsukade, B., D. Iono, K. Motohara, K. Nakanishi, M. Hayashi, K. Shimasaku, T. Nagao, Y.
Tamura, M. Malkan, C. Ly, and K. Kohno [2009], "A Search for Molecular Gas toward a
BzK-Selected Star-Forming Galaxy at z = 2.044," Publ. Astron. Soc. Japan, vol.61,
pp.487-491.
We present a search for CO (3-2) emission in SDF-26821, a BzK -selected star forming galaxy(sBzK) at z = 2.044, using the 45-m telescope of the Nobeyama Radio Observatory and theNobeyama Millimeter Array. We did not detect significant emission, and derived the 2σ limits:
CO luminosity of L' CO < 3.1
x 1010 K km s-1 pc-2, ratio of far-infrared luminosity to CO luminosity of LFIR /L'CO > 57 L ⦿(Kkm s-1 pc2)-1, and molecular gas mass of MH2 < 2.5 x 1010 M ⦿, assuming a velocity width of
200 km s-1 and a CO-to-H2 conversion factor of αCO = 0.8 M⦿ (K km s-1 pc2)-1. The ratio
LFIR=L'CO, a measure of the star-formation efﬁciency (SFE), is comparable to, or higher than,
the two z ~ 1.5 sBzKs detected in CO (2 ﾐ 1) previously, suggesting that sBzKs can have awide range of SFEs. Comparisons of far-infrared luminosity, gas mass, and stellar mass among
the sBzKs suggest that SDF-26821 is at an earlier stage of forming stars with a similar SFE
and/or more ef ﾞ ciently forming stars than the two z ~ 1.5 sBzKs. The higher SFEs and speci ﾞc star-formation rates of the sBzKs compared to local spirals are indicative of a difference inthe star-formation modes between these systems, suggesting that sBzKs are not just scaled-up
versions of local spirals.
Hatsukade, B., D. Iono, M. Akiyama, T. Yoshikawa, J. S. Dunlop, R. J. Ivison, A. B. Peck, S.
Ikarashi, A. Briggs, H. Ezawa, H. Hanami, P. Ho, D. H. Hughes, R. Kawabe, K. Kohno, S.
Matsushita, K. Nakanishi, N. Padilla, G. Petitpas, Y. Tamura, J. Wagg, D. J. Wilner, G. W.
Wilson, T. Yamada, and M. S. Yun [2010a], "Unveiling the Nature of Submillimeter Galaxy
SXDF 850.6," Astrophys. J., vol.711, pp.974-979.
We present an 880 μm Submillimeter Array (SMA) detection of the submillimeter galaxy
SXDF 850.6. SXDF 850.6 is a bright source (S850μm = 8 mJy) detected in the SCUBA Half
Degree Extragalactic Survey and has multiple possible radio counterparts in its deep radio
image obtained at the VLA. Our new SMA detection finds that the submillimeter emission
coincides with the brightest radio emission that is found ~8'' north of the coordinates

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determined from SCUBA. Despite the lack of detectable counterparts in deep UV/opticalimages, we find a source at the SMA position in near-infrared and longer wavelength images.
We perform spectral energy distribution (SED) model fits to UV-optical-IR photometry (u, B,
V, R, i', z', J, H, K, 3.6 μm, 4.5 μm, 5.8 μm, and 8.0 μm) and to submillimeter-radio
photometry (850 μm, 880 μm, 1100 μm, and 21 cm) independently, and we find both are welldescribed by starburst templates at a redshift of z ∼ 2.2± 0.3. The best-fit parameters from the
UV-optical-IR SED fit are a redshift of z = 1.87+0.15-0.07, a stellar mass of M∼ = 2.5+2.2-0.3 ×1011
M ⦿, an extinction of AV = 3.0+0.3-1.0 mag, and an age of 720+1880-210 Myr. The
submillimeter-radio SED fit provides a consistent redshift of z ~ 1.8-2.5, an IR luminosity of
LIR = (7-26)×1012 L ⦿, and a star formation rate of 1300-4500 M⦿yr-1. These results suggest that
SXDF 850.6 is a mature system already having a massive amount of old stellar population
constructed before its submillimeter bright phase and is experiencing a dusty starburst,
possibly induced by major mergers.
Hatsukade, B., K. Kohno, Y. Tamura, K. Nakanishi, D. Iono, G. W. Wilson, M. S. Yun, D. H.
Hughes, S. Matsuura, M. Shirahata, T. T. Takeuchi, K. S. Scott, J. E. Austermann, T. Perera, I.
Aretxaga, K. Tanaka, T. Tosaki, H. Matsuo, H. Ezawa, R. Kawabe, and ADF-S team [2010b],"AzTEC/ASTE 1.1-mm Survey of the AKARI Deep Field-South," Proc. of the "AKARI, alight to illuminate the misty universe", eds. T. Onaka, G. J. White, T. Nakagawa, and I.
Yamamura, ASP Conf. Ser. vol.418, pp.307-312.
We present the first results of a deep 1.1-mm survey of the AKARI Deep Field-South (ADF-S)
with the AzTEC camera on the Atacama Submillimetre Telescope Experiment (ASTE). Thissurvey covers ~400 arcmin2, of which the central 202 arcmin2 is a uniform low-noise region
with an rms noise level of 0.48-0.71 mJy. This is one of the deepest surveys at 1-mm
wavelength, to cover such a large contiguous region. We detected 37 sources with asignificance of 3.5–10 σ. The expected number of false detections at ≥3.5 σ is at most one,indicating that the detected sources are highly reliable. We construct differential andcumulative number counts and find a difference in number counts among 1-mm blank fieldsurveys: the number counts of the ADF-S are less than those of GOODS-N and COSMOS
fields. Most of the sources are not detected in the far-infrared bands of the AKARI, suggestingthat they lie mostly at z ga 1 given the detection limits. In this survey, about 10% of cosmic
infrared background at 1.1 mm is resolved into discrete sources.
Hatsukade, B., K. Kohno, I. Aretxaga, J. E. Austermann, H. Ezawa, D. H. Hughes, S. Ikarashi,
D. Iono, R. Kawabe, H. Matsuo, K. Nakanishi, T. Oshima, T. Perera, K. S. Scott, M. Shirahata,
T. T. Takeuchi, Y. Tamura, K. Tanaka, T. Tosaki, G. W. Wilson, and M. S. Yun [2010c],"AzTEC/ASTE 1.1 mm Deep survey: Number Counts and Clustering of Millimeter-Bright
Galaxies," AIP Conf. Proc., vol.1279, pp.324.
We present number counts and clustering properties of millimeter-bright galaxies uncoveredby the AzTEC camera mounted on the Atacama Submillimeter Telescope Experiment (ASTE).
We surveyed the AKARI Deep Field South (ADF-S), the Subaru/XMM Newton Deep Field(SXDF), and the SSA22 fields with an area of ~0.25 deg2 each with an rms noise level of~0.4-1.0 mJy. We constructed differential and cumulative number counts, which provide
currently the tightest constraints on the faint end. The integration of the best-fit number counts
in the ADF-S find that the contribution of 1.1 mm sources with fluxes ≥1 mJy to the cosmic
infrared background (CIB) at 1.1 mm is 12-16%, suggesting that the large fraction of the CIB
originates from faint sources of which the number counts are not yet constrained. We estimate
the cosmic star-formation rate density contributed by 1.1 mm sources with >=1 mJy using thebest-fit number counts in the ADF-S and find that it is lower by about a factor of 5-10
compared to those derived from UV/optically-selected galaxies at z~2-3. The average mass ofdark halos hosting bright 1.1 mm sources was calculated to be 1013-1014 M⦿. Comparison of

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correlation lengths of 1.1 mm sources with other populations and with a bias evolution model
suggests that dark halos hosting bright 1.1 mm sources evolve into systems of clusters atpresent universe and the 1.1 mm sources residing the dark halos evolve into massive ellipticalgalaxies located in the center of clusters.
Higuchi, A. E., Y. Kurono, M. Saito, and R. Kawabe [2009], "A Mapping Survey of Dense
Clumps Associated with Embedded Clusters : Evolutionary Stages of Cluster-Forming
Clumps," Astrophys. J., vol.705, pp.468-482.
We have carried out a survey of the dense clumps associated with 14 embedded clusters in the
C18O (J = 1-0) line emission with the Nobeyama 45 m telescope in order to understand theformation and evolution of stellar clusters in dense clumps of molecular clouds. We haveselected these clusters at distances from 0.3 to 2.1 kpc and have mapped about 6'x6'-10' x 10'
regions (corresponding to 3.8 pc x 3.8 pc at 2.1 kpc) for all the clumps with 22'' resolution(corresponding to Jeans length at 2.1 kpc). We have obtained dense clumps with radii of
0.40-1.6 pc, masses of 150-4600 M⦿, and velocity widths in FWHM of 1.4-3.3 km s-1. Most of
the clumps are found to be approximately in virial equilibrium, which implies that C18O gas
represents parental dense clumps for cluster formation. From the spatial relation between the
distributions of clumps and clusters, we classified C18O clumps into three types (Type A, B,
and C). Type A clumps have emission distributions with a single peak at the stellar clusters andhigher brightness contrast than that of other target sources. Type B clumps have double or
triple peaks, which are associated with the cluster, and moderately high brightness contrast
structure. Type C clumps also have multiple peaks, although they are not associated with thecluster, and low brightness contrast structure. We suggest that our classification represents anevolutionary trend of cluster-forming dense clumps because dense gas in molecular clouds is
expected to be converted into stellar constituents, or dispersed by stellar activities. Moreover,although there is a scatter, we found a tendency that the star formation efficiencies of the dense
clumps increase from Type A to Type C, which also supports our scenario.
Higuchi, A. E., Y. Kurono, M. Saito, and R. Kawabe [2010], "A Mapping Survey of Dense
Associated with Embedded Clusters II: Can Clump-Climp Collisions Induce Stellar Clusters?,"
Astrophys. J., vol.719, pp.1813-1827.
We report the H13CO+ (J = 1-0) survey observations toward embedded clusters obtained using
the Nobeyama 45 m telescope, which were performed to follow up our previous study in the
C18O survey with a dense gas tracer. Our aim is to address the evolution of cluster-forming
clumps. We observed the same 14 clusters in C18O, which are located at distances from 0.3 to
2.1 kpc with a 27'' resolution (corresponding to the Jeans length for most of our targets) in
H13CO+. We detected the 13 clumps in H13CO+ line emission and obtained the physicalparameters of the clumps with radii of 0.24-0.75 pc, masses of 100-1400 Msun, and velocity
widths in FWHM of 1.5-4.0 km s-1. The mean density is ~3.9 x 104 cm-3 and the equivalent
Jeans length is ~0.13 pc at 20 K. We classified the H13CO+ clumps into three types, type A,
type B, and type C according to the relative locations of the H13CO+ clumps and the clusters(see our previous study). Our classification represents an evolutionary trend of cluster-forming
clumps because dense clumps are expected to be converted into stellar constituents, ordispersed by stellar activities. We found a similar, but clearer trend than our previous results,
for derived star formation efficiencies to increase from type A to C in the H13CO+ data, and forthe dense gas regions within the clumps traced by H13CO+ to be sensitive to the physicalevolution of the clump-cluster systems. In addition, we found that 4 out of 13 H13CO+ clumps,
which we named "Distinct Velocity Structure Objects" (DVSOs), have distinct velocity
gradients at their central parts, i.e., at the location of the embedded clusters. Assuming that thevelocity gradients represent the rigid-like rotation of the clumps, we calculated the virial
parameter of the H13CO+ clumps by taking into account the contribution of the rotation and

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found that the DVSOs tend to be gravitationally unbound. In order to explain the above
physical properties for DVSOs in a consistent way, we propose a clump-clump collision model
as a possible mechanism for triggering the formation of clusters.
Higuchi, K., N. Kishimoto, T. Mizuno, K. Kawahara, S. Tachikawa, Y. Murata, M. Tsuboi, H.
Ogawa, S. Kimura, H. Ujihara, A. Meguro, H. Tanaka, M. Yoshihara, and S. IIkura [2009],"VSOP-2 Antenna and its Structure," Proc. of the "Approaching Micro-Arcsecond Resolution
with VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M.,
and Murata, Y., ASP Conf. Ser. vol.402, pp.41-45.
To achieve scientific improvements from VSOP (HALCA) to VSOP-2 (ASTRO-G), thesatellite design incorporates the engineering characteristics of a large-scale deployable antennaof offset Cassegrain type with observation bands of 8, 22, and 43 GHz. The antenna subsystem
requires the surface accuracy of 0.4mm RMS on the main reflector named LDR (Large-scale
Deployable Reflector) of about 9m in diameter. An off-axis paraboloid reflector is adopted toachieve this surface accuracy for millimeter-wave observation. The main reflector is composedof seven deployable modular antennas, and each of the modules employs a new idea ofradial-rib/hoop-cable reflector construction to stretch metal mesh and to satisfy the required
surface accuracy. The deployment mechanism employs most of the LDR technology developed
for JAXA’s ETS-VIII satellite, which was launched in December 2006, and both of the twoantennas on the ETS-VIII deployed successfully on orbit. Some prototype models of one
module have been made to investigate the surface accuracy. In addition, the antenna will havea two-axis adjustment mechanism for the main reflector, and a three-axis adjustment
mechanism for the sub-reflector in order to optimize the antenna gain after deployment inorbit.
Hiramatsu, M., N. Hirano, and S. Takakuwa [2010], "Outflow - Core Interaction in Barnard 1,"
Astrophys, J., vol.712, pp.778-789.
In order to study how outflows from protostars influence the physical and chemical conditionsof the parent molecular cloud, we have observed the Barnard 1 (B1) main core, which harbors
four Class 0 and three Class I sources, in the CO (J = 1 - 0), CH3OH (JK = 2K - 1K), and theSiO (J = 1 - 0) lines using the Nobeyama 45 m telescope. We have identified three CO
outflows in this region: one is an elongated (~0.3 pc) bipolar outflow from a Class 0 protostar
B1-c in the submillimeter clump SMM 2, another is a rather compact (~0.1 pc) outflow from a
Class I protostar B1 IRS in the clump SMM 6, and the other is an extended outflow from a
Class I protostar in SMM 11. In the western lobe of the SMM 2 outflow, both the SiO andCH3OH lines show broad redshifted wings with the terminal velocities of 25 km s-1 and 13 km
s-1, respectively. It is likely that the shocks caused by the interaction between the outflow andambient gas enhance the abundance of SiO and CH3OH in the gas phase. The total energy
input rate by the outflows (1.1 × 10–3 L⦿) is smaller than the energy-loss rate (8.5 × 10–3 L⦿)through the turbulence decay in the B1 main core, which suggests that the outflows cannot
sustain the turbulence in this region. Since the outflows are energetic enough to compensate
the dissipating turbulence energy in the neighboring, more evolved star-forming region NGC
1333, we suggest that the turbulence energy balance depends on the evolutionary state of thestar formation in molecular clouds.
Hirata, N., O. S. Barnouin-Jha, C. Honda, R. Nakamura, H. Miyamoto, S. Sasaki, H. Demura,A. M. Nakamura, T. Michikami, R. W. Gaskell, and J. Saito [2009], "A Survey of Possible
Impact Structures on 25143 Itokawa," Icarus, vol.200, pp.486-502.
We determined the morphologies and dimensions of possible impact craters on the surface ofAsteroid 25143 Itokawa from images taken by the Hayabusa spacecraft. Circular depressions,circular features with flat floors or convex floors, and circular features with smooth surfaces
were identified as possible craters. The survey identified 38 candidates with widely varying

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morphologies including rough, smooth and saddle-shaped floors, a lack of raised rims andfresh material exposures. The average depth/diameter ratio was 0.08±0.03: these craters arevery shallow relative to craters observed on other asteroids. These shallow craters are a resultof (1) target curvature influencing the cratering process, (2) raised rim not being generated bythis process, and (3) fines infilling the craters. As many of the crater candidates have an
unusual appearance, we used a classification scheme that reflects the likelihood of an observed
candidate's formation by a hypervelocity impact. We considered a variety of alternativeinterpretations while developing this scheme, including inherited features from a
proto-Itokawa, spall scars created by the disruption of the proto-Itokawa, spall scars following
the formation of a large crater on Itokawa itself, and apparent depressions due to randomarrangements of boulders. The size-frequency distribution of the crater candidates was close to
the empirical saturation line at the largest diameter, and then decline with decreasing diameter.
Hiroi, T., T. Nimura, Y. Ueda, S. Sasaki, and C. M. Pieters [2008a], "Deriving theDistribution of Ordinary Chondrite (H, L, LL)-like Materials in Asteroids from Their Visible
and Near-Infrared Reflectance Spectroscopy," 39th Lunar and Planetary Science Conference,(Lunar and Planetary Science XXXIX), held March 10-14, 2008 in League City, Texas. LPI
Contribution No. 1391, p.1997.
We have attempted to identify asteroid surface materials similar to ordinary chondrite types by
examining reflectance spectra of the S, A, R, and V asteroids over the 1- m band range, andderive their distributions.
Hiroi, T., M. Abe, T. Nimura, K. Kitazato, S. Abe, Y. Takagi, S. Sasaki, and M. Ishiguro [2008],"Danger in Interpreting the 2-Micron Band of Reflectance Spectra of Small Asteroids: A
Lesson from Hayabusa/NIRS Data of Itokawa," Meteoritics and Planetary Sci. Suppl., 43,
paper id. 5283.
Not Available
Hirota, A., N. Kuno, N. Sato, T. Tosaki, H. Nakanishi, and K. Sorai [2008b], "GMCs in the
Nearby Galaxy IC 342," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds. Wada,K., and Combes, F., p.334.
Without abstract
Hirota, A., N. Kuno, N. Sato, H. Nakanishi, T. Tosaki, H. Matsui, A. Habe, and K. Sorai [2009],"Determination of the Pattern Speed of Barred Spiral Galaxies," Publ. Astron. Soc. Japan,
vol.61, pp.441-450.
We evaluated the availability of a method proposed by Kuno et al. (2000, PASJ, 52, 775) for
measuring the pattern speed of barred galaxies, and applied it to observational data. We madeerror estimations using a hydro-dynamical galaxy model to test the validity of the method.
Error estimations suggest that the method is able to determine the pattern speed within an errorof 10%-20%. The method was applied to 12CO(1-0) data of three late-type barred galaxies:
NGC 2903, M 83, and NGC 3627. The derived pattern speed was 40 km s-1 kpc-1 for NGC
2903, 57 km s-1 kpc-1 for M 83, 39 km s-1 kpc-1 for NGC 3627, respectively. For the sake of acomparison with measurements in other galaxies, we used the distance-independent value R( RCR/Rbar), and found that bars in the three late-type spirals are “slow” (R > 1.4). Our results
support recent claims that bars are not always “fast” (R ≤ 1.4), at least for late-type spiralgalaxies.
Hirota, A., N. Kuno, N. Sato, H. Nakanishi, T. Tosaki, and K. Sorai [2010], "Variation of
Molecular Gas Properties Across the Spiral Arms in IC 342: Large-Scale 13CO (1-0)
Emission," Publ. Astron. Soc. Japan, vol.62, pp.1261-1275.
We present a 13CO (1-0) mapping survey of the nearby galaxy IC 342 carried out with theNobeyama 45m radio telescope. The map covers a 32" x 32" region including its center, bar,and most of one of the spiral arms. The 13CO (1-0) data were compared with 12CO (1-0), Hα,

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24μm, and Ks-band images to investigate spatial relations among molecular clouds,
star-forming regions, and the stellar potential. The line ratio between both CO lines, I [13CO(1-0)]=I [12CO (1-0)] ≡ R13/12, was also derived to investigate the variation of molecular gas
properties. The mean value of R13/12 in the center of IC 342 is low (~0.10±0.01) compared tothe disk region (~0.15±0.01). While R13/12 in the central region is rather uniform, significant
variations of R13/12 were found in the spiral arms; that is, while it is low (~0.1) at both ends ofthe bar and at the giant molecular cloud association (GMA) found in the spiral arm, it is high(0.14-0.20) downstream from the low R13/12 region. The low- and high-R13/12 regions in thedisk correspond to the 12CO peak and star-forming regions, respectively. The low R13/12 in thegalactic center is likely due to the higher gas temperature in the starburst region. The mostprobable explanation of the R13/12 variation in the disk is that a low R13/12 in the GMA and theends of the bar reflects an increased fraction of the diffuse molecular component, which has a
low column density and low volume density. Around the GMA and the north end of the bar,
not only are the star-forming regions downstream from the CO distributions, but R13/12 is also
higher downstream implying the presence of gas compression and ionized/molecular gas
spatial offsets, as predicted by density wave models.
Hirota, T. [2008a], "Observations of H2O Maser Sources in Nearby Molecular Clouds with
VERA," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes,
F., p.335.
Without abstract
Hirota, T., T. Bushimata, Y. K. Choi, M. Honma, H. Imai, K. Iwadate, T. Jike, S. Kameno, O.
Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, M. K. Kim, H. Kobayashi, S.
Kuji, T. Kurayama, S. Manabe, K. Maruyama, M. Matsui, N. Matsumoto, T. Miyaji, T.
Nagayama, A. Nakagawa, K. Nakamura, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, T. Sasao,
K. Sato, M. Sato, K. M. Shibata, M. Shintani, Y. Tamura, M. Tsushima, and K. Yamashita[2008b], "Astrometry of H2O Maser Sources in Nearby Molecular Clouds with VERA," Proc.
of the IAU Symp. 242, "Astrophysical Masers and their Environments", eds. Jessica Chapman
and Willem Baan, pp.158-159.
We have carried out multi-epoch VLBI observations of the H2O maser sources associated withyoung stellar objects (YSOs) in nearby molecular clouds with VERA (VLBI Exploration ofRadio Astrometry), which is a newly constructed VLBI network in Japan (Kobayashi et al.
2003). The main goal of our study is to measure the absolute proper motions and distances tonearby molecular clouds within 1 kpc from the Sun, to reveal their 3-dimensional structuresand dynamical properties. Using the VERA dual-beam receiving system (Honma et al. 2003),
we have carried out phase-referencing VLBI observations and measured annual parallaxes andabsolute proper motions of the H2O maser features with respect to the extragalactic radiosources. We have successfully detected the annual parallax of one of the H2O maser features inOrion KL to be 2.29±0.10 mas, corresponding to the distance of 437±19 pc from the Sun(Hirota et al. 2007). In addition, the annual parallax of SVS13 in NGC 1333 is also determined
to be4.10±0.17 mas, corresponding to the distance of 244±10 pc from the Sun, although thelife time of the maser features are only 6 months. The absolute proper motions of the H2O
maser features associated with Orion KL and NGC 1333 are derived, possibly indicating theoutflow motions from the YSOs as well as the systemic motions of the powering sources.
Hirota, T., T. Bushimata, Y. K. Choi, M. Honma, H. Imai, K. Iwadate, T. Jike, O. Kameya, R.
Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, H. Kobayashi, S. Kuji, T. Kurayama, S.
Manabe, T. Miyaji, T. Nagayama, A. Nakagawa, C. S. oh, T. Omodaka, T. Oyama, S. Sakai, T.
Sasao, K. Sato, K. M. Shibata, Y. Tamura, and K. Yamashita [2008c], "Astrometry of H2O
Maserss in Nearby Star-Forming Regions with VERA. II. SVS13 in NGC 1333," Publ. Astron.
Soc. Japan, vol.60, pp.37-44.

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We report on the results of multiepoch very long baseline interferometry (VLBI) observations
with VERA (VLBI Exploration of Radio Astrometry) of the 22 GHz H2O masers associatedwith the young stellar object SVS13 in the NGC1333 region. We carried out phase-referencing
VLBI astrometry, and measured the annual parallax of the maser features in SVS13 of
4.25±0.32mas, corresponding to a distance of 235±18pc from the Sun. Our result is consistent
with a photometric distance of 220pc, previously reported. Even though the maser features
were detectable only for 6 months, the present result provides the distance to NGC1333 withmuch higher accuracy than photometric methods. The absolute positions and proper motions
have been derived, revealing that the H2O masers with LSR (local standard of rest) velocitiesof 7-8kms-1 are most likely associated with VLA4A, which is a radio counterpart of SVS13. It
is currently difficult to attribute the observed proper motions of the maser features to either thejet or the rotating circumstellar disk associated with VLA4A, which should be investigatedthrough future high-resolution astrometric observations of VLA4A and other radio sources in
NGC1333.
Hirota, T., K. Ando, T. Bushimata, Y. K. Choi, M. Honma, H. Imai, K. Iwadate, T. Jike, S.
Kameno, O. Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, M. K. Kim, H.
Kobayashi, S. Kuji, T. Kurayama, S. Manabe, M. Matsui, N. Matsumoto, T. Miyaji, A.
Miyazaki, T. Nagayama, A. Nakagawa, D. Namikawa, D. Nyu, C. S. Oh, T. Omodaka, T.
Oyama, S. Sakai, T. Sasao, K. Sato, M. Sato, K. M. Shibata, Y. Tamura, K. Ueda, and K.
Yamashita [2008d], "Astrometry of H2O Masers in Nearby Star-Forming Regions with VERA
III. IRAS22198+6336 in Lynds 1204G," Publ. Astron. Soc. Japan, vol.60, pp.961-974.
We present results of multi-epoch VLBI observations with VERA (VLBI Exploration of Radio
Astrometry) of the 22 GHz H2O masers associated with a young stellar object (YSO) IRAS
22198+6336 in a dark cloud, L1204G. Based on the phase-referencing VLBI astrometry, wederived an annual parallax of IRAS 22198+6336 to be 1.309±0.047 mas, corresponding to the
distance of 764 ｱ 27 pc from the Sun. Although the most principal error source of ourastrometry is attributed to the internal structure of the maser spots, we successfully reduced theerrors in the derived annual parallax by employing position measurements for all of the 26
detected maser spots. Based on this result, we reanalyzed the spectral energy distribution of
IRAS 22198+6336 and found that the bolometric luminosity and total mass of IRAS
22198+6336 are 450Lsolar and 7Msolar, respectively. These values are consistent with anintermediate-mass YSO deeply embedded in the dense dust core, which has been proposed to
be an intermediate-mass counterpart of a low-mass Class 0 source. In addition, we obtained
absolute proper motions of the H2O masers for the most blue-shifted components. We proposethat the collimated jets aligned along the east-west direction are the most plausible explanation
for the origin of the detected maser features.
Hirota, T., M. Ohishi, and S. Yamamoto, [2009a], "A Search for Carbon-Chain-Rich Cores in
Dark Clouds," Astrophys. J., vol.699, pp.585-602.
We present results of a survey of CCS, HC3N, and HC5N toward 40 dark cloud cores to searchfor "Carbon-Chain-Producing Regions (CCPRs)," where carbon-chain molecules are
extremely abundant relative to NH3, as in L1495B, L1521B, L1521E, and the cyanopolyyne
peak of TMC-1. We have mainly observed toward cores where the NH3 lines are weak, notdetected, or not observed in previous surveys, and the CCS, HC3N, and HC5N lines have been
detected toward 17, 17, and 5 sources, respectively. Among them, we have found a CCPR,
L492, and its possible candidates, L1517D, L530D, L1147, and L1172B. They all show low
abundance ratios of [NH3]/[CCS] (hereafter called the NH3/CCS ratio) indicating the chemical
youth. Combining our results with those of previous surveys, we have found a significant
variation of the NH3/CCS ratio among dark cloud cores and among molecular cloud complexes.
Such a variation is also suggested by the detection rates of carbon-chain molecules. For

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instance, the NH3/CCS ratios are higher and the detection rates of carbon-chain molecules arelower in the Ophiuchus cores than in the Taurus cores. An origin of these systematicabundance variation is discussed in terms of the difference in the evolutionary stage or thecontraction timescale. We have also identified a carbon-chain-rich star-forming core, L483,
where intense HC3N and HC5N lines are detected. This is a possible candidate for a core with
"Warm Carbon-Chain Chemistry."
Hirota, T., T. Bushimata, Y. K. Choi, M. Honma, H. Imai, K. Iwadate, T. Jike, S. Kameno, O.
Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, M. K. Kim, H. Kobayashi, S.
Kuji, T. Kurayama, S. Manabe, K. Maruyama, M. Matsui, N. Matsumoto, T. Miyaji, T.
Nagayama, A. Nakagawa, K. Nakamura, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, T. Sasao,
K. Sato, M. Sato, K. M. Shibata, M. Shintani, Y. Tamura, M. Tsushima, and K. Yamashita[2009b], "Astrometry of H2O Maser Sources in Nearby Molecular Clouds with VERA," Proc.
of the "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser.
vol.402, pp.456-459.
We report on the recent results of astrometic observations of H2O maser sources associatedwith the nearby molecular clouds with VERA. We carried out phase-referencing VLBI
astrometry of H2O masers in a high-mass star-forming region Orion KL and successfully
detected an annual parallax of Orion KL to be 2.29±0.10 mas, corresponding to the distance of
437±19 pc from the Sun. In addition, we obtained an annual parallax of a nearby low-massstar-forming region NGC 1333 to be 4.25±0.32 mas, corresponding to the distance of 235±18
pc from the Sun. Our results demonstrate the high capability of astrometry with VERA, which
can provide the most accurate distances to nearby molecular clouds.
Hirota, T., N. Sakai, and S. Yamamoto [2010], "Depletion of CCS in a Candidate
Warm-Carbon-Chain-Chemistry Source L483," Astrophys. J., vol.720, pp.1370-1373.
We have carried out an observation of the CCS (JN = 21-10) line with the Very Large Array in
its D-configuration toward a protostellar core L483 (IRAS 18140-0440). This is a candidate
source
of
the
newly
found
carbon-chain-richenvironment
called"Warm-Carbon-Chain-Chemistry (WCCC)," according to the previous observations ofcarbon-chain molecules. The CCS distribution in L483 is found to consist of two clumps
aligned in the northwest-southeast direction, well tracing the CCS ridge observed with thesingle-dish radio telescope. The most remarkable feature is that CCS is depleted at the corecenter. Such a CCS distribution with the central hole is consistent with those of previously
observed prestellar and protostellar cores, but it is rather unexpected for L483. This is because
the distribution of CS, which is usually similar to that of CCS, is centrally peaked. Our results
imply that the CCS (JN = 21-10) line would selectively trace the outer cold envelope in thechemically less evolved phase that is seriously resolved out with the interferometricobservation. Thus, it is most likely that the high abundance of CCS in L483 relative to theother WCCC sources is not due to the activity of the protostar, although it would be related toits younger chemical evolutionary stage, or a short timescale of the prestellar phase.
Hodokuma, T., K. Kuriki, N. Asada, H. Demura, J. Terazono, H. Hirata, J. Haruyama, M.
Ohtake, T. Matsunaga, and H. Araki [2009], "Integration of Multi-Instrumental Data Sets of
Kaguya, LISM and LALT," 40th Lunar and Planetary Science Conference, (Lunar andPlanetary Science XL), held March 23-27, 2009 in The Woodlands, Texas, id.1637.
We report current status on integration of multi-instrumental data sets of Kaguya, LISM and
LALT, such as digital terrain model, altitude profiles, multiband images, and spectral data.
Honma, M., T. Bushimata, Y. K. Choi, T. Hirota, H. Imai, K. Iwadate, T. Jike, O. Kameya, R.
Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, H. Kobayashi, S. Kuji, T. Kurayama, S.
Manabe, T. Miyaji, T. Nagayama, A. Nakagawa, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, K.

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Sato, T. Sasao, K. M. Shibata, M. Shintani, H. Suda, Y. Tamura, M. Tsushima, and K.
Yamashita [2008a], "VERA Project," Proc. of the "Mapping the Galaxy and Nearby Galaxies",
eds. Wada, K., and Combes, F., pp.27-32.
Is this paper we review the current status VERA (VLBI Exploration of Radio Astrometry)project. First, we present an overview of VERA, and then we report on recent results from
VERA, particularly the parallax measurement of Galactic star forming region S269 at the
distance of 5.3 kpc.
Honma, M., T. Bushimata, Y. K. Choi, T. Hirota, H. Imai, K. Iwadate, T. Jike, O. Kameya, R.
Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, S. Manabe, T. Miyaji, T. Nagayama, A.
Nakagawa, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, K. Sato, T. Sasao, K. M. Shibata, M.
Shintani, H. Suda, Y. Tamura, M. Tsushima, and K. Yamashita [2008b], "Galactic Rotation
Measurements Based on H2O Maser Astrometry with VERA," Proc. of the IAU Symp. 242,
"Astrophysical Masers and their Environments", eds. Jessica Chapman and Willem Baan,
pp.361-365.
We present results of astrometric observations of S269 H2O maser performed with VERA(VLBI Exploration of Radio Astrometry). We have monitored the positions of S269 H2Omasers for 1 year and successfully detected its parallax to be 189 ｱ 8 micro-arcsecond. This
corresponds to a source distance of 5.28-0.22+0.24 kpc, and is the smallest parallax (and thus thelargest distance) that has ever been measured by means of annual parallax. Proper motions of
S269 H2O maser were also measured and used to determine the Galactic rotation velocity at
the position of S269. Our measurements show that the Galactic rotation velocity at S269 is thesame to that at the Sun within 3%, indicating that the Galactic rotation curve is flat out to R~13
kpc.
Honma, M., T. Bushimata, Y. K. Choi, T. Hirota, H. Imai, K. Iwadate, T. Jike, S. Kameno, O.
Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima, M. K. Kim, H. Kobayashi, S.
Kuji, T. Kurayama, S. Manabe, N. Matsumoto, T. Miyaji, T. Nagayama, A. Nakagawa, K.
Nakamura, C.-S. Oh, T. Omodaka, S. Sakai,K. Sato, M. Sato, T. Sasao, K. M. Shibata, Y.
Tamura, and K. Yamashita [2008c], "Astrometry of Galactic Star-Forming Regions with
VERA," Proc. of the IAU Symp. 248, "A Giant Step: from Milli- to Micro-arcsecond
Astrometry", eds. Wenjing Jin, Imants Platais, Michael A. C. Perryman, pp.198-199.
We present an overview of recent astrometric results with VERA. Since 2004, we have been
conducting astrometry of tens of Galactic maser sources with VERA, and recently obtained
trigonometric parallaxes for several sources, with distances ranging from 180 pc to 5.3 kpc. In
this paper, we briefly summarize the results for Galactic star-forming regions, including S269,
Orion-KL, NGC 1333, ρ-oph, NGC 281 and others.
Honma, M., K. Kijima, H. Suda, N. Kawaguchi, H. Kobayashi, T. Bushimata, R. Shimizu, A.
Yoshimura, T. Sasao, T. Hirota, H. Imai, K. Iwadate, T. Jike, O. Kameya, R. Kamohara, S. Kuji,
T. Kurayama, S. Manabe, T. Miyaji, A. Nakagawa, T. Omodaka, T. Oyama, S. Sakai, K. Sato,K. M. Shibata, and Y. Tamura [2008d], "Dual-Beam Delay Calibration for VERA," Publ.
Astron. Soc. Japan, vol.60, pp.935-950.
We present the technique of instrumental delay calibration for the dual-beam system of VLBI
Exploration of Radio Astrometry (VERA), namely, the horn-dish method, in which artificial
noise sources are mounted on the antenna feedome base and a wide-band radio noise isinjected into the dual-beam receivers after reflection by a subreflector. We introduce the basic
concept of calibration with the horn-on-dish method, and also present results of theexperiments to evaluate its calibration accuracy. Detailed comparisons between model pathcalculations and measured paths from the noise sources show that the horn-on-dish method cancalibrate the dual-beam delay difference in the antenna structure and receiver within an ~0.1mm level. We estimated that the systematic error in the calibration does not exceed

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0.127mm, which was evaluated at an elevation angle of 15°. This error corresponds to an
astrometric error of ~11μas with VERA's maximum baseline. An experimental confirmation of
the systematic error in the horn-on-dish method has also been obtained by sing a pair of 10m
and VERA's 20m antennas at the Mizusawa station, demonstrating that the systematicdifference between the dual-beam delay difference measured with noise sources and that forcelestial objects was 0.118mm, being consistent with the above estimate.
Honma, M., Y. Tamura, and M. J. Reid [2008e], "Tropospheric Delay Calibrations for VERA,"
Publ. Astron. Soc. Japan, vol.60, pp.951-960.
We present techniques for the tropospheric delay calibration, which is the key to increasing theaccuracy of the phase-referencing astrometry with Very Long Baseline Interferometry (VLBI).
We study three methods, and make a comparison of these methods to discuss the accuracy incalibration. Our results show that all three methods can calibrate the tropospheric zenith delay
within accuracy of ~ 2 cm. We also present simulations of positional errors in VLBI
Exploration of Radio Astronomy (VERA) at the presence of an error in the tropospheric zenith
delay, showing that parallax measurements with accuracy of 10μas can be readily achieved forsources at high declination and with small separation angles between the target Galactic maser
and extragalactic position references.
Honma, M. [2008f], "Galaxy-Scale Astrometry and Galactic Rotation Measurement with
VERA," Proc. of the 9th European VLBI Network Symposium on The role of VLBI in theGolden Age for Radio Astronomy and EVN Users Meeting, September 23-16, 2008, Bologna,
Italy, pp.77-79.
We present results of Galaxy-scale astrometry with VERA (VLBI Exploration of Radio
Astrometry). VERA had been conducting regular monitoring of Galactic radio sources since2004, and we have already detected parallaxes for several sources, ranging from a few 100 pc
to 5 kpc. In this paper, we summarize the recent results of astrometric measurements anddiscuss the Galaxy rotation obtained with VERA.
Honma, M. [2009a], "AGB Star Observations with VERA," Proc. of the "AGB Stars andRelated Phenomena", eds. Toshiya Ueta, Noriyuki Matsunaga, and Yoshifusa Ita, p.54.
Not Available
Honma, M., T. Bushimata, Y. K. Choi, T. Hirota, H. Imai, K. Iwadate, T. Jike, S. Kameno, O.
Kameya, R. Kamohara, N. Kawaguchi, M. Kijima, K. M. Kim, H. Kobayashi, S. Kuji, T.
Kurayama, S. Manabe, M. Matsui, N. Matsumoto, T. Miyaji, T. Nagayama, A. Nakagawa, K.
Nakamura, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, K. Sato, M. Sato, T. Sasao, K. M.
Shibata, Y. Tamura, and K. Yamashita [2009b], "Maser Astrometry with VERA and VSOP-2,"
Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser.
vol.402, pp.460-464.
We present recent results of maser astrometry obtained with VERA (VLBI Exploration ofRadio Astrometry), which is a Japanese VLBI array dedicated to phase-referencing astrometry
to explore the 3-D structure of the Milky Way Galaxy. Since 2004 we have been conducting
regular monitoring of maser sources with VERA, and we have already detected parallaxes forseveral sources, ranging from a few 100 pc to 5 kpc. These results include mea- surements for
Galactic star-forming regions such as ORI-KL, S269, NGC 281 as well as those for late typestars such as VY CMa. We also discuss the VERA-VSOP-2 connection in the near future, andpropose astrometric observations with VSOP-2.
Hsieh, P.-Y., S. Matsushita, J. Lim, K. Kohno, and S. Sawada-Satoh [2008], "Interferometric
12
CO J = 1-2 Image of the Nuclear Region of Seyfert 1 Galaxy NGC 1097," Astrophys. J.,
vol.683, pp.70-77.
We have mapped the central region of the Seyfert 1 galaxy NGC 1097 in 12CO J=2-1 with the

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Submillieter Array (SMA). The 12CO J-2-1 map shows a central concentration and asurrounding ring coinciding, respectively, with the Seyfert nucleus and a starburst ring. Theline intensity peaks at the nucleus, whereas in a previously published 12CO J=1-0 map theintensity peaks at the starburst ring. The azimuthally averaged 12CO J-1-0 intensity ratio R21of the ring is about unity, which is similar to those in nearby active star-forming galaxies,
suggesting that most of the molecular gas in the ring is involved in fueling the starburst. The
ratio of molecular gas to dynamical mass in the starburst ring shows a somewhat lower value
than that found in nearby star-forming galaxies, suggesting that the high R21 of unity may becaused by additional effects, such as shocks induced by gas infall along the bar. The molecular
gas can last for about 1.2x108 yr without further replenishment, assuming a constant starformation rate. The central gas is rotating with the molecular ring in the same direction, while
its velocity gradient is steeper than that of the ring, and similar to what usually observed in
Seyfert 2 galaxies. To view the Seyfert nucleus without obscuration, the central gas can be a
low-inclined disk or torus but not too low to be less massive than the mass of the host galaxy,or be a highly inclined thin disk or clumpy and thick torus, inner part of the galactic disk isalso possible. The R21 of ~1.9 of the central gas is significantly higher than that of the ring,indicates that the activity of the Seyfert nucleus may significant influence the central gas.
Hughes, A., T. Wong, J. Ott, E. Muller, J. L. Pineda, Y. Mizuno, J.-P. Bernard, D. Paradis, S.
Maddison, W. T. Reach, L. Staveley-Smith, A. Kawamura, M. Meixner, T. Kim, T. Onishi, N.
Mizuno, and Y. Fukui [2010a], "Physical Properties of Giant Molecular Clouds in the Large
Magellanic Cloud," Mon. Not. Roy. Astron. Soc., vol.406, pp.2065-2086.
The Magellanic Mopra Assessment (MAGMA) is a high angular resolution 12CO (J = 1 -> 0)
mapping survey of giant molecular clouds (GMCs) in the Large Magellanic Cloud (LMC) andSmall Magellanic Cloud using the Mopra Telescope. Here we report on the basic physicalproperties of 125 GMCs in the LMC that have been surveyed to date. The observed clouds
exhibit scaling relations that are similar to those determined for Galactic GMCs, although
LMC clouds have narrower linewidths and lower CO luminosities than Galactic clouds of asimilar size. The average mass surface density of the LMC clouds is 50 Msolarpc-2,
approximately half that of GMCs in the inner Milky Way. We compare the properties of GMCs
with and without signs of massive star formation, finding that non-star-forming GMCs havelower peak CO brightness than star-forming GMCs. We compare the properties of GMCs withestimates for local interstellar conditions: specifically, we investigate the HI column density,
radiation field, stellar mass surface density and the external pressure. Very few cloudproperties demonstrate a clear dependence on the environment; the exceptions are significant
positive correlations between (i) the HI column density and the GMC velocity dispersion, (ii)the stellar mass surface density and the average peak CO brightness and (iii) the stellar mass
surface density and the CO surface brightness. The molecular mass surface density of GMCs
without signs of massive star formation shows no dependence on the local radiation field,
which is inconsistent with the photoionization-regulated star formation theory proposed by
McKee. We find some evidence that the mass surface density of the MAGMA clouds increases
with the interstellar pressure, as proposed by Elmegreen, but the detailed predictions of thismodel are not fulfilled once estimates for the local radiation field, metallicity and GMC
envelope mass are taken into account.
Hughes, A. M., S. M. Andrews, D. J. Wilner, M. R. Meyer, J. M. Carpenter, C. Qi, A. S. Hales,
S. Casassus, M. R. Hogerheijde, E. E. Mamajek, S. Wolf, T. Henning, and M. D. Silverstone[2010b], "Structure and Composition of Two Transitional Circumstellar Disks in Corona,"
Astron. J., vol.140, pp.887-896.
The late stages of evolution of the primordial circumstellar disks surrounding young stars arepoorly understood, yet vital to constraining theories of planet formation. We consider basic

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structural models for the disks around two ~10 Myr old members of the nearby RCrA
association: RX J1842.9-3532 and RX J1852.3-3700. We present new arcsecond-resolution
maps of their 230 GHz continuum emission from the Submillimeter Array and unresolvedCO(3-2) spectra from the Atacama Submillimeter Telescope Experiment. By combining thesedata with broadband fluxes from the literature and infrared fluxes and spectra from the catalogof the Formation and Evolution of Planetary Systems Legacy program on the Spitzer Space
Telescope, we assemble a multiwavelength data set probing the gas and dust disks. Using theMonte Carlo radiative transfer code RADMC to model simultaneously the spectral energy
distribution and millimeter continuum visibilities, we derive basic dust disk properties andidentify an inner cavity of radius 16 AU in the disk around RX J1852.3-3700. We also identify
an optically thin 5 AU cavity in the disk around RX J1842.9-3532, with a small amount of
optically thick material close to the star. The molecular line observations suggest anintermediate disk inclination in RX J1842.9-3532, consistent with the continuum emission. In
combination with the dust models, the molecular data allow us to derive a lower CO content
than expected, suggesting that the process of gas clearing is likely underway in both systems,
perhaps simultaneously with planet formation.
Iguchi, S., and T. Okuda [2008], "The FFX Correlator," Publ. Astron. Soc. Japan, vol.60,
pp.857-869.
We established a new algorithm for a correlation process in radio astronomy. This scheme
consists of a 1st-stage Fourier transform as a filter and a 2nd-stage Fourier transform forspectroscopy. The "FFX" correlator stands for Filter and FX architecture, since the 1st-stage
Fourier transform is performed as a digital filter, and the 2nd-stage Fourier transform isperformed as a conventional FX scheme. We developed FFX correlator hardware not only forverifying the FFX scheme algorithm, but also for applying to the Atacama Submillimeter
Telescope Experiment (ASTE) telescope toward high-dispersion and wideband radio
observations at submillimeter wavelengths. In this paper, we present of the FFX correlator andits properties, as well as evaluation results with the production version.
Iguchi, S., K.-I. Morita, M. Sugimoto, B. Vila-Vilaro, M. Saito, T. Hasegawa, R. Kawabe, K.
Tatematsu, S. Sakamoto, H. Kiuchi, S. K. Okumura, G. Kosugi, J. Inatani, S. Takakuwa, D.
Iono, T. Kamazaki, R. Ogasawara, and M. Ishiguro [2009], "The Atacama Compact Array(ACA)," Publ. Astron. Soc. Japan, vol.61, pp.1-12.
For realizing high ﬁdelity of imaging with mosaicing observations, the Atacama Large
Millimeter/submillimeter Array (ALMA) consists of a homogeneous array of 12 m antennas(12 m Array) and the Atacama Compact Array (ACA) in order to cover all spatial frequency
Fourier components of the brightness distribution of observed sources. The array is located at
an altitude site of about 5000 m with an operating wavelength range of 0.3 to 3 mm. ACA is anarray composed of four 12 m dishes [TP (Total Power) Array] and twelve 7 m dishes (7 m
Array). The 7 m Array has a very compact con ﾞ guration to take short-baseline data
corresponding to the low spatial frequency Fourier components. The 7 m Array has two con ﾞ
gurations extended over 30-50 m to avoid shadowing at low elevation. The scientiﬁcimportances and operation concepts of ACA, and the system design of ACA and its
performance are presented in this paper.
Ikeda, N., Y. Kitamura, and K. Sunada [2009a], "A Survey of Dense Cores in the Orion B
Cloud," Astrophys. J., vol.691, pp.1560-1582.
We have carried out an H13CO+(J = 1-0) core survey in a large area of 1 deg2, covering most of
the dense region in the Orion B molecular cloud, using the Nobeyama 45 m radio telescopewith the 25-BEam Array Receiver System. We cataloged 151 dense cores using the clumpfind
method. The cores have mean radius, velocity width, and mass of 0.10±0.02 pc, 0.53±0.15 km
s-1, and 8.1± 6.4 M⦿, respectively, which are very similar to those in the Orion A cloud. We

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examined the spatial relation between our H13CO+ cores and the 850 μm cores observed by
Johnstone and colleagues in 2001 and 2006, and found that there are two types of spatial
relationships: H13CO+ cores with and without the 850μm cores. Since the mean density of the
850μm cores is higher than that of the H13CO+ cores, we can interpret the H13CO+ cores with
850μm cores as being more centrally concentrated and hence more evolved, compared withthose without. Considering the relationship between the masses of the H13CO+ and 850μm
cores, we estimate the 850μm core mass function (CMF) using the H13CO+ CMF through thegeneralization of the confusion model proposed by Ikeda and colleagues in 2007. Our
predicted 850μm CMF is found to be quite consistent with that directly derived by Johnstone
and colleagues. Furthermore, we predict the initial mass function (IMF) by the generalized
confusion model assuming a star formation efficiency of 40% for the H13CO+ cores, and foundthat our predicted IMF is consistent with the Galactic field-averaged IMF within uncertainties.
This agreement may indicate that the origin of the IMF goes back to the cloud structures withdensities of less than 104 cm-3.
Ikeda, N., and Y. Kitamura [2009b], "A C18O Study of the Origin of the Power-Law Nature in
the Initial Mass Function," Astrophys. J. (Letters), vol.705, pp.L95-L98.
We have performed C18O (J = 1-0) mapping observations of a 20' x 20' area of the OMC-1
region in the Orion A cloud. We identified 65 C18O cores, which have a mean radius, a velocity
width in FWHM, and an LTE mass of 0.18 ± 0.03 pc, 0.40 ± 0.15 km s-1, and 7.2 ± 4.5 Msun,
respectively. All the cores are most likely to be gravitationally bound by considering theuncertainty in the C18O abundance. We derived a C18O core mass function, which shows apower-law-like behavior above 5 Mun. The best-fit power-law index of -2.3 ± 0.3 is consistent
with those of the dense core mass functions and the stellar initial mass function (IMF)
previously derived in the OMC-1 region. This agreement strongly suggests that the power-law
form of the IMF has been already determined at the density of ~103 cm-3, traced by the C18O (J= 1-0) line. Consequently, we propose that the origin of the IMF should be searched in tenuous
cloud structures with densities of less than 103 cm-3.
Imada, S., H. Hara, T. Watanabe, A. Asai, T. Minoshima, L. K. Harra, and J. T. Mariska [2008],"Non-Gaussian Line Profiles in a Large Solar Flare Observed on 2006 December 13,"
Astrophys. J. (Letters), vol.679, pp.L155-L159.
We have studied the characteristics of the non-Gaussian line profile of the Fe xiv 274.20 Å line
in and around a flare arcade. We found that broad non-Gaussian line profiles associated with
redshifts are observed in the flare arcade. There were two typical types of broad line profiles.
One was a distorted line profile caused by multiple flows, and the other was a symmetric line
profile without any additional component. We successfully distinguished those two types using
higher order statistical moments or M-the additional component contribution-defined in thisLetter. The distorted/symmetric broad line profiles were preferentially observed in new/old
flare loops, respectively.
Imai, H., K. Nakashima, T. Bushimata, Y. K. Choi, T. Hirota, M. Honma, K. Horiai, N.
Inomata, K. Iwadate, T. Jike, O. Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. Kijima,
H. Kobayashi, S. Kuji, T. Kurayama, S. Manabe, T. Miyaji, T. Nagayama, A. Nakagawa, C. S.
Oh, T. Omodaka, T. Oyama, S. Sakai, S. Sakakibara, K. Sato, T. Sasao, K. M. Shibata, R.
Shimizu, M. Shintani, Y. Sofue, K. Sora, H. Sudo, Y. Tamura, M. Tsushima, Y. Ueno, and K.
Yamashita [2007], "Astrometry of H2O Masers in Nearby Star-Forming Regions with VERA I.
IRAS 16239-2422 in ρOph East," Publ. Astron. Soc. Japan, vol.59, pp.1107-1113.
We report on results of multi-epoch VLBI observations of H2O masers associated with alow-mass young stellar object, IRAS 16239-2422 in ρOph East, and a fringe-phase andposition reference sources, ICRF J162546.8-252738, using the VLBI Exploration of Radio
Astrometry (VERA) for high-precision astrometry. We obtained an annual parallax of a maser

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feature to be π=5.6+1.5-0.5 mas, corresponding to a distance of D=178+18-37 pc. We also found 10
relative proper motions of maser feature with respect to the maser feature mentioned above.
The motion of the accompanying young stellar object (YSO) has already been found inthermal continuum emission previously observed with the Very Long Array. The intrinsic
motions of masers have been estimated from the relative proper motions after the YSO's
motion is subtracted from, and a systemic secular motion of the position reference feature isadded to the proper motions originally measured. The intrinsic maser kinematical structure
may trace a bipolar outflow.
Imai, H., T. Fujii, T. Omodaka, and S. Deguchi [2008a], "JVN Observations of H20 Masers
around the Evolved Star IRAS 22480+6002," Publ. Astron. Soc. Japan, vol.60, pp.55-62.
We report on the H2O maser distributions around IRAS 22480+6002 (=IRC+60370) observedwith the Japanese VLBI Network (JVN) at three epochs spanning 2 months. This object was
identified as a K-type supergiant in 1970s, which was unusual as a stellar maser source. The
spectrum of H2O masers consists of 5 peaks separated roughly equally by a few km/s each.
The H2O masers were spatially resolved into more than 15 features, which spread about 50
mas along the east-west direction. However, no correlation was found between the propermotion vectors and their spatial distributions; the velocity field of the envelope seems random.
A statistical parallax method applied to the observed proper-motion data set gives a distance of
1.0±0.4 kpc for this object, that is considerably smaller than previously thought. The distanceindicates that this is an evolved star with L~5800 Lsun. This star shows radio, infrared, andoptical characteristics quite similar to those of the population II post-AGB stars such as RV
Tau variables.
Imai, H., T. Omodaka, T. Hirota, T. Umemoto, K. Sorai, T. Kondo, and the VERA
collaboration [2008b], "A Collimated Jet and an Infalling-Rotating Disk in G192.16-3.84
Traced by H2O Maser Emission," Proc. of the IAU Symp. 242, "Astrophysical Masers andtheir Environments", eds. Jessica Chapman and Willem Baan, pp.340-341.
We present H2O masers associated with the massive-star forming region G192 observed with
the Japan VLBI network since the year 2005, The spatio-kinematical structure of the maser
feature clusters has well persisted since previous observations, in which the masers areassociated with two young stellar objects (YSOs) separated by ~1200 AU and expected to be
associated with a highly-collimated bipolar jet and an infalling-rotating disk in the northernand southern YSOs, respectively. We estimated a jet speed of ~100 km s-1 and re-estimated a
dynamical age of the whole jet to be 5.6x104 years. The spatial distribution of maser Doppler
velocities found during the previous and present observations, relative proper motions of H2O
maser features in the southern cluster found in the present observations, a relative bulk motion
between the two maser clusters are well explained by a model of an infalling-rotating disk witha radius of ~1000 AU and a central stellar mass of ~8 Msolar.
Imai, H., J.-H. He, J. Nakashima, N. Ukita, S. Deguchi, and N. Koning [2009], "CO J=3-2
Emission from the "Water Fountain" Sources IRAS 16342-3814 and IRAS 18286-0959," Publ.
Astron. Soc. Japan, vol.61, pp.1365-1372.
We observed CO J=3-2 emission from "water-fountain'' sources, which exhibit high-velocity
collimated stellar jets traced by H2O maser emission, with the Atacama Submillimeter
Telescope Experiment (ASTE) 10 m telescope. We detected CO emission from two sources:
IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits aspectrum that could be well fit to a Gaussian profile, rather than to a parabolic profile, with avelocity width (FWHM) of 158 ｱ 6 km s-1 and an intensity peak at VLSR=50±2 km s-1. The
mass-loss rate of the star is estimated to be ~2.9×10-5 M⦿yr-1. Our morpho-kinematic models
suggest that the CO emission is optically thin, and associated with a bipolar outflow rather
than with a (cold and relatively small) torus. The IRAS 18286-0959 CO emission has a

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velocity width (FWHM) of 3.0±0.2 km s-1, smaller than typically seen in AGB envelopes. The
narrow velocity width of the CO emission suggests that it originates from either an interstellar
molecular cloud or a slowly-rotating circumstellar envelope that harbors the H2O maser
source.
Imai, H., J. Nakashima, S. Deguchi, A. Yamauchi, A. Nakagawa, and T. Nagayama, [2010],"Japanese VLBI Network Mapping of SiO ν=3 J=1-0 Maser Emission in W Hydrae," Publ.
Astron. Soc. Japan, vol.62, pp.431-439.
We report first on two-epoch mapping observations of SiO v = 3 J = 1-0 maser emission in thesemiregular variable W Hydrae using the Japanese VLBI Network. The flux density of the v =3 J = 1-0 emission detected on 2009 February 28 was two orders of magnitude smaller thanthose of the v = 1 and v = 2 emissions, while a month and half later the v = 3 flux density
suddenly increased by a factor of ˜25. In contrast, the v = 1 and v = 2 flux densities decreased
during this period, as expected from the optical light curve. At the first epoch, the v = 3 maser
features were located inside of a ring composed of the v = 1 and v = 2 features by 6 mas(gtrsim0.5 AU) toward the central star. These offsets are meaningfully larger than the error of
the fitted ring radius and the difference in the ring sizes of v = 1 and v = 2 masers (lesssim 0.2
AU). The present result at the first epoch suggests that v = 3 J = 1-0 SiO masers are
predominantly excited in a pumping mechanism (e.g., collisional pumping) different from thatrecently proposed on the basis of the line overlap with infrared H2O lines. Interestingly, thesecond-epoch observation revealed that the v = 3 features were located on almost the same ringas the v = 2 ring, which is consistent with what line-overlap theory suggests.
Imamura, T., T. Iwata, Z. Yamamoto, K.-L. Oyama, A. Nabatov, Y. Kono, M. Matsumoto, Q.
Liu, H. Noda, H. Hanada, Y. Futaana, and A. Saito [2008a], "Initial Results of the Lunar
Ionosphere Observation with SELENE Radio Science," 39th Lunar and Planetary Science
Conference, (Lunar and Planetary Science XXXIX), held March 10-14, 2008 in League City,
Texas. LPI Contribution No. 1391, p.1659.
The electron density distribution near the lunar surface in various conditions are being
observed by radio occultation technique in the Kaguya (SELENE) mission using the Vstar
sub-satellite. Initial results from this experiment are presented.
Imamura, T., K.-I. Oyama, T. Iwata,Y. Kono, K. Matsumoto, Q. Liu, H. Noda, Y. Futaana, and
A. Nabatov [2008b], "The Possibility of Studying the Lunar Ionosphere with the SELENE
Radio Science Experiment," Earth Planets and Space, vol.60, pp.387-390.
The electron density profiles above the lunar surface will be observed by the radio occultation
technique during the SELENE mission using the Vstar sub-satellite. Previous radio occultation
observations have indicated the existence of an ionosphere with densities of up to 1000 cm-3
above the dayside lunar surface. The measured densities are difficult to explain theoreticallywhen the removal of plasma by the solar wind is considered, and thus the generation
mechanism of the lunar ionosphere is a major issue, with even the validity of previous
observations still under debate. The SELENE radio science experiment will establish themorphology of the lunar ionosphere and will reveal its relationship with various physicalconditions to provide possible clues to the mechanism.
Imamura, T., T. Iwata, Z. Yamamoto, N. Mochizuki, Y. Kono, K. Matsumoto, Q. Liu, H. Noda,
H. Hanada, K. Oyama, A. Nabatov, Y. Futaana, A. Saito, and H. Ando [2008c], "Studying the
Lunar Ionosphere with SELENE Radio Science Experiment," American Geophysical Union,
Fall Meeting 2008, abstract #P51D-04.
Lunar ionosphere is generally thought to be as thin as 1 cm-3; the process that will prevent theaccumulation of newly produced ions near the lunar surface is the impingement of the solar
wind magnetic field on the lunar surface, which induces an electric field that sweeps away ions.
In harmony with this prediction, most of the radio occultation experiments performed with

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radio stars failed to detect the lunar ionosphere. Radio occultation experiments conducted with
the Soviet Luna 19 and 22 spacecraft, on the other hand, detected large electron densities near
the dayside lunar surface. Vyshlov (1974) obtained peak electron densities of 500-1000 cm-3 atheights of 5-10 km, with a gradual decrease at higher altitudes with a scale height of 10-30 km.
The measured densities are difficult to explain theoretically, and thus the generation
mechanism of the lunar ionosphere is a major issue, with even the validity of the previous
observations still under debate. If a thick lunar ionosphere exists, possible mechanisms tomaintain the ionized layer are the effect of the remnant magnetic field which stands off thesolar wind magnetic field, certain processes that enhance the neutral gas concentration, or
charged dust grains that are lifted up by the near-surface electric field. The electron density
profiles above the lunar surface are being observed by radio occultation during the SELENE(KAGUYA) mission using sub-satellites. The systematic measurements will establish themorphology of the lunar ionosphere and reveal its dependence on various conditions, thereby
providing clues to the generation mechanism. The S-band (2.2GHz) and X-band (8.5GHz)
signals transmitted by the Vstar sub- satellite is received at the Usuda Deep Space Center inJapan. The most serious error source is the temporal variation in the terrestrial ionosphere
during measurements. In the region where the contribution of the lunar ionosphere is virtuallyabsent, i.e. at altitudes above ~100 km, a gradual variation caused by the terrestrial ionosphereis observed. This variation is extrapolated into the near-moon portion and subtracted from theobserved one, thereby eliminating the influence of the terrestrial ionosphere to some extent. In
addition to this method, we also use the Rstar sub- satellite, which transmits coherent two
signals in S-band, to measure the terrestrial ionosphere during the lunar occultation of Vstar;
the subtraction of the Rstar's measurement from the Vstar's measurement gives the lunar
ionosphere. The opportunities of the latter method are rather limited, however. More than 100
measurements using Vstar and more than 10 measurements using Rstar and Vstar have been
conducted during the first half of the mission. Although the error due to the fluctuation of theterrestrial ionosphere is rather significant, there seems to be a tendency that the electron
density increases on the morning side of the moon.
Imanishi, M., K. Nakanishi, Y. Tamura, N. Oi, and K. Kohno [2007], "Millimeter
Interferometric HCN(1-0) and HCO+(1-0) Observations of Luminous Infrared Galaxies,"
Astron. J., vol.134, pp.2366-2384.
We present the results on millimeter interferometric observations of four luminous infrared
galaxies (LIRGs), Arp 220, Mrk 231, IRAS 08572+3915, and VV 114, and one Wolf-Rayetgalaxy, He 2-10, using the Nobeyama Millimeter Array (NMA). Both the HCN(1-0) andHCO+(1-0) molecular lines were observed simultaneously, and their brightness-temperature
ratios were derived. High-quality infrared L-band (2.8-4.1μm) spectra were also obtained forthe four LIRGs to better constrain their energy sources deeply buried in dust and molecular gas.
When combined with other LIRGs we have previously observed with NMA, the final sample
comprised nine LIRGs (12 LIRG nuclei) with available interferometric HCN(1-0) andHCO+(1-0) data, sufficient to investigate the overall trend in comparison with known AGNs
and starburst galaxies. We found that LIRGs with luminous buried AGN signatures at otherwavelengths tend to show high HCN(1-0)/HCO+(1-0) brightness-temperature ratios as seen in
AGN-dominated galaxies, while the Wolf-Rayet galaxy He 2-10 displays a small ratio. An
enhanced HCN abundance in the interstellar gas surrounding a strongly X-ray-emitting AGN,
as predicted by some chemical calculations, and/or infrared radiative pumping, are possible
explanations of our results.
Imanishi, M. [2008], "Nobeyama Millimeter Array Observations of Luminous Infrared
Galaxis," EAS Publication Series, vol.31, pp.93-96.
We present the results of systematic millimeter interferometric observations of luminous

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infrared galaxies (LIRGs), using the Nobeyama Millimeter Array. We observed HCN (J = 1-0)
and HCO+ (J = 1-0) emission lines simultaneously, and derived their brightness-temperature
ratios, to investigate whether the observed ratios are similar to those found in AGN-dominatednuclei or starburst galaxies. LIRGs with (without) luminous buried AGN signatures in our
infrared spectra tend to show high (low) HCN (J = 1-0) to HCO+ (J = 1-0)
brightness-temperature ratios as seen in galaxy nuclei dominated by AGNs (starbursts). The
high ratios in buried AGN candidates could be explained by the enhanced HCN abundance,
and/or infrared radiative pumping of the HCN molecule, in the close vicinity of an AGN.
Imanishi, M., K. Nakanishi, Y. Tamura, and C.-H. Peng [2009], "Nobeyama Millimeter
Interferometric HCN(1-0) and HCO+(1-0) Observations of Further Luminous Infrared
Galaxies," Astron. J., vol.137, pp.3581-3598.
We report the results of interferometric HCN(1-0) and HCO+(1-0) observations of four
luminous infrared galaxies (LIRGs), NGC 2623, Mrk 266, Arp 193, and NGC 1377, as a final
sample of our systematic survey using the Nobeyama Millimeter Array. Our survey contains
the most systematic interferometric, spatially resolved, simultaneous HCN(1-0) andHCO+(1-0) observations of LIRGs. Ground-based infrared spectra of these LIRGs are alsopresented to elucidate the nature of the energy sources at the nuclei. We derive theHCN(1-0)/HCO+(1-0) brightness-temperature ratios of these LIRGs and confirm thepreviously discovered trend that LIRG nuclei with luminous buried active galactic nucleus(AGN) signatures in infrared spectra tend to show high HCN(1-0)/HCO+(1-0)
brightness-temperature ratios, as seen in AGNs, while starburst-classified LIRG nuclei ininfrared spectra display small ratios, as observed in starburst-dominated galaxies. Our new
results further support the argument that the HCN(1-0)/HCO+(1-0) brightness-temperature
ratio can be used to observationally separate AGN-important and starburst-dominant galaxy
nuclei.
Imanishi, M., K. Nakanishi, M. Yamada, Y. Tamura, and K. Kohno [2010], "ASTE
Simultaneous HCN(4-3) and HCO+(4-3) Observations of the Two Luminous Infrared Galaxies
NGC 4418 and Arp 220," Publ. Astron. Soc. Japan, vol.62, pp.201-209.
We report the results of HCN (J = 4-3) and HCO+ (J = 4-3) observations of two luminous
infrared galaxies, NGC 4418 and Arp 220, made using the Atacama Submillimeter Telescope
Experiment (ASTE). The ASTE wide-band correlator provided simultaneous observations of
HCN (4-3) and HCO+(4-3) lines, and a precise determination of their fiux ratios. Both galaxies
showed high HCN (4-3) to HCO+ (4-3) fiux ratios of > 2, possibly due to AGN-related
phenomena. The J = 4-3 to J = 1-0 transition fiux ratios for HCN (HCO+) are similar to those
expected for fully thermalized (sub-thermally excited) gas in both sources, in spite of HCN’s
higher critical density. If we assume collisional excitation and neglect an infrared radiative
pumping process, our non-LTE analysis suggests that HCN traces gas with signiﬁcantly cantly
higher density than HCO+. In Arp 220, we separated the double-peaked HCN (4-3) emission
into eastern and western nuclei, based on velocity information. We conﬁrmed that the eastern
nucleus showed a higher HCN (4-3) to HCN (1-0) fiux ratio, and thus contained a larger
amount of highly excited molecular gas than the western nucleus.
Inoue, H., K. Muraoka, T. Sakai, A. Endo, K. Kohno, S. Asayama, T. Noguchi, and H. Ogawa[2008], "350 GHz Sideband Separating Receiver for ASTE," Proc. of the 19th International
Symposium on Space THz Technology, ed. Wolfgang Wild, pp.281-285.
We have developed a 350 GHz Sideband Separating Receiver for ASTE (Atacama
Submillimeter Telescope Experiment). The RF frequency range is 330-360 GHz and the IF
frequency range is 4-8 GHz. The receiver noise temperature was 150 - 200 K (SSB) and theimage rejection ratio was typically 10 dB. This receiver
was installed on the ASTE telescope in October 2007. The system noise temperature at the

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atmosphere condition ofτ220 ~ 0.6 - 0.8 was 200 K (SSB). This is almost half of that of theprevious DSB receiver.
Inoue, M., A. Haba, K. Asada, H. Nagai, Y. Murata, and P. Edwards [2008a], "Possible
Detection of Outer Plasma Around AGN Jets," Proc. of the "Mapping the Galaxy and Nearby
Galaxies", eds. Wada, K., and Combes, F., p.338.
Without abstract
Inoue, M., K. Asada, and H. Nagai [2008b], "A New Method to Detect Faraday Screen," Proc.
of the "Extragalactic Jets: Theory and Observation from Radio to Gamma Ray", eds. Travis A.
Rector and David S. De Young, ASP Conf. Ser., vol.386, pp.459-461.
We point out a possible method to investigate a plasma sheath, or Faraday screen, which has
been revealed by recent Faraday rotation studies of AGN jets. When a jet is spiral in shape, it
may happen to go across a jet trajectory behind the front jet. The plasma sheath around thefront jet can be seen as an absorption feature against the jet behind the front jet. Thisconfiguration should not be a special case when the jet trajectory is spiral in shape, and thepoint overlapping the jet with each other provides opportunity to investigate the plasma sheath.
However, it might be difficult if the sheath is thin, and high angular resolution observations are
required. VSOP observation shows a sharp absorption feature to suggest free-free absorption
by the plasma sheath, which demonstrates a reality to study the sheath.
Inoue, M., H. Nagai, K. Asada, H. Saito, and M. Tsuboi [2008c], "The Next Generation SpaceVLBI Project: VSOP-2," Proc. of the "Extragalactic Jets: Theory and Observation from Radio
to Gamma Ray", eds. Travis A. Rector and David S. De Young, ASP Conf. Ser., vol.386,
pp.262-264.
The second space VLBI project VSOP-2 has just approved, and started construction of thesatellite Astro-G in the Institute of Space and Astronautical Science (ISAS). Its key sciencetargets are to investigate physical phenomena around massive black holes with its superb
spatial resolutions up to 40 micro arcsec. By the dual polarization capability at all the threeobserving frequencies at 8, 22, and 43 GHz, VSOP-2 is anticipated to be a powerful tool toinvestigate structures of the magnetic field in AGN jets to see the acceleration and collimation
mechanisms.
Inoue, M., M. Sato, H. Saito, and M. Tsuboi [2008d], "Next Generation Space VLBI Project:
VSOP-2," Proc. of the "Observational Evidence for Black Holes in the Universe", AIP Conf.
Proc., vol.1053, pp.377-379.
The second space VLBI Project (VSOP-2) was approved, and just started construction of thesatellite ASTRO-G in the Institute of Space and Astronautical Science (ISAS). Discussion forworldwide collaboration has also been started. Its key science targets are to investigate
physical phenomena around massive black holes with its superb spatial resolutions up to 40
micro arc seconds. By the dual polarization capability at all the three observing frequencies of8, 22, and 43 GHz, VSOP-2 is anticipated to be a powerful tool to investigate structure ofaccretion disk and the magnetic field structure in AGN jets to see the acceleration andcollimation mechanisms.
Ishihara, Y., S. Sasaki, H. Araki, H. Noda, S. Tazawa, Laser Altimeter (Lalt) in Migita, E.
Kaguya, and N. Kawano [2008a], "A Preliminary Lunar Topographic Model by
KAGUYA/LALT - New Views of Lunar Topographic Features, Slope -," 37th COSPAR
Scientific Assembly, held 13-20 July 2008, in Montreal, Canada, p.1326.
Japanese lunar explorer KAGUYA (SELENE) was successfully lunched on September 14,
2007, and installed planed lunar orbit on October 19, 2007. The Laser ALTimeter (LALT)
aboard a main orbiter of KAGUYA is a ranging instrument that measures the distance between
the satellite and the lunar surface with accuracy of 5m by round trip time of the laser light. As
Kaguya is in a polar orbit, the first global and precise topographic map is expected to be

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obtained. Especially, previous experiments (ex. Clementine LIDAR) had not been gatheredhigh latitude regions (above 75-degree north and south). Our LALT will measure those regions
for the first time. The LALT nominal measurement was started on 30th, December 2007 after
the some test and adjustment phase on orbit. As of the middle of February 2008, the LALT
footprints cover thrice of the entire moon, and measurement points are reached 30,00,000. It isenough to make a preliminary LALT lunar topographic model. We started to build LALT lunar
topographic model, and compare with a previous model. Before LALT, the Unified Lunar
Control Network 2005 (ULCN2005) was most precise lunar global topographic model basedon a combination of Clementine images and a previous lunar control network derived from
Earth-based & Apollo photographs, and Mariner 10, & Galileo images. Comparing our
preliminary model with ULCN2005, it is obviously showed that lunar topographic model
would be totally (not only polar region, but also equatorial region) refined by our LALT model.
Our model is already more accurate and detail model than ULCN2005. For example, ourmodel expresses some ridge feature that had never been shown in any previous models on
near-side mare regions. In our paper, we will show preliminary LALT lunar topographic map
and slope map derived from topography. Moreover, we shall show the reflectance (@1micrometer) map derived from analysis of return laser light intensity.
Ishihara, Y., K. Matsumoto, S. Goossens, H. Araki, N. Namiki, H. Hanada, T. Iwata, H. Noda,
and S. Sasaki [2008b], "Localized Gravity/Topography Correlation Spectra on the Moon,"
Meteoritics and Planetary Sci. Suppl., vol.43, paper id. 5213.
Not Available
Ishihara, Y., H. Noda, S. Sasaki, H. Araki, E. Migita, S. Goossens, S. Tazawa, and N. Kawano[2008c], "Investigation of Lunar Impact Structures and Ridge Features by KAGUYA Altimetry(LALT) Data," American Geophysical Union, Fall Meeting 2008, abstract #P31B-1418.
The Laser ALTimeter (LALT) aboard a main orbiter of Japanese lunar explorer KAGUYA(SELENE) is a ranging instrument that measures the distance between the satellite and thelunar surface with accuracy of 5m by round trip time of the laser light every 1 second. Kaguya
is in a polar orbit, the first global, precise, high-resolution topographic map has been obtained.
Especially, previous experiments (ex. Clementine LIDAR) had not been gathered at highlatitude regions (above 75-degree north and south). Our LALT measured that region for the
first time. Using LALT data, we built a new lunar topographic mode and compared it with aprevious model. As of LALT, the Unified Lunar Control Network 2005 (ULCN2005) was mostprecise lunar global topographic model based on a combination of Clementine images and aprevious lunar control network derived from Earth-based & Apollo photographs, and Mariner
10, & Galileo images. Comparing our model with both ULCN2005 and Clementine LIDAR
model, it is obviously shown that lunar topographic model would be totally (not only polar
region, but also equatorial region) refined by our LALT model. LALT model can clarify thepresence and shape of craters as well as large impact structure. Previously unresolved heights
of central peaks of large craters are obtained. Several large impact structures in far side highland regions show multi-ring morphologies some of which were obscure in the previous map.
LALT data clarified the presence of new ring structure around Moscoviense basin. The centerof newly defined ring structure is offset from that of other Moscoviense rings. It means that,the new ring is not the third ring of Moscoviense, but it is predated impact structure. In nearside, LALT data could express some tectonic ridges and rimas within the mare region.
Ishihara, Y., N. Namiki, S. Sugita, K. Matsumoto, S. Goossens, H. Araki, H. Noda, S. Sasaki, T.
Iwata, and H. Hanada [2009a], "Localized Gravity/Topography Correlation and AdmittanceSpectra on the Moon," 40th Lunar and Planetary Science Conference, (Lunar and Planetary
Science XL), held March 23-27, 2009 in The Woodlands, Texas, id.1623.
We show the results of localized correlation and admittance analysis using new lunar gravity

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and topography models from Kaguya mission.
Ishihara, Y., S. Goossens, K. Matsumoto, H. Noda, H. Araki, N. Namiki, H. Hanada, T. Iwata,
S. Tazawa, and S. Sasaki [2009b], "Crustal Thickness of the Moon: Implications for Farside
Basin Structures," Geophys. Res. Letters, vol.36, CitelD L19202-1-4.
Based on the latest SELENE lunar gravity and topography model obtained by Kaguya mission,
we compute the lunar crustal thickness map to investigate differences between farside basin
structures. The thickest crust is located in the southern rim of the Dirichlet-Jackson basin andthe thinnest crust at the Moscoviense basin. The thickest crust corresponds to the highest
topography and is consistent with Airy isostasy. The thinnest crust is due to an abnormallylarge mantle plug. The crustal thicknesses at Apollo 12/14 sites of our crustal thickness modelare 45.1 and 49.9 km. The crustal thickness map indicates that the differences between recently
proposed type I and type II basins are probably controlled by the ratio between pre-impact
crustal thickness and impact scale.
Ishihara, Y., T. Morota, T. Iwata, K. Matsumoto, S. Goossens, and S. Sasaki [2010], "Lunar
Large Impact Basin Structures and Implications for Thermal History," LPI Contribution No.
1533, p.1559.
We reconstruct excavate cavity geometry of large impact basins on the Moon (including
farside basins) using the Kaguya crustal thickness model. We discuss the impact structures andthermal history.
Isobe, N., H. Seta, M. Tashiro, Y. Yaji, M. Hayashida, M. Terashima, K. Nakanishi, T. Tosaki,
K. Kohno, Y. Shimajiri, M. Fukuhara, M. Sasada, A. Arai, and M. Uemura [2008], "Suzaku
Observation of the Blazar OJ287; Quiescence and Predicted Flare in 2007," 37th COSPAR
Scientific Assembly, held 13-20 July 2008, in Montreal, Canada, p.1330.
OJ 287 is a famous blazar at a redshift of z = 0.306. Optical monitors of OJ 287 over morethan 100 years indicate periodic flares every about 12 years, which make the source one of themost promising candidates for a supermassive binary black holes. Since OJ 287 was predicted
to flare up in the autumn of 2007, based on the periodicity, we conducted a Suzaku X-ray
observation of OJ 287 on 2007 November 7 - 9, in corporation with radio, optical andgamma-ray observation with Nobeyama Millimeter Array, Kanata telescope, and MAGIC
telescope, respectively. Suzaku has detected the significant X-ray signals up to about 30 keV,for the first time from OJ 287, with a very hard X-ray spectrum of a photon index, Gamma~1.5. The X-ray flux of the source, ~4.5x10-12 ergs cm-2 s-1 in the 0.5 - 10 keV range, wasfound to nearly double up, compared with that of the quiescent phase obtained in the Suzaku
observation of 2007 April. We present a discussion on the nature of the quiescent and flareemissions of OJ 287, with the simultaneously obtained multi-wavelength information.
Isobe, N., M. S. Tashiro, P. Gandhi, A. Hayato, H. Nagai, K. Hada, H. Seta, and K. Matsuta[2009], "Suzaku Observation of the Giant Radio Galaxy 3C 326," Astrophys. J., vol.706,
pp.454-463.
A Suzaku observation of a giant radio galaxy, 3C 326, which has a physical size of about 2
Mpc, was conducted on 2008 January 19-21. In addition to several X-ray sources, diffuse
emission was significantly detected and associated with its west lobe, but the east lobe wascontaminated by an unidentified X-ray source WARP J1552.4+2007. After careful evaluationof the X-ray and non-X-ray background, the 0.4-7 keV X-ray spectrum of the west lobe isdescribed by a power-law model modified with the Galactic absorption. The photon index and
1 keV flux density were derived asΓ= 1.82+0.26-0.24 ± 0.04 and SX = 19.4+3.3-3.2 ± 3.0 nJy,
respectively, where the first and second errors represent the statistical and systematic ones. The
diffuse X-rays were attributed to be inverse Compton (IC) radiation by the synchrotron radio
electrons scattering off the cosmic microwave background photons. This radio galaxy is thelargest among those with lobes detected through IC X-ray emission. A comparison of the radio

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to X-ray fluxes yields the energy densities of electron and magnetic field as ue = (2.3 ± 0.3 ±0.3) × 10-13 erg cm-3 and um = (1.2+0.2-0.1 ± 0.2) × 10-14 erg cm-3, respectively. The galaxy issuggested to host a low-luminosity nucleus with an absorption-corrected 2-10 keV luminosityof <2 × 1042 erg s-1, together with a relatively weak radio core. The energetics in the west lobeof 3C 326 were compared with those of moderate radio galaxies with a size of ~100 kpc. The
west lobe of 3C 326 is confirmed to agree with the correlations for the moderate radio galaxies,ue ∼ D-2.2±0.4 and um ∼D-2.4±0.4, where D is their total physical size. This implies that the lobes
of 3C 326 are still being energized by the jet, despite the current weakness of the nuclear
activity.
Iwata, T., K. Imai, H. Misawa, H. Noda, T. Kondo, T. Nakajo, H. Takeuchi, A. Kumamoto, F.
Tsuchiya, Y. Nariyuki, K. Asari, and N. Kawano [2010], "A Study on the Moon-EarthInterferometry for Jovian Low Frequency Radio Observation," LPI Contribution No. 1533,
p.1677.
Lunar Low Frequency Astronomy Telescope (LLFAST) is the Moon-Earth baseline
interferometry which is a candidate mission instrument of Japan ﾕ s lunar explorer SELENE-2.
It will shed light on the mechanism of Jovian radio sources.
Jung, T., B. W. Sohn, H. Kobayashi, T. Sasao, T. Hirota, O. Kameya, Y. K. Choi, and H. S.
Chung [2008], "Phase Solution Analysis for the Simultaneous Dual Frequency VLBI
Observations," Proc. of the 9th European VLBI Network Symposium on The role of VLBI in
the Golden Age for Radio Astronomy and EVN Users Meeting, September 23-16, 2008,
Bologna, Italy, pp.2-6.
We present the results of the first simultaneous dual-frequency VLBI observation using
VERA(VLBI Exploration of Radio Astrometry). This experiment is a pilot study to test thefeasibility of multi-frequency phase referencing technique, which will be a main phasereferencing method for KVN (Korean VLBI Network). A pair of bright continuum sources
NRAO 512 at 22 GHz and 3C 345 at 43 GHz were simultaneously observed with dual beams
of VERA, and the fringe phases obtained for the two sources were compared to monitor thephase fluctuation at the two different frequencies. The connected phase solutions clearly
showed the non-dispersive characteristics of the neutral atmosphere at the observing
frequencies. For the differential phases of the two sources, the Allan standard deviation shows
the white phase noise behaviour up to the time scale of ~1000 sec. These preliminary results
demonstrate that the multi-frequency phase referencing technique, which will be implemented
in KVN is a promising tools to remove the atmospheric phase fluctuation effectively.
Kamata, S., S. Sugita, Y. Abe, Y. Ishihara, Y. Harada, N. Namili, H. Hanada, and H. Araki[2010], "Viscoelastic Deformation of Lunar Basins: Implications for Lunar Farside Thermal
History Based on Selenodetic Data of Kaguya," LPI Contribution No. 1533, p.1727.
Using our newly developed numerical code for viscoelastic motion of a Maxwell body, we
analyzed the result of lunar farside gravity and topography data obtained by Kaguya, yielding
several important constraints on lunar farside thermal history.
Kameno, S., M. Tsuboi, Y. Murata, A. Doi, Y. Asaki, N. Mochizuki, Y. Hagiwara, M. Kino, H.
Nagai, K. Asada, M. Inoue, H. Sudou, and S. Sawada-Satoh [2010], "VSOP-2 : A Space VLBI
Mission to Image Central Engines and Jet Launching Regions," 38th COSPAR Scientific
Assembly, 18-25 July 2010, symposium E, p.2(E11-0036-10).
VSOP-2 is a space VLBI program using the spacecraft ASTRO-G to be launched in 2015 by
the Japan Aerospace eXploration Agency. The array consisting of a 9-m antenna in orbit andground radio telescopes offers angular resolutions of 40, 80, and 210 microarcsec at 43, 22,
and 8 GHz, respectively. The resolution allows us to image accretion disks and jet launchingregions in nearby active galactic nuclei such as M 87. Dual polarization receivers enable full
Stokes images at all frequency to illustrate magnetic fields in jets. Phase referencing is capable

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for astrometry by 60-sec-cycle switching maneuvers. Higher sensitivity than the VSOP(HALCA) is achieved by cooled receivers at 22 and 43 GHz, 1-Gbps wideband downlink, andlonger coherent integration. We will introduce the mission overview, observational
specifications, and key sciences of the VSOP-2. We call for community's scientificcontributions to the mission.
Kameya, O., and VERA Team [2009], "Water Vapor Masers in the NGC7538 Region," Proc. ofthe "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies",
eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402,
pp.369-371.
Water vapor masers in the NGC7538 molecular cloud were observed with VERA. This region
has at least three active regions (IRS1-3,IRS9, and IRS11) in a dense molecular gas core. Eachregion consists of IR sources, ultra-compact HII regions, CO outflows, high-dense gas cores,
water vapor masers, OH masers, methanol masers, etc. We have performed multi epoch
observations of water vapor masers in IRS1-3 and IRS11 regions with VERA for more than
one year. The purpose of these observations are to determine the detailed distribution of water
vapor spots. The detailed distribution of the maser spots are compared with the position andshape of velocity structure of the other activities.
Kamikura, M., M. Naruse, S. Asayama, N. Satou, W. Shan, and Y. Sekimoto [2010],"Development of a Submillimeter Double-Ridged Waveguide Ortho-Mode Transducer (OMT)
for the 385-500 GHz Band," J. of Infrared, Millimeter, and Terahertz Waves, vol.31,
pp.697-707.
We present design and evaluations of a submillimeter double-ridged waveguide ortho-mode
transducer (OMT) for ALMA Band 8 (385-500 GHz) cartridge receiver. The measured
transmission loss of the OMT at 4 K was 0.4-0.5 dB according to noise measurements with an
SIS mixer. The polarization isolation was measured to be larger than 29 dB from quasiopticalmeasurements. The OMT consists of a Bϕifot junction and a double-ridged guide. A robust
design with allowable mechanical errors of 20μm has been demonstrated.
Kamohara, R., and the VERA team [2008a], "VLBI Phase-Referencing Observations of SiO
Masers towards R Aquarii," Proc. of the IAU Symp. 242, "Astrophysical Masers and their
Environments", eds. Jessica Chapman and Willem Baan, pp.322-323.
We show a phase-referenced image of the SiO maser emissions towards the Mira variable R
Aqr. These data have been obtained using the VLBI Exploration of Radio Astrometry (VERA).
The proper motion we have obtained is different from that obtained using the HST. The propermotion from 2004 to 2005 is not different from that of 1991 to 2005 and supports the current
orbital elements.
Kamohara, R., V. Bujarrabal, T. Bushimata, Y. K. Choi, T. Hirota, M. Honma, H. Imai, K.
Iwadate, T. Jike, T. Kameya, Y. Kan-ya, N. Kawaguchi, M. K. Kim, M. Kijima, H. Kobayashi,
S. Kuji, T. Kurayama, S. Manabe, T. Miyaji, T. Nagayama, A. Nakagawa, C. S. Oh, T.
Omodaka, T. Oyama, S. Sakai, T. Sasao, K. Sato, M. Sato, K. M. Shibata, Y. Tamura, and K.
Yamashita [2008b], "VERA Observations of SiO Masers in the Symbiotic Star R Aquarii,"
Publ. Astron. Soc. Japan, vol.60, pp.1023-1029.
We present phase-referenced maps of the SiO maser transitions ν=1 J=1-0 and ν=2 J=1-0 fromthe symbiotic stellar system R Aquarii, which hosts an evolved AGB star plus a hot companion.
Observations were performed at two epochs: 2004.98 and 2005.98. Accurate absolutecoordinates and proper motions of the emission centroid were obtained; the errors expected forthese parameters are also given. We compare the VERA data with the previous astrometry by
Hipparcos. This represents a possibility to improve the orbital parameters of the system in adifferent way than that done before. Thanks to our accurate astrometry, we have also estimatedthe percentage of spot coincidences between both maser transitions, a parameter that has been

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proposed to be relevant to discriminate between different maser pumping schemes. Although
the overall distributions of both lines are always similar, the spots are rarely coincident, in apercentage ranging between 3% and 20% of the cases. The lack of systematic coincidence
favors, in principle, radiative pumping. However, we argue that no firm conclusion can bereached due to a lack of models that include an overlap of rovibrational lines, and that
accurately address the coincidence of very intense spots of different maser transitions.
Kaneko, H., N. Kuno, D. Iono, T. Tosaki, T. Sawada, H. Nakanishi, and A. Hirota [2010],"Molecular Gas in the Early Stage of Interacting Galaxies: The NGC 4567/8 Pair," Proc. of the"Galaxy Wars: Star Formation and Stellar Populations in Interacting Galaxies", eds. B. J.
Smith, N. Bastian, S. J. U. Higdon, and J. L. Higdon, ASP Conf. Ser. vol.423, pp.26-31.
We present the results of 12CO(J=1-0) observations with the NRO 45m radio telescope of theinteracting galaxy pair NGC4567/8, known to be in the early stage of the interaction. Our goal
is to investigate the influence of the interaction of galaxies on molecular gas in the early stage.
This is the first CO observations covering the whole system for this galaxy pair. Their CO andHI gas distributions suggest NGC 4567/8 are surely colliding. We found high molecular gas
fraction, fmol and high star formation efficiency (SFE) in their overlap region though the low
surface density of molecular gas is low. The discrepancy of the regions with high fmol andhigh SFE may be reflecting the progression of the interaction.
Kano, R., T. Sakao, H. Hara, S. Tsuneta, K. Matsuzaki, K. Kumagai, M. Shimojo, K. Minesugi,
K. Shibasaki, E. E. Deluca, L. Golub, J. Bookbinder,D. Caldwell, P. Cheimets, J. Cirtain, E.
Dennis, T. Kent, and M. Weber [2008], "The Hinode X-Ray Telescope (XRT): Camera Design,
Performance and Operations," Solar Physics, vol.249, pp.263-279.
The X-ray Telescope (XRT) aboard the Hinode satellite is a grazing incidence X-ray imager
equipped with a 2048×2048 CCD. The XRT has 1 arcsec pixels with a wide field of view of
34×34 arcmin. It is sensitive to plasmas with a wide temperature range from < 1 to 30 MK,
allowing us to obtain TRACE-like low-temperature images as well as Yohkoh/SXT-likehigh-temperature images. The spacecraft Mission Data Processor (MDP) controls the XRTthrough sequence tables with versatile autonomous functions such as exposure control,
region-of-interest tracking, flare detection, and flare location identification. Data arecompressed either with DPCM or JPEG, depending on the purpose. This results in higher
cadence and/or wider field of view for a given telemetry bandwidth. With a focus adjust
mechanism, a higher resolution of Gaussian focus may be available on-axis. This paper
follows the first instrument paper for the XRT (Golub et al., Solar Phys. 243, 63, 2007) anddiscusses the design and measured performance of the X-ray CCD camera for the XRT and its
control system with the MDP.
Kato, M., Y. Takizawa, S. Sasaki, and Selene Project Team [2008a], "The Kaguya (SELENE)
Mission: Present Status and Science Goals," 39th Lunar and Planetary Science Conference,(Lunar and Planetary Science XXXIX), held March 10-14, 2008 in League City, Texas. LPI
Contribution No. 1391, p.1232.
Japanese lunar orbiter Kaguya (SELENE) was successfully launched on September 14, 2007.
We report the present status of the Kaguya mission and its science goals in this session.
Kato, M., Y. Takizawa, S. Sasaki, and Project Team [2008b], "The Kaguya (SELENE)
Mission: Present Status and Lunar Science," Meteoritics and Planetary Sci. Suppl., 43, paper id.
5209.
Not Available
Kato, Y., M. Miyoshi, R. Takahashi, H. Negoro, and R. Matsumoto [2010], "Measuring Spin ofa Supermassive Black Hole at the Galactic Center - Implications for a Unique Spin," Mon. Not.
Roy. Astron. Soc. (Letters,) vol.403, pp.L74-L78.
We determine the spin of a supermassive black hole in the context of disc-seismology by

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comparing newly detected quasi-periodic oscillations (QPOs) of radio emission in the Galactic
centre, Sagittarius A* (Sgr A*), as well as infrared and X-ray emissions with those of the
Galactic black holes. We find that the spin parameters of black holes in Sgr A* and in Galactic
X-ray sources have a unique value of ≈0.44 which is smaller than the generally accepted value
for supermassive black holes, suggesting evidence for the angular momentum extraction of
black holes during the growth of supermassive black holes. Our results demonstrate that the
spin parameter approaches the equilibrium value where spin-up via accretion is balanced byspin-down via the Blandford-Znajek mechanism regardless of its initial spin. We anticipate
that measuring the spin of black holes by using QPOs will open a new window for exploring
the evolution of black holes in the Universe.
Kawaguchi, N. [2008], "eVLBI Technical Development in Japan," Proc. of the 9th European
VLBI Network Symposium on The role of VLBI in the Golden Age for Radio Astronomy and
EVN Users Meeting, September 23-16, 2008, Bologna, Italy, p.41.
Not Available
Kawaguchi, N. [2009], "HALCA Data Recording and ASTRO-G?," Proc. of the "Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara,
Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.18-21.
Three different types of a data acquisition terminals were used for VSOP: the K4, the S2 andthe Mark-IV, which were developed in Japan, Canada and the U.S.A., respectively. The
compatibility was achieved by translating proceedures among the recording media, an IDR
cassette of K4, a VHS cassette of S2 and a 14=81h reel tape of Mark-IV. In the next generationof space VLBI for ASTRO-G, the strongly recommended unified interface will be the Vlbi
Standard Interface (VSI) established in 2001. Also, the successful accomplishment of thephase transfer from a ground tracking station to the space orbiting telescope is presented in thispaper by showing the statistical analysis of the loop phase fluctuations. A similar phase transfer
system is suggested to follow for the ASTRO-G project.
Kawaguchi, T., K. Nakanishi, K. Kohno, K. Ohta, and K. Aoki [2008a], "First Detection of
12
CO (1-0) Emission from Two Narrow-Line Seyfert 1 Galaxie," Astrophys. J., vol.676,
pp.137-146.
In order to investigate how the growth of galactic bulges progresses with the growth of central
black holes (BHs), we observed molecular gas (fuel for the coming star formation) in possibly
young active galaxies: narrow-line Seyfert 1 galaxies (NLS1s). We present the results of radio
observations of 12CO(1→0) using the Nobeyama Millimeter Array (with 2-4 kpc spatial
resolution) for two FIR-bright NLS1s, yielding the first detection of their CO emission.
Corresponding molecular gas masses M(H2) of (1-3)x109 Msolar are the second and fourthlargest among NLS1s. By estimating dynamical masses and bulge masses Mbulge for thesetwo NLS1s using CO channel maps and CO line widths, we found that M(H2) amounted to13%-35% of these masses. Taking into account the star formation efficiency (~0.1), theincrease in Mbulge in those NLS1s in the near future (<~107.5 yr) is not expected to be a huge
fraction (1%-5% of the preexisting stars). Bulge growth may have finished before BH growth,or bulge-BH coevolution may proceed with many occasionally discrete events, where one
coevolution event produces only a small amount of mass growth of BHs and bulges. We also
discuss the ratios of star formation rate to gas accretion rate onto BHs, finding that two NLS1s
have very small ratios (~1) compared with the Mbulge/MBH ratios found in active and inactive
galaxies (~700). This huge difference suggests either nonoverlapped coevolution, a long starformation duration, or a temporarily high accretion rate during the NLS1 phase.
Kawaguchi, T., K. Nakanishi, K. Kohno, K. Ohta, and K. Aoki, [2008b], "12CO Observations
on Narrow-Line Seyfert 1 Galaxies," Proc. of the IAU Symp. 245, "Formation and evolutionof galaxy buldge", eds. Bureau, M., Athanassoula, E., Barbuy, B., pp.249-250.

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In order to investigate how the growth of galactic bulges is accompanied with the growth ofcentral black holes (BHs), we observed molecular gas (fuel for the coming star formation) in
possibly young active galaxies, narrow-line Seyfert 1 galaxies (NLS1s). We present the resultsof pilot observations of 12CO (1→0) line using the Nobeyama Millimeter Array for two
FIR-bright NLS1s, ending in the first detection of their CO emission. Corresponding
molecular-gas masses M(H2) of (1-3) 109 M⦿are the 2nd and 4th largest ones among NLS1s.
Together with CO data for other NLS1s (including our sub-kpc observations) and forbroad-line Seyfert 1 galaxies (BLS1s), we found that NLS1s and BLS1s contain a similar
amount of molecular-gas. We do not see a significant difference in M(H2)/MBH ratios and inM(H2)/Mbulge ratios between NLS1s and BLS1s. The lack of a clear difference in M(H2)between them indicates either that bulge and BH growth phases are not overlapped or that the
duration of star formation is much longer than that of active galaxies.
Kawaguchi, T., K. Nakanishi, K. Kohno, K. Ohta, and W. Aoki [2008c], "Molecular Gas in
Narrow-Line seyfert 1 Galaxy: A Search for Coevolving Massive Black Holes and Galaxies,"
Proc. of the "Panoramic views of galaxy formation and evolution", eds. T. Kodama, T. Yamada,and K. Aoki, ASP Conf. Ser. vol.399, pp.427-428.
In order to investigate how the growth of galactic bulges progresses with the growth of central
black holes (BHs), we observed molecular gas (fuel for the upcoming star formation) in
narrow-line Seyfert 1 galaxies (NLS1s, possibly young active galaxies). We present the resultsof radio observations of 12CO (1→0) line using the Nobeyama Millimeter Array for two far
infrared (FIR)-bright NLS1s, yielding the first detection of their CO emission. Corresponding
molecular-gas masses M(H2) of (1-3) 109M⦿ are the 2nd- and 4th-largest among NLS1s. We
found that these M(H2) amounted to 13%-35% of their dynamical or bulge masses.
Kawakatu, N., H. Nagai, and M. Kino [2008], "The Fate of Young Radio Galaxies:
Decelerations Inside Host Galaxies?" Astrophys. J., vol.687, pp.141-155.
We examine the evolution of variously sized radio galaxies (i.e., compact symmetric objects[CSOs], medium-size symmetric objects [MSOs], Fanaroff-Riley type II (FR II) radio galaxies
by comparing the relation between the hot spot size and the projected linear size with a
coevolution model of hot spots and a cocoon. We take account of the deceleration effect by the
cocoon head growth. We find that the advance speed of hot spots and lobes inevitably show thedeceleration phase (CSO-MSO phase) and the acceleration phase (MSO-FR II phase). This is
ascribed to the change of the power-law index of ambient density profile in the MSO phase (~1kpc). It is also found that the cocoon shape becomes nearly spherical or disrupted for MSOs,
while an elongated morphology is predicted for CSOs and FR II galaxies. This seems to beconsistent with the higher fraction of distorted morphology of MSOs than that of CSOs and FR
II galaxies. Finally, we predict that only CSOs whose initial advance speed is higher than about
0.1 c can evolve into FR II galaxies, comparing the hot spot speed with the sound speed of theambient medium.
Kawakatu, N., M. Kino, and H. Nagai, [2009], "On the Origin of Fanaroff-Riley Classificationof Radio Galaxies: Deceleration of Supersonic Radio Lobes," Astrophys. J. (Letters), vol.697,
pp.L173-L176.
We argue that the origin of "FRI/FRII dichotomy"- the division between Fanaroff-Riley class I(FRI) with subsonic lobes and class II (FRII) radio sources with supersonic lobes is sharp inthe radio-optical luminosity plane (Owen-White diagram) ﾑ can be explained by thedeceleration of advancing radio lobes. The deceleration is caused by the growth of theeffective cross-sectional area of radio lobes. We derive the condition in which an initiallysupersonic lobe turns into a subsonic lobe, combining the ram pressure equilibrium between
the hot spots and the ambient medium with the relation between "the hot spot radius" and "thelinear size of radio sources" obtained from the radio observations. We find that the dividing

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line between the supersonic lobes and subsonic ones is determined by the ratio of the jet power
Lj to the number density of the ambient matter at the core radius of the host galaxy na. It isalso found that the maximal ratio of Lj/na exists and its value resides in (Lj/na)max ≈1044-47
erg s-1 cm3, taking into account considerable uncertainties. This suggests that the maximal
value (Lj/na)max separates between FRIs and FRIIs.
Kawamura, A. [2008], "Molecular Clouds and Star Formation in the Magellanic Clouds andthe Milky Way," Astrophys. Sp. Sci., vol.313, pp.145-151.
Star formation is a fundamental process that dominates the life-cycle of various matters ingalaxies: Stars are formed in molecular clouds, and the formed stars often affect thesurrounding materials strongly via their UV photons, stellar winds, and supernova explosions.
It is therefore revealing the distribution and properties of molecular gas in a galaxy is crucial toinvestigate the star formation history and galaxy evolution. Recent progress in developing
millimeter and sub-millimeter wave receiver systems has enabled us to rapidly increase ourknowledge on molecular clouds. In this proceedings, the recent results from the surveys of themolecular clouds in the Milky Way and the Magellanic Clouds as well as the Galactic center as
the most active regions in the Milky Way are presented. The high sensitivity with unrivaled
high resolution of ALMA will play a key role in detecting denser gas that is tightly connected
to star formation.
Kikuchi, F., Q. Liu, N. Petrova, K. Matsumoto, Y. Ishihara, S. Goossens, K. Asari, S. Tsuruta,
T. Ishikawa, H. Noda, H. Hanada, T. Iwata, N. Namiki, N. Kawano, and S. Sasaki [2008a],"Preliminary Results for VRAD Mission of Kaguya (SELENE)," 39th Lunar and Planetary
Science Conference, (Lunar and Planetary Science XXXIX), held March 10-14, 2008 in
League City, Texas. LPI Contribution No. 1391, p.1562.
The preliminary analysis of VRAD mission of Kaguya has been carried out and theperformance of the system is confirmed. The differential phase delay of the signal from twosatellites is derived without the cycle ambiguity within an error of 2 pico-seconds.
Kikchi, F., Q. Liu, K. Matsumoto, H. Hanada, and N. Kawano [2008b], "Simulation Analysis
of Differential Phase Delay Estimation by Same Beam VLBI Method," Earth, Planets andSpace, vol.60, pp.391-406.
The same beam VLBI method (SBV) is newly applied to the multi-frequency VLBI method in
the VRAD mission of SELENE (KAGUYA). By simultaneously observing two nearby
spacecraft with one antenna, the error sources of VLBI measurement common in two
propagation paths can be almost canceled out. In this paper, error estimation and simulation
analysis are carried out for a feasibility study to apply the SBV method to the VRAD mission.
Differential phase delay can be estimated without cycle ambiguity even if troposphericfluctuation is large and/or traveling ionospheric disturbance occurs. The sensitivity of thedifferential phase delay with respect to the average elevation angle and the elongation of two
spacecraft is also investigated. Moreover, a method is developed for estimating differential
phase delay in switching VLBI observations using the cycle ambiguity derived from SBV
observations. This method can be performed in more than 90% of the VRAD mission's total
paths. Precise positioning with SBV contributes to accurate estimation of the low degree
coefficients of lunar gravity fields by more than one order of magnitude than previous results.
Kikuchi, F., Q. Liu, N. Petrova, H. Noda, K. Matsumoto, Y. Ishihara, S. Goossens, T. Iwata, N.
Namiki, H. Hanada, N. Kawano, and S. Sasaki [2008c], "VLBI Observations in VRAD
Mission of KAGUYA (SELENE)," 37th COSPAR Scientific Assembly, held 13-20 July 2008,
in Montreal, Canada, p.1508.
One of the important questions still remaining about the Moon is the existence and state of a
lunar core. The size and density of the lunar core estimated from the moment of inertia of theMoon are important constraints for investigating the origin of the Moon. However, the lack of

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accurate gravity field information especially for the far side and the limb region of the Moon
restrict the accuracy of the moment of inertia of the Moon. In Japanese lunar exploring
program KAGUYA (SELENE), VRAD (the differential VLBI RADio sources) mission iscarried out to improve the accuracy of the lunar gravity field. Two VLBI radio sources areloaded on two sub-satellites called Rstar and Vstar. These on-board radio sources transmit four
carrier wave signals and the differential VLBI observations between Rstar and Vstar are
carried out. The differential phase delay (DPD), which is the measurement of the differential
VLBI, is highly sensitive to the relative position and velocity of the two sub-satellites in the
direction perpendicular to the line-of-sight (LOS). VRAD is expected to contribute to theimprovement of the gravity field over the limb region. After combining with the 2-way and4-way Doppler observation in the RSAT (the Relay SAtellite Transponder) mission, which issensitive to the LOS direction, the spacecraft's three-dimensional motion can be determinedand precise global lunar gravity field estimation will be possible. Highlight of this work is theapplication of the same-beam VLBI method for DPD estimation. By simultaneously observing
two nearby spacecraft, most of tropospheric and ionospheric delays that are major error
sources of VLBI can be canceled out. This makes it possible to derive the cycle ambiguity of
the DPD by multi-frequency VLBI (MFV) method. As the result of the data analysis, the DPD
can be estimated without the cycle ambiguity. The error of DPD is smaller than 2 ps in
30-second integration interval. The desired accuracy of the VRAD mission is successfully
achieved and it is expected that VRAD will contribute to improve the accuracy of the lunar
gravity field estimation. In the presentation, the results of the DPD estimation as well as theprocess of the cycle ambiguity reduction are shown. The details of the dedicated VRAD
system, the analysis software, and the same-beam VLBI observation method are also shown.
Kikuchi, F., Q. Liu, H. Hanada, N. Kawano, K. Matsumoto, T. Iwata, S. Goossens, K. Asari, Y.
Ishihara, S. Tsuruta, T. Ishikawa, H. Noda, N. Namiki, N. Petrova, Y. Harada, J. Ping, and S.
Sasaki [2009], "Picosecond Accuracy VLBI of the Two Subsatellites of SELENE (KAGUYA)
Using Multifrequency and Same Beam Methods," Radio Sci.vol.44, pp.RS2008-1-7.
Same beam very long baseline interferometry (VLBI) observations of the two subsatellites of
SELENE (KAGUYA) are demonstrated for purpose of the precise gravimetry of the Moon.
Same beam VLBI contributes a great deal to cancel out the tropospheric and ionosphericdelays and to determine the absolute value of the cycle ambiguity by using the multifrequency
VLBI method. As a result, the differential phase delay of the X-band signal is estimated within
an error of below 1 ps. This accuracy is more than 1 order of magnitude smaller than former
VLBI results. The preliminary results for the orbit determination of the subsatellites show adecrease of the orbit error from a few hundreds of meters to around 10 m when the differential
phase delay data are added to the conventional range and Doppler data. These results reveal thepossibility of precise gravimetry.
Kikuchi, F., Q. Liu, N. Petrova, Y. Harada, H. Hanada, T. Iwata, N. Namiki, N. Kawano, and S.
Sasaki, [2010], "Differential Phase Delay Estimation in VRAD Mission of SELENE(KAGUYA)," Trans. of Sp. Tech. Japan, vol.7, Ppp.k7-Pk10.
In the very long baseline interferometry (VLBI) radio sources mission of selenological andengineering explorer, the differential phase delay between the Rstar and Vstar sub-satellites isobtained by using the multifrequency VLBI method during the switching VLBI observation
period. The cycle ambiguity is successfully determined and the differential phase delay isestimated within an error of 7 picoseconds. The RMS error is somewhat larger than that for thecase of same-beam VLBI because fluctuations of propagation delays whose periods are shorter
than the switching interval cannot be canceled out between Rstar and Vstar. However, thedifferential phase delay during the switching VLBI period is sufficiently accurate and, together
with Doppler and range measurements, can be a useful means for precisely determining

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satellite orbits and precisely estimating the lunar gravity field.
Kim, M. K., T. Hirota, M. Honma, H. Kobayashi, T. Bushimata, Y. K. Choi, H. Imai, K.
Iwadate, T. Jike, S. Kameno, O. Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, S. Kuji, T.
Kurayama, S. Manabe, M. Matsui, N. Matsumoto, T. Miyaji, T. Nagayama, A. Nakagawa, C. S.
Oh, T. Omodaka, T. Oyama, S. Sakai, T. Sasao, K. Sato, M. Sato, K. M. Shibata, Y. Tamara,and K. Yamashita [2008], "SiO Maser Observations toward Orion-KL with VERA," Publ.
Astron. Soc. Japan, vol.60, pp.991-999.
We present results of phase-referencing VLBI observations of SiO masers in the Orion-KL
region made with VERA. Using a strong maser spot in the 43 GHz ν=1-0 emission, we derived
the trigonometric parallax of Orion-KL to be 2.39±0.03 mas, corresponding to a distance of
418±6pc, with the highest accuracy among existing parallax measurements of the source. We
made a superimposed image of ν=1 J=1-0 and ν=2 J=1-0 maser features in Orion-KL based on
absolute positions obtained from the phase-referencing with a common reference source. The
maser features of both transitions show similar X-shaped distributions centered at Source I.
However, in each of the four arms of the X-shape, the SiO ν=2 features tend to lie closer to
Source I than the SiO ν=1 features. The radial velocities of the maser emission decrease withthe distance from Source I. The spatial and radial velocities distributions of the SiO masers
suggest that the SiO masers lie in the rotating materials associated with a disk around Source I,
rather than a decelerating outflow.
Kim, M. K., T. Hirota, M. Honma, H. Kobayashi, and other VERA members [2009], "SiO
Maser Observations toward Orion-KL with VERA," Proc. of the "Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara,
Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.469-472.
We present results of phase-referencing VLBI observations of SiO masers in the Orion KL
region made with VERA. The goal of our study is to investigate the dynamics of the gas
surrounding Source I, as well as to determine the distance to Orion-KL. We imaged SiO v=1,
J=1-0 and v=2, J=1-0 maser emission in Orion-KL and compared the absolute positions of themaser spots with that of Source I. The maser emission shows an X-shaped distribution
centered at Source I, and the SiO v=2 emission lies closer to Source I than the SiO v=1
emission. The radial velocities and proper motions of the maser spots indicate that the gas
around Source I is rotating and expanding. In addition, we present the preliminary result of themeasurement of the annual parallax using the SiO v=2 emission. The parallax of Orion-KL is
2.39±0.03 mas, corresponding to the distance of 418±6 pc.
Kimura, K., H. Iwashita, S. Asayama, M. Sugimoto, G. Kikuchi, and H. Ogawa [2008],"Antenna Performance of a Directory Dug Corrugated Feedhorn for the 150-GHz Bnad," Int. J.
of IR and MM Waves, vol.29, pp.713-723.
We have developed a 150 GHz band corrugated feed horn. These corrugated feed horns havebeen established by a new machining method, which involves digging corrugations through ametal material. We were able to realize E plane and H plane symmetry, low side lobe level, andlow cross-polarization level. Measured co-polarization beam patterns above -35 dB wereconsistent with the simulated patterns within a designed frequency range. The peak levels ofcross-polarization beam patterns were less than -30 dB. And, the performances were uniform
in several horns. In the present paper, we describe the corrugated horn produced by thismethods.
Kimura, K., T. Toshikawa, N. Shiroyama, A. Kurozumi, T. K. Ojima, Y. Abe, Y. Yonekura, H.
Ogawa, H. Ujihara, Y. Murata, M. Tsuboi, and T. Kasuga [2009], "Simulation of the Optical
System for the ASTRO-G Offset Cassegrain Antenna," Proc. of the "Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara,
Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.74-76.

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We are developing the satellite (ASTRO-G) for the space VLBI mission, called VSOP-2(Hirabayashi et al. 2004). This system will have an offset cassegrain antenna, and the threemulti-mode feed horns (8, 22, 43 GHz bands) will be chosen by the Cassegrain focus position.
We are designing the antenna optics of the three band receivers by using the GRASP physical
optics software package on simulated feed configurations. The result of these simulations
shows low cross-polarization level, a good radiation pattern, and the antenna efficiencies are
63 ﾐ 68 percent in these bands, assuming a perfect reflector. In this paper, we present theseresults of simulation of ASTRO-G antenna optics.
Kino, M., K. Asada, Y. Hagiwara, P. G. Edwards, and VSOP-2 Science Working Group [2009],"Direct Observations of the Dynamics and Variability at High Energy Emission Regions in
TeV Blazars," Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y.,
ASP Conf. Ser. vol.402, pp.270-273.
VSOP-2 observations of “blazar” may be part of the VSOP-2 Key Science Program for Active
Galactic Nuclei. We propose VSOP-2 observations of nearby blazars together with amulti-frequency campaign observations. For example, in two nearby TeV blazars Mrk 421 andMrk 501, the 38 micro-arcsec resolution corresponds to about 0.03 pc in linear scale, which iscomparable to the size of the high energy emission region in the standard one-zone model. We
show the advantages of VSOP-2 observation of these blazars compared with previous VLBI
studies, and discuss some relevant unresolved problems.
Kobayashi, H., N. Kawaguchi, S. Manabe, K. M. Shibata, M. Honma, Y. Tamura, O. Kameya,
T. Hirota, T. Jike, H. Imai, and T. Omodaka [2008a], "Phase Referencing VLBI Astrometry
Observation System: VERA," Proc. of the IAU Symp. 248, "A Giant Step: from Milli- to
Micro-arcsecond Astrometry", eds. Wenjing Jin, Imants Platais, Michael A. C. Perryman,
pp.148-155.
VERA aims at astrometric observations using phase referencing VLBI techniques, whose goal
is a 10 micro arc-second accuracy for annual parallax measurements. VERA has four 20-m
diameter VLBI radio telescopes in Japanese archipelago with the maximum baseline length of
2,300 km. They have the two-beam observing system, which makes simultaneous observationsof two objects possible. This leads to very accurate phase referencing VLBI observations. An
important science goal is to make a 3-dimensional map of the Galaxy and reveal its dynamics.
In order to achieve this, VERA has the 22GHz and 43GHz bands for H2O and SiO maser
objects, respectively. Maser objects are compact and suitable for astrometry observations.
VERA's construction was started in 2000 and the array became operational in 2004. We havealready measured annual parallaxes and proper motions of some galactic objects. In the future,
VERA will collaborate with Korean and Chinese VLBI stations.
Kobayashi, H. [2008b], "Recent Activities of VERA and East Asia VLBI Network," Proc. of
the 9th European VLBI Network Symposium on The role of VLBI in the Golden Age forRadio Astronomy and EVN Users Meeting, September 23-16, 2008, Bologna, Italy, p.48.
Not Available
Kobayashi, M., H. Ohashi, S. Sasaki, T. Iwai, M. Fujii, K. Nogami, H. Kimura, M. Nakamura,and T. Hirai [2010], "Lunar Dust Monitor for the Orbiter of the Next Japanese Lunar Mission
SELENE2," LPI Contribution No. 1533, p.1964.
A dust particle detector is proposed to be onboard the orbiter of SELENE-2 mission. We
summarize the significance of circumlunar dust and report an overview of our instrument
proposed to accompany the SELENE-2 mission.
Koda, J., and CARMA team [2007], "CARMA M51 Project: Dynamically-Driven ISM
Evolution," American Astron. Soc., AAS meeting #211, #153.04, BAAS, vol.39, p.1005.
The entire M51 disk is observed in CO(1-0) line with the CARMA interferometer and

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Nobeyama 45m telescope. With the unprecedented high image fidelity and spatial resolution,
we detect many giant molecular clouds (GMCs) both on spiral arms and in interarm regions.
Associations of giant molecular clouds (GMAs) are found only on spiral arms, and thus, they
are unbound, short-lived structures. Molecular gas fraction is high even in interarm regions.
Therefore, the GMA destruction is not caused by stellar feedback, which is likely to destroy
molecules as well as GMAs and GMCs. We will discuss dynamically-driven ISM evolution -strong shear motions in spiral arms cause GMA destruction and trigger ISM evolution.
Koda, J. [2008], "Star Formation and Interstellar Medium Evolution in Galaxies," Proc. of the"Formation and evolution of galaxy disks", eds. J. G. Funes, and E. M. Corsini, ASP conf. Ser.,vol.396, pp.97-104.
I review recent studies of star formation in galaxies, and discuss the underlying structure of theinterstellar medium (ISM). Studies of star formation in galaxies have been limited by spatial
resolution, and focused mostly on empirical correlations between star formation rate and gas
properties averaged over large areas. With recent and upcoming facilities (e.g., Spitzer,
GALEX, CARMA, Herschel, and ALMA), studies of star formation are transitioning to theregime in which the star forming regions and their local environment are well-resolved. With
this in mind, I re-consider classical arguments for star formation (e.g., Toomre criterion) by
taking into account the underlying gas structure. With new CO(1-0) data from CARMA andNobeyama 45-m telescope, I show the evolution of the ISM in M 51, and argue that theevolution is largely triggered by global galactic dynamics.
Koda, J., and Nearby Galaxies CO survey Group [2009a], "CARMA & Nobeyama CO Surveyof Nearby Galaxies," American Astron. Soc., AAS meeting #213, #485.04.
Our observations of M51 in CO(1-0) line with CARMA and Nobeyama 45m telescope hasrevealed a new picture of ISM evolution in galaxies, namely one driven by galaxy's global
dynamics -- the most massive GMCs (Giant Molecular Associations - GMAs) are first
assembled and then broken up as the gas flow through the spiral arms. The GMAs and their H2molecules are not fully dissociated into atomic gas as predicted in stellar feedback scenarios,
but are fragmented into smaller GMCs upon leaving the spiral arms. We have initiated a new
survey of nearby galaxies in CO(1-0) line with CARMA and Nobeyama 45m telescope,
probing the generality of the scenario of dynamically-driven ISM evolution. The sample isselected from that of the Spitzer SINGS survey, and comprises the most famous nearby
galaxies with the full range of ancillary data; those data are crucial in our study of ISM
evolution (CARMA, Nobeyama ¥& VLA) and star formation (Spitzer, GALEX ¥& Herschel).
We will present initial results from this new CO survey.
Koda, J., N. Scoville, T. Sawada, M. A. La Vigne, S. N. Vogel, A. E. Potts, J. M. Carpenter, S.
A. Corder, M. C. Wright, S. M. White, B. A. Zauderer, J. Patience, A. I. Sargent, D. C. J. Bock,
D. Hawkins, M. Hodges, A. Kemball, J. W. Lamb, R. L. Plambeck, M. W. Pound, S. L. Scott, P.
Teuben, and D. P. Woody [2009b], "Dynamically Driven Evolution of the Interstellar Medium
in M51," Astrophys. J. (Letters), vol.700, pp.L132-L136.
Massive star formation occurs in giant molecular clouds (GMCs); an understanding of theevolution of GMCs is a prerequisite to develop theories of star formation and galaxy evolution.
We report the highest-fidelity observations of the grand-design spiral galaxy M51 in carbon
monoxide (CO) emission, revealing the evolution of GMCs vis-a-vis the large-scale galactic
structure and dynamics. The most massive GMCs (giant molecular associations (GMAs)) are
first assembled and then broken up as the gas flow through the spiral arms. The GMAs andtheir H2 molecules are not fully dissociated into atomic gas as predicted in stellar feedback
scenarios, but are fragmented into smaller GMCs upon leaving the spiral arms. The remnantsof GMAs are detected as the chains of GMCs that emerge from the spiral arms into interarm
regions. The kinematic shear within the spiral arms is suf ﾞ cient to unbind the GMAs against

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self-gravity. We conclude that the evolution of GMCs is driven by large-scale galactic
dynamics-their coagulation into GMAs is due to spiral arm streaming motions upon entering
the arms, followed by fragmentation due to shear as they leave the arms on the downstreamside. In M51, the majority of the gas remains molecular from arm entry through the interarm
region and into the next spiral arm passage.
Kohno, K., K. Nakanishi, T. Tosaki, K. Muraoka, R. Miura, H. Ezawa, and R. Kawabe [2008a],"Dense Gas in Normal and Active Galaxies," Astrophys. and Sp. Sci., vol.313, pp.279-285.
Dense molecular medium plays essential roles in galaxies. As demonstrated by the tight andlinear correlation between HCN(1-0) and FIR luminosities among star-forming galaxies, fromvery nearby to high-z ones, the observation of a dense molecular component is indispensable
to understand the star formation laws in galaxies. In order to obtain a general picture of the
global distributions of dense molecular medium in normal star-forming galaxies, we haveconducted an extragalactic CO(3-2) imaging survey of nearby spiral galaxies using the
Atacama Submillimeter Telescope Experiment (ASTE). From the survey (ADIoS; ASTE
Dense gas Imaging of Star-forming galaxies), CO(3-2) images of M 83 and NGC 986 arepresented. Emphasis is placed on the correlation between the CO(3-2)/CO(1-0) ratio and thestar formation efficiency in galaxies. In the central regions of some active galaxies, on theother hand, we often find enhanced or overluminous HCN(1-0) emission. The
HCN(1-0)/CO(1-0) and HCN(1-0)/HCO+(1-0) intensities are often enhanced up to ~0.2-0.3
and ~2-3, respectively. Such elevated ratios have never been observed in the nuclear starburst
regions. One possible explanation for these high HCN(1-0)/CO(1-0) and
HCN(1-0)/HCO+(1-0) ratios is X-ray induced chemistry in X-ray dominated regions (XDRs),i.e., the overabundance of the HCN molecule in the X-ray irradiated dense molecular tori. If
this view is true, the known tight correlation between HCN(1-0) and the star-formation rate
breaks in the vicinity of active nuclei. Although the interpretation of these ratios is still an open
question, these ratios have a great potential for a new diagnostic tool for the energy sources of
dusty galaxies in the ALMA era because these molecular lines are free from dust extinction.
Kohno, K. [2008b], "ASTE Surveys of Galactic Star-Forming Regions," Bulletin of American
Astronomical Society, vol.40, p.272.
We report some recent highlights on the observational studies of Galactic star formation basedon surveys using the Atacama Submillimeter Telescope Experiment (ASTE), a new 10 m
telescope in the Atacama desert in northern Chile (Kohno et al., 2008, ApSS, 313, 279). The
highlights will include (1) a large scale CO(3-2) imaging survey of the Galactic Center,
unveiling the presence of numerous compact high velocity clouds with high CO(3-2)/CO(1-0)
ratios as a "fossil'' of the recent burst of star formation in the Galactic Center region (Oka et al.,2007, PASJ, 59, 15; Nagai et al., 2007, PASJ, 59, 25; Tanaka et al., 2007, PASJ, 59, 323), (2) alarge scale CO(3-2) imaging survey of the Sgr arm and inter-am regions, revealing the distinct
difference on the morphology and physical property of molecular gas between the arm andinter-arm regions for the first time (Sawada, Koda, et al., in prep.), and (3) a wide area 1.1 mm
imaging survey of Southern low mass star-forming regions such as Chamaeleon and Lupus
molecular clouds using the bolometer camera AzTEC (Wilson et al., 2008, MNRAS, in press)
mounted on ASTE, yielding detections of starless cores with a very low mass detection limist
down to 0.1 solar masses (Hiramatsu, Tsukagoshi, Kawabe et al., in prep.). Related topics on
the massive star-forming regions in very nearby galaxies such as LMC (Minamidani et al.,2008, ApJS, in press) and M 33 (Tosaki et al., 2007, ApJ, 664, L27; Onodera et al., in prep.;
Komugi et al., in prep.) will also be reviewed.
Kohno, K., T. Tosaki, R. Miura, K. Muraoka, T. Sawada, K. Nakanishi, N. Kuno, T. Sakai, K.
Sorai, K. Kamegai, K. Tanaka, T. Okuda, A. Endo, B. Hatsukade, M. Sameshima, H. Ezawa, S.
Sakamoto, T. Kamazaki, N. Yamaguchi, J. Cortes, Y. Tamura, M. Fukuhara, D. Iono, and R.

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Kawabe [2008c], "ASTE CO(3-2) Observations of the Southern Barred Spiral Galaxy NGC
986: a Large Gaseous Bar Filled with Dense Molecular Medium," Publ. Astron. Soc. Japan,
vol.60, pp.457-464.
We present CO(3-2) emission observations toward the 3'x3' (or 20x20kpc at a distance of
23Mpc) region of the southern barred spiral galaxy NGC 986 using the Atacama Submillimeter
Telescope Experiment (ASTE). This effort is a part of our on-going extragalactic CO(3-2)
imaging project ADIoS (ASTE Dense gas Imaging of Spiral galaxies). Our CO(3-2) image
revealed the presence of a large (the major axis is 14 kpc in total length) gaseous bar filledwith dense molecular medium along the dark lanes observed in optical images. This is thelargest "dense-gas rich bar'' known to date. The dense gas bar discovered in NGC 986 could bea huge reservoir of possible "fuel'' for future starbursts in the central region, and we suggestthat the star formation in the central region of NGC 986 could still be in a growing phase. We
found a good spatial coincidence between the overall distributions of dense molecular gas
traced by CO(3-2) and the massive star formation depicted by H . The global CO(3-2)
luminosity L'CO(3-2) of NGC 986 was determined to be (5.4 ± 1.1) ×108 K km s-1 pc2. The
CO(3-2)/CO(1-0) integrated intensity ratio was found to be 0.60 ± 0.13 at a spatial resolutionof 44'' or 5 kpc, and a CO(3-2)/CO(2-1) ratio was 0.67 ± 0.14 at a beam size of ~25'' or ~2.8
kpc. These line ratios suggest moderate excitation conditions of CO lines (nH2 ~ 103-4 cm-3) inthe central a few kpc region of NGC 986.
Kohno, K., K. Muraoka, B. Hatuskade, K. Tanaka, D. Iono, K. Nakanishi, T. Tosaki, T. Sawada,
R. Kawabe, H. Ezawa, N. Yamaguchi, Y. Tamura, G. Wilson, M. S. Yun, D. Hughes, S.
Matsushita, and P.-Y. Hsieh [2008d], "Tracing Star Formation in Galaxies with Molecular Lineand Continuum Observations," EAS Publication Series, vol.31, pp.65-71.
We report our recent progress on extragalactic spectroscopic and continuum observations,
including HCN(J=1-0), HCO+(J=1-0), and CN(N=1-0) imaging surveys of local Seyfert andstarburst galaxies using the Nobeyama Millimeter Array, high-J CO observations (J=3-2
observations using the Atacama Submillimeter Telescope Experiment (ASTE) and J=2-1
observations with the Submillimeter Array) of galaxies, and λ1.1 mm continuum observationsof high-z violent starburst galaxies using the bolometer camera AzTEC mounted on ASTE.
Kohno, K., Y. Tamura, B. Hatsukade, K. Nakanishi, D. Iono, T. Takata, G. W. Wilson, M. S.
Yun, T. Perera, J. E. Austermann, K. S. Scott, H. Hughes, I. Aretxaga, K. Tanaka, N.
Yamaguchi, H. Matsuo, H. Ezawa, and R. Kawabe [2008e], "AzTEC on ASTE Survey ofSubmillimeter Galaxies," Proc. of the "Panoramic views of galaxy formation and evolution",eds. T. Kodama, T. Yamada, and K. Aoki, ASP Conf. Ser. vol.399, pp.264-267.
We have conducted an unprecedented survey of submillimeter galaxies (SMGs) using the 144
pixel bolometer camera AzTEC mounted on the ASTE 10-m dish in Chile. We have alreadyobtained many (>20) wide (typically 12' x 12' or wider) and deep (1 σ sensitivity of 0.5-1.0mJy) 1.1 mm continuum images of known blank fields and over-density regions/protoclusters
across a wide range of redshifts with a spatial resolution of ~30". It has resulted in the
numerous (~ a few 100, almost equivalent to the total number of the previously known SMGs)
new and secure detections of SMGs. In this paper, we present initial results of two selected
fields, SSA 22 and AKARI Deep Field South (ADFS). A significnat clustering of bright SMGs
toward the density peak of LAEs is found in SSA 22. We derived the differential andcumulative number counts from the detected sources in ADF-S, which probe the faintest flux
densities (down to -1 mJy) among 1-mm blank field surveys to date.
Komugi, S., Y. Sofue, H. Nakanishi, S. Onodera, F. Egusa, K. Muraoka, and J. S. Young[2008a], "Molecular Gas and Star Formation in Nearby Galaxies," Proc. of the "Mapping the
Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F., pp.231-236.
The quantitative relationship between molecular gas and star formation, or the Schmidt Law,

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was derived for the central kpc of nearby spiral galaxies using 12CO(J=1-0) line data and H
alphaimaging. The CO spectra were obtained at the 45m telescope at Nobeyama Radio
Observatory (NRO). The derived Schmidt law index is found to be affected significantly
depending on galaxy distance, ranging from 0.7 to 1.3. The data covers the densest regions ofnormal spirals, and overlaps with starburst galaxies. We categorize the Schmidt law according
to existence of bars. Barred galaxies are found to display a Schmidt law with higher gas
density, but on the same Schmidt law track as non-barred samples.
Komugi, S., Y. Sofue, S. Onodera, F. Egusa, K. Muraoka, H. Nakanishi, and J. S. Young[2008b], "The Star Formation Law as a Function of Galactic Properties," Proc. of the"Pathways Through an Eclectic Universe", eds. J. H. Knapen, T. J. Mahoney, and A. Vazdekis,
ASP Conf. Ser., vol.390, pp.161-165.
The relation between molecular gas quantity and star formation rate, known as the Schmidt law,is tested for its dependency on galactic morphology, with an emphasis on the presence of bars.
The galaxy sample is based on a survey of the 12CO(J = 1→0) emission in nearby galaxies
completed at the Nobeyama Radio Observatory 45m telescope, combined with previous
surveys with similar resolution. These data were compared to star formation rates derived
using internal extinction corrected Hα. The slope of the Schmidt law is found to varyconsiderably with sample distance, from 0.7 to 1.4. The Schmidt law is categorized according
to the presence of bars. Consequently, we find that barred galaxies occupy the denser regime of
the Schmidt law, but with no apparent difference in the star formation efficiency, indicatingthat bars stimulate central inflow of gas, but that star formation still occurs according to acommon star formation law as with non-barred galaxies.
Komugi, S., Y. Sofue, K. Kohno, H. Nakanishi, S. Onodera, F. Egusa, and K. Muraoka [2008c],"Molecular Gas Distribution in Barred and Non-Barred Galaxies along the Hubble Sequence,"
Astrophys. J. Suppl, vol.178, pp.225-246.
We present results from a survey of 12CO (J=1-0) spectra obtained for the central regions of 68
nearby galaxies at an angular resolution of 16" using the Nobeyama Radio Observatory 45 m
telescope, aimed at characterizing the properties of star-forming molecular gas. Combined withobservations of similar resolution in the literature, the compiled sample set of 166 galaxies
span a wide range of galactic properties. NGC 4380, which was previously undetected in CO,
was detected. This initial paper of a series will focus on the data and the gaseous properties ofthe samples, and particularly on the degree of central concentration of molecular gas in a rangeof morphological types, from early (S0/Sa) to late (Sd/Sm) galaxies with and without bars. The
degree of molecular central concentration in the central kiloparsec, compared with the central
several kiloparsecs of galaxies, is found to vary smoothly with Hubble type, so that early-typegalaxies show larger central concentration. The comparison of barred and nonbarred galaxies
within early- and late-type galaxies suggest that difference in Hubble type, representing theeffect of bulges, is the more important factor in concentrating gas into the central regions thanbars.
Kotani, T., S. Fabrika, N. Kawai, K. Kinugasa, K. Kubota, S. Trushkin, and M. Tsuboi [2009],"Multi-Wavelength Observations of the Microquasar SS433," Proc. of "Astrophysics with
All-Sky X-Ray Observations", pp.108-113.
A radio-IR-optical-X-ray observation campaigns have been performed in 2006 April and 2006
December for SS433, the unique microquasar known for the very stable continuous jet
emanating at a quarter of the speed of light. The participating observatories/telescopes include
Suzaku, RXTE, BTA, 150-cm Telescope at Gunma, Nayuta at Nishi-Harima, Crimean
Observatory, MITSuME, VSOLJ, 1.4-m Telescope at SAAO, RATAN-600, RT-32 at IAA RAS,
and Nobeyama Millimeter Array. In the April campaign, five radio flares have been detected
and the source seems to be in the active state. In the December campaign, a simple radio flare

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has been detected, and we triggered a series of observations with RXTE.
Kuno, N., A. Hirota, T. Tosaki, and R. Miura [2008a], "Observations of molecular clouds innearby galaxies with ALMA," Astrophys. and Sp. Sci., vol.313, pp.293-296.
We present recent results of the observations of giant molecular clouds in nearby galaxies with
the Nobeyama 45 m telescope and Millimeter Array. We give some brief comments about
observations of GMCs in nearby galaxies with ALMA.
Kuno, N., N. Sato, H. Nakanishi, A. Hirota, T. Tosaki, Y. Shioya, K. Sorai, N. Nakai, K.
Nishiyama, and B. Vila-Vilaro [2008b], "Nobeyama CO Atlas of Nearby Spiral Galaxies,"
Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F.,
pp.170-177.
The results of a CO(1-0) mapping survey of 40 nearby spiral galaxies performed with theNobeyama 45-m telescope are presented. The maps of CO cover most of the optical disk of thegalaxies. We investigated the influence of bar on distribution of molecular gas in spiralgalaxies using these data. We confirmed that the degree of central concentration is higher inbarred spirals than in non-barred spirals as shown by previous works. Furthermore, we showthat bars are efficient in driving molecular gas that lies within their radial scales toward thecenter, while the role in the accumulation from the larger spatial scales on the disks is small.
The transported gas accounts for about half of molecular gas within the central region in barredspiral galaxies. We found a correlation between the degree of central concentration and bar
strength. Galaxies with stronger bars tend to have higher central concentration. The correlation
implies that stronger bars accumulate molecular gas toward the center more efficiently. These
results are consistent with long-lived bars.
Kuno, N., K. Nakanishi, K. Sorai, and T. Shibatsuka [2008c], "Central Spiral Structure of
Molecular Gas in Maffei 2," Publ. Astron. Soc. Japan, vol.60, pp.475-485.
The distribution and kinematics of molecular gas in the central region of the barred spiralgalaxy Maffei 2 were investigated using a data set of 12CO(1-0), 12CO(2-1), CS(2-1) lines, and
103 GHz continuum. We found that the offset ridges along the kpc-scale bar continue to thecentral spiral structure embedded in a weak oval structure, which is regarded as χ2 orbit in thebar potential. The spiral structure continues toward the center, diverging from the oval
structure. The size of these structures is less than R ~ 100 pc. The mass concentration within R= 35 pc is estimated to be 2 X 108 M⦿. The high mass concentration is consistent withtheoretical predictions concerning the creation of such a nuclear spiral structure. A comparison
with the tracers of dense gas and star-forming region suggests that the dense molecular gas
traced by the CS(2-1) line is formed at the crossing points of the x1 and x2 orbits and thestar-forming region appears after 2 X 105 yr, which is comparable to the free-fall time of dense
gas traced by the CS line (~ 105 cm-3).
Kuno, N., T. Tosaki, S. Onodera, K. Muraoka, H. Kaneko, T. Sawada, K. Nakanishi, S.
Komugi, Y. Tamura, K. Kohno, R. Kawabe, N. Arimoto, and S. Okamoto [2010], "NRO
Legacy Project: Survey of Giant Molecular Clouds in M33," Highlights of Astronomy, 1vol.5 :XXVIIth IAU General Assembly, August 2009, ed. Ian F. Corbett, pp.416-416.
As the Nobeyama Radio Observatory Legacy Project: Survey of Giant Molecular Clouds inM33, we have been mapping M33 in CO(1-0) with the multi-beam receiver BEARS equippedon the 45-m telescope using the OTF mapping technique since 2007. The purpose of thisproject is to investigate the physical properties of GMCs and understand the evolutionary
process from GMC formation to star formation in GMCs by comparing with various data suchas CO(3-2), 1.1 mm continuum obtained with ASTE10m telescope at Atacama and the optical
data obtained with SUBARU. We identified 87 GMCs using the first year data of CO(1-0) andobserved 28 GMCs among them in CO(3-2) with ASTE (Onodera 2009, PhD thesis,
University of Tokyo). From the comparison of these lines, it was shown that the

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CO(3-2)/CO(1-0) ratio increases with star forming activity in the GMCs. Furthermore, we
found that more massive GMCs tend to have higher CO(3-2)/CO(1-0) ratio. Since the ratio isthought to be an indicator of the fraction of warm and dense molecular gas, our results imply
that the fraction of warm and dense gas increases with GMC mass. Especially, since the ratio
in the GMCs with low star forming activity is in the range where the ratio depends mainly on
the density, we speculate that dense gas fraction increases with GMC mass.
Kurayama, T. [2008], "VERA Observation of the Massive Star Forming Region G34.4+0.23,"
Proc. of the IAU Symp. 248, "A Giant Step: from Milli- to Micro-arcsecond Astrometry", eds.
Wenjing Jin, Imants Platais, Michael A. C. Perryman, pp.202-203.
We observed with VERA the massive star forming region G34.4+0.23, to obtain parallaxes andproper motions. Four infrared dark clouds were observed and water maser were found in two
dark clouds, MM1 and MM4. In MM1, the distribution of maser spots shows a "V-shaped"
structure and most features co-moving with this structure. Phase-referenced images have peaks
and their motion is much larger than the expected parallax. Further analysis is needed tocorrectly interpret our measurement of parallax.
Kurayama, T. [2009], "VERA Observation of G34.4+0.23 and Matters that Require Attention
for VSOP-2 Phase Referencing," Proc. of the "Approaching Micro-Arcsecond Resolution with
VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and
Murata, Y., ASP Conf. Ser. vol.402, pp.473-475.
We observed the massive star forming region G34.4+0.23 with VERA to determine parallaxes
and proper motions. Four infrared dark clouds were observed and water masers are found fromtwo dark clouds, MM1 and MM4. In MM1, the distribution of the maser spots shows a“V-shape” structure and most features move along this structure. The peaks on the phase(position)-referenced images are detected, but their motions indicate a parallax that is larger
than expected and with a large scatter. The analysis processes should be checked to confirm themeasurement of the parallax.
Kurono, Y., K.-I. Morita, and T. Kamazaki [2009], "A Study of Combining Technique ofSingle-Dish and Interferometer Data: Imaging Simulations and Analysis," Publ. Astron. Soc.
Japan, vol.61, pp.873-894.
We have investigated a technique of combining single-dish data and interferometer data in thespatial frequency domain, using imaging simulations and analytical considerations. Our study
shows that there is an optimum of the relative weights between the visibility data of asingle-dish and an interferometer The quality of the reconstructed combined image achieves
the highest values at relative weights where the mean of the difference between thesynthe-sized beam and the CLEAN beam is close to zero. We also examined the (u,v)-rangethat can be effectively used for the data combining by considering a blurring effect due to apointing error. The error in single-dish deconvolution caused by the beam approximation issmall with a large diameter of the single-dish aperture. The diameter should be at least
1.7-times larger than the minimum baseline of the interferometer for an amplitude accuracy
better than 10%. Furthermore, we derived an estimate of the noise variance in the combined
image, which agrees with our simulation results. The noise-added simulations demonstrate that
there is a threshold of the noise level of the single-dish image, beyond which a large-scaleerror is emphasized in the combined image. We should take observation times to make at least
the same noise level at the border of the spatial frequency between the single-dish and theinterferometer. Although our examinations were assumed to use the 45 m telescope and NMA,
our results concerning the required conditions for observations and data processes can be used
in a general case of heterogeneous array imaging.
Levshakov, S. A., P. Molaro, M. G. Kozlov, A. V. Lapinov, C. Henkel, D. Reimers, T. Sakai,
and I. I. Agafonova [2010], "Search for Chameleon-Like Scalar Fields," JENAM 2010, Joint

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European and National Astronomy Meeting held 6-10 September, 2010 in Lisbon Portugal,
p.68.
Using the 32-m Medicina, 45-m Nobeyama, and 100-m Effelsberg telescopes we found a
statistically significant velocity offset ΔV ≈ 27±3 m s-1 between the inversion transition inNH3(1,1) and low-J rotational transitions in N2H+(1-0) and HC3N(2-1) arising in cold anddense molecular cores in the Milky Way. Systematic shifts of the line centers caused byturbulent motions and velocity gradients, possible non-thermal hyperfine structure populations,pressure and optical depth effects are shown to be lower than or about 1 m s-1 and thus can beneglected in the total error budget. The reproducibility ofΔV at the same facility (Effelsberg
telescope) on a year-to-year basis is found to be very good. Since the frequencies of theinversion and rotational transitions have different sensitivities to variations in μ = me/mp, therevealed non-zeroΔV may imply that mu changes when measured at high (terrestrial) and low(interstellar) matter densities as predicted by chameleon-like scalar field models - candidates tothe dark energy carrier. Thus we are testing whether scalar field models have chameleon-type
interactions with ordinary matter. The measured velocity offset corresponds to the ratio Δμ/μ =(μspace - μlab)/μlab of (26±3)x10-9 (1σ).
Li, J., Z.-Q. Shen, A. Miyazaki, L. Huang, R. J. Sault, M. Miyoshi, M. Tsuboi, and T. Tsutsumi[2009], "The Variability of Sagittarius A* at 3 Millimeter," Astrophys. J., vol.700, pp.417-425.
We have performed monitoring observations of the 3 mm flux density toward the Galactic
center compact radio source Sagittarius A* (Sgr A*) with the Australia Telescope Compact
Array since 2005 October. Careful calibrations of both elevation-dependent andtime-dependent gains have enabled us to establish the variability behavior of Sgr A*. Sgr A*
appeared to undergo a high and stable state in the 2006 June session, and a low and variablestate in the 2006 August session. We report the results, with emphasis on two detected intraday
variation events during its low states. One is on 2006 August 12 when Sgr A* exhibited a 33%
fractional variation in about 2.5 hr. The other is on 2006 August 13 when two peaks separated
by about 4 hr, with a maximum variation of 21% within 2 hr, were seen. The observed shorttimescale variations are discussed in light of two possible scenarios, i.e., the expanding
plasmon model and the sub-Keplerian orbiting hot spot model. The fitting results indicate thatfor the adiabatically expanding plasmon model, the synchrotron cooling cannot be ignored,
and a minimum mass-loss rate of 9.7 × 10–10 M⦿yr–1 is obtained based on parameters derived
for this modified expanding plasmon model. Simultaneous multiwavelength observation is
crucial to our understanding of the physical origin of rapid radio variability in Sgr A*.
Li, J., T. An, Z.-Q. Shen, and A. Miyazaki [2010], "ATCA Observations of SiO Masers in the
Galactic Center," Astrophys. J. (Letters), vol.720, pp.L56-L61.
We present the Australia Telescope Compact Array observations of the SiO masers in the
Galactic center (GC) in transitions of v = 1, J = 2-1 at 86 GHz and v = 1, J = 1-0 at 43 GHz.
Two 86 GHz SiO masers were detected within the central parsec, and they are associated with
IRS 10EE and IRS 15NE, respectively. We detected eighteen 43 GHz SiO masers within aprojected separation of ∼2 pc from Sagittarius A*, among which seven masers are newly
discovered from our observations. This raises the total number of 43 GHz SiO masers within
the central 4 pc of the GC region to 22. Simultaneous observations at 86 and 43 GHz showedthat the intensity of 43 GHz SiO maser is ~3 times higher than that of 86 GHz maser in IRS
10EE (an OH/IR star), while the integrated flux of the SiO maser emission at 43 GHz iscomparable with that at 86 GHz in IRS 15NE (an ordinary Mira variable). These results are
consistent with previous observations of massive late-type stars in the Galaxy in which the 86
GHz SiO maser is in general weaker than the 43 GHz SiO maser in OH/IR stars, while the twotransitions are comparably strong in Mira stars.
Lightfoot, J., G. Kosugi, F. Wyrowski, L. Zapata, D. Muders, F. Boone, T. Tsutsumi, L. Davis,

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C. Wilson, and D. Shepherd [2008], "ALMA Pipeline Heuristics," Proc. of the "Astronomical
data analysis software and systems", eds. Robert W. Argyle, Peter S. Bunclark, and James R.
Lewis, ASP conf. ser., vol.394, p.573.
The ALMA Pipeline Heuristics system is being developed to reduce automatically data takenwith the standard observing modes. The goals are to make ALMA comfortable to use forastronomers who are new to radio interferometry and to provide reduced results of publishable
quality. The reduction sequence will continue to develop as experience is gained at thetelescope, so it is important that the system has a framework and interface that are flexible andeasy to use. Observing modes to be handled include single field interferometry, mosaics, single
dish 'on the fly' maps, and combinations of these. The data will be produced by the main
ALMA array, the Alma Compact Array, and single dish antennas. The reduction sequence islogged to a collection of html files that can examined using a standard browser for verificationof the process. The reduction is performed by a Python script and classes bound to the CASA
libraries.
Lisenfeld, U., D. Espada, S. Leon, L. Lerdes-Montenegro, N. Kuno, and N. Sato [2010],"Molecular Gas Properties in the Most Isolated Galaxies," Proc. of the "Galaxies in Isolation:
Exploring Nature Versus Nurture", eds. Verdes-Montenegro, L., del Olmo, A., Sulentic, J. W.,
ASP Conf. Ser., vol.421, p.262.
We present results obtained from CO(1-0) data of a velocity-restricted subsample of isolated
galaxies from the AMIGA project.
Liszt, H. S., J. Pety, and K. Tachihara [2009], "Imaging Galactic Diffuse Clouds: CO Emission,
Reddening and Turbulent Flow in the Gas aroundζOph,Astron. " Astrophys., vol.499,
pp.503-513.
Context. Most diffuse clouds are only known as kinematic features in absorption spectra, but
those with appreciable H2 content may be visible in the emission of such small molecules as
CH, OH, and CO.
Aims. We interpret in greater detail the extensive observations of 12CO emission from diffuse
gas seen around the archetypical line of sight toζOph.
Methods. The 12CO emission is imaged in position and position-velocity space, analyzed
statistically, and then compared with maps of total reddening E∞B-V and with models of the C+- CO transition in H2-bearing diffuse clouds.
Results. AroundζOph, 12CO emission appears in two distinct intervals of reddening centerednear E∞B-V ≈ 0.4 and 0.65 mag, of which ∼0.2 mag is background material. Within either
interval, the integrated 12CO intensity varies up to 6-12 K km s-1, compared to 1.5 K km s-1
toward ζOph. Nearly 80% of the individual profiles have velocity dispersionsσv < 0.6 km s-1,
which are subsonic at the kinetic temperature derived from H2 towardζOph, 55 K. Partly as aresult, 12CO emission exposes the internal, turbulent, supersonic (1-3 km s-1) gas flows withespecial clarity in the cores of strong lines. The flows are manifested as resolved velocity
gradients in narrow, subsonically-broadened line cores.
Conclusions. The scatter between N(CO) and EB-V in global, CO absorption line surveys
toward bright stars is present in the gas seen aroundζOph, reflecting the extreme sensitivity ofN(12CO) to ambient conditions. The two-component nature of the optical absorption
towardζOph is coincidental and the star is occulted by a single body of gas with a complex
internal structure, not by two distinct clouds. The very bright 12CO lines in diffuse gas arise atN(H2) ≈ 1021 cm-2 in regions of modest density n(H) ≈ 200-500 cm-3 and somewhat more
complete C+-CO conversion. Given the variety of structure in the foreground gas, it is apparent
that only large surveys of absorption sightlines can hope to capture the intrinsic behavior of
diffuse gas.
Liu, G., D. Calzetti, M. S. Yun, G. W. Wilson, B. T. Draine, K. Scott, J. Austermann, T. Perera,

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D. Hughes, I. Aretxaga, K. Kohno, R. Kawabe, and H. Ezawa [2010a], "From Near-Infrared toMillimeter: An Investigation of the Content in the NGC 1512/1510 Pair," American Astron.
Soc., AAS Meeting #215, #432.18.
We combine new ASTE/AzTEC 1.1 mm maps of the galaxy pair NGC1512/1510 with archival
Spitzer IRAC and MIPS images covering the wavelength range 3.6-160μm from the SINGS
project. The two galaxies form a high-metallicity, large spiral (NGC1512)/low-metallicity
compact dwarf (NGC1510) pair. Using the models of Draine & Li (2007), the derived total
dust masses are (2.4±0.6)×107 and (1.7±3.6)×105 Msun for NGC1512 and NGC1510,
respectively. The derived dust/H I ratio is within expectations of low-metallicity galaxies for
NGC1510, but it is much lower, by at least a factor of 3, than expected for NGC1512, aspreviously found by Draine et al. (2007). In contrast, regions within NGC1512, specifically thecentral region and the arms, do not show such unusually low dust/H I values, suggesting thepossibility that some of the H I included in the determination of the dust/H I ratio of NGC1512
is not associated with the star forming disk. Simple two-temperature modified-blackbody fits
to the far-infrared/mm data of the two galaxies and the sub-regions of NGC1512 are also
performed to derive the dust masses associated with warm and cool dust components. As
generally expected, the warm dust temperature of the low-metallicity, low-mass NGC1510(~36 K) is substantially higher than the corresponding warm temperature of thehigh-metallicity spiral NGC1512 (~24 K). In both galaxies, our fits indicate that a substantial
fraction (>93%) of the total dust mass is in a cool dust component (~14-16 K for NGC1512
and ~15-24 K for NGC1510). This result is similar to what is determined for a few othernearby galaxies. The warm dust component in the sub-galactic regions of NGC1512 represents
a much larger fraction of the total dust content (17-40%), in agreement with the fact that all
three regions have higher specific star formation rates than the average in the galaxy.
Liu, G., D. Calzetti, M. S. Yun, G. W. Wilson, B. T. Draine, K. Scott, J. Austerman, T. Perera,
D. Hughes, I. Aretxaga, K. Kohno, R. Kawabe, and H. Ezawa [2010b], "An Investigation of
the Dust Content in the Galaxy Pair NGC 1512/1510 from Near-Infrared to Millimeter
Wavelengths," Astron. J., vol.139, pp.1190-1198.
We combine new ASTE/AzTEC 1.1 mm maps of the galaxy pair NGC 1512/1510 witharchival Spitzer IRAC and MIPS images covering the wavelength range 3.6-160μm from the
SINGS project. The availability of the 1.1 mm map enables us to measure the long-wavelength
tail of the dust emission in each galaxy, and in sub-galactic regions in NGC 1512, and to derive
accurate dust masses. The two galaxies form a pair consisting of a large, high-metallicity spiral(NGC 1512) and a low-metallicity, blue compact dwarf (NGC 1510), which we use to compare
similarities and contrast differences. Using the models of Draine and Li, the derived total dust
masses are (2.4 ± 0.6) ×107 Msun and (1.7 ± 3.6) × 105 Msun for NGC 1512 and NGC 1510,
respectively. The derived ratio of dust mass to H I gas mass for the galaxy pair, Md/MHI~0.0034, is much lower (by at least a factor of 3) than expected, as previously found by Draine
et al. In contrast, regions within NGC 1512, specifically the central region and the arms, do notshow such unusually low Md/MHI ratios; furthermore, the dust-to-gas ratio is within
expectations for NGC 1510. These results suggest that a fraction of the HI included in thedetermination of the Md/MHI ratio of the NGC 1512/NGC 1510 pair is not associated with thestar-forming disks/regions of either galaxy. Using the dust masses derived from the models ofDraine & Li as references, we perform simple two-temperature modified blackbody fits to the
far-infrared/millimeter data of the two galaxies and the sub-regions of NGC 1512, in order toderive and compare the dust masses associated with warm and cool dust temperaturecomponents. As generally expected, the warm dust temperature of the low-metallicity,
low-mass NGC 1510 (Tw ~ 36 K) is substantially higher than the corresponding warm
temperature of the high-metallicity spiral NGC 1512 (Tw ~ 24 K). In both galaxies (albeit with

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a large uncertainty for NGC 1510), our fits indicate that a substantial fraction (>93%) of thetotal dust mass is in a cool dust component, with temperatures ~14-16 K for NGC 1512 and~15-24 K for NGC 1510. This result is similar to what is determined for a few other nearby
galaxies. In contrast, the warm dust component in the sub-galactic regions of NGC 1512
represents a much larger fraction of the total dust content, in agreement with the fact that all
three regions have higher specific star formation rates than the average in the galaxy; in thecenter, the warm dust represents about 40% of the total, while in the arms the fractions areclose to ~20%.
Liu, Q., X. Shi, F. Kikuchi, Q. Huang, S. Kamata, K. Matsumoto, H. Hanada, X. Hong, A. Yu,
J. Ping, Q. Fan, B. Xia, T. An, Z. Qian, W. Yang, H. Zhang, Z. Wang, and N. Wang, [2009],"High-Accuracy Same-Beam VLBI Observations using Shanghai and Urumqi Telescope,"
Science in China Ser. G: Phys. Mathe. & Astron., vol.52, pp.1858-1866.
The same-beam VLBI observations of Rstar and Vstar, which were two small satellites ofJapanese lunar mission, SELENE, were successfully performed by using Shanghai and Urumqi
25-m telescopes. When the separation angle between Rstar and Vstar was less than 0.1 deg, thedifferential phase delay of the X-band signals between Rstar and Vstar on Shanghai-Urumqi
baseline was obtained with a very small error of 0.15 mm rms, which was reduced by 1-2 ordercompared with the former VLBI results. When the separation angle was less than 0.56 deg, thedifferential phase delay of the S-band signals was also obtained with a very small error ofseveral mm rms. The orbit determination for Rstar and Vstar was performed, and the accuracy
was improved to a level of several meters by using VLBI and Doppler data. The high-accuracy
same-beam differential VLBI technique is very useful in orbit determination for a spacecraft,
and will be used in orbit determination for Mars missions of China Yinghuo-1 and Russia
Phobos-grunt.
Liu, Q., F. Kukuchi, K. Matsumoto, S. Goossens, H. Hanada, Y. Harada, X. Shi, Q. Huang, T.
Ishikawa, S. Tsuruta, K. Asari, Y. Ishihara, N. Kawano, S. Kamata, T. Iwata, H. Noda, N.
Namiki, S. Sasaki, S. Elingsen, K. Sato, K. Shibata, Y. Tamura, T. Jike, K. Iwadate, O. Kameya,
J. Ping, B. Xia, T. An, Q. Fan, X. Hong, W. Yang, H. Zhang, Y. Aili, B. Reid, W. Hankey, J.
McCallum, G. Kronschnabl, and W. Schluter [2010], "Same-Beam VLBI Observations of
SELENE for Improving Lunar Gravity Field Model," Radio Sci., 45, CitelID RS2004(1-16).
The Japanese lunar mission, Selenological and Engineering Explorer (Kaguya), which was
successfully launched on 14 September 2007, consists of a main satellite and two small
satellites, Rstar and Vstar. Same-beam very long baseline interferometry (VLBI) observationsof Rstar and Vstar were performed for 15.4 months from November 2007 to February 2009
using eight VLBI stations. In 2008, S band same-beam VLBI observations totaling 476 h on
179 days were undertaken. The differential phase delays were successfully estimated for most(about 85%) of the same-beam VLBI observation periods. The high success rate was mainly
due to the continuous data series measuring the differential correlation phase between Rstar
and Vstar. The intrinsic measurement error in the differential phase delay was less than 1 mm
RMS for small separation angles and increased to approximately 2.5 mm RMS for the largest
separation angles (up to 0.56 deg). The long-term atmospheric and ionospheric delays along
the line of sight were reduced to a low level (several tens of milimeters) using the same-beam
VLBI observations, and further improved through application of GPS techniques. Combining
the eight-station (four Japanese telescopes of VLBI Exploration of Radio Astrometry and fourinternational telescopes) S band same-beam VLBI data with Doppler and range data, theaccuracy of the orbit determination was improved from a level of several tens of meters when
only using Doppler and range data to a level of 10 m. As a preliminary test of the technique,the coefficient sigma degree variance of the lunar gravity field was compared with and without
4 months of VLBI data included. A significant reduction below around 10 deg (especially for

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the second degree) was observed when the VLBI data were included. These observations
confirm that the VLBI data contribute to improvements in the accuracy of the orbit
determination and through this to the lunar gravity field model.
Maeda, T., H. Imai, T. Omodaka, H. Kobayashi, K. M. Shibata, T. Bushimata, Y. K. Choi, T.
Hirota, M. Honma, K. Horiai, N. Inomata, K. Iwadate, T. Jike, S. Kameno, O. Kameya, R.
Kamohara, Y. Kan-ya, N. Kawaguchi, S. Kuji, T. Kurayama, S. Manabe, T. Miyaji, T.
Nagayama, A. Nakagawa, K. Nakashima, C. S. Oh, T. Oyama, S. Sakai, S. Sakakibara, K. Sato,R. Shimizu, M. Shintani, K. Sora, H. Suda, Y. Tamura, and K. Yamashita [2008], "A Bipolar
Outflow of the M-Type Giant IRC 10414 Traced by H2O Maser Emission," Publ. Astron. Soc.
Japan, vol.60, pp.1057-1067.
We report on results of five-epoch VLBI observations of H2O maser emission in the M-typestar IRC - 10414, carried out with the VLBI Exploration of Radio Astrometry (VERA). The
maser distribution extends over an area of 70 mas x 260 mas and exhibits a bipolar structure.
The relative proper motions of 17 maser features were measured during the monitoring
observations spanning nine months. The distance to IRC - 10414 was re-estimated on the basisof the statistical treatment of parallax and the model-fitting method, yielding D = 3.1±0.4 kpc
and D = 2.0±0.2 kpc, respectively. The estimated distance, D = 2-3 kpc, is much larger thanthat previously adopted. The stellar luminosity of IRC - 10414 is also re-estimated to be L* ~ 9x 104 (D/2 kpc)2 L , much brighter by a factor of 10-20 than previously adopted (L* ~ 10000
L ). The maser motions exhibit not only a spherically expanding flow with a velocity of ~10(D/2 kpc) km s-1, but also a faster bipolar outflow with a major axis in the north-south
direction and at a small inclination angle with respect to the celestial sphere. These
characteristics of the star and the circumstellar envelope seen in IRC - 10414 are very similar
to those in some supergiants exhibiting bipolar stellar mass loss.
Mamyoda, K., N. Nakai, A. Yamauchi, P. Diamond, and J.-M. Huré [2009], "Detection of a
Sub-Keplerian Water Maser Disk at the Active Galactic Nuclear of the Galaxy IC 481," Publ.
Astron. Soc. Japan, vol.61, pp.1143-1151.
We present a study of H2O maser emission from the LINER, IC 1481, based on single-dish andhighly sensitive VLBI observations. The Nobeyama 45-m telescope detected new maser
features near the systemic velocity and blue-shifted by 124-205 km s-1. In addition, the known
features red-shifted by ≈97-155 km s-1 were monitored. VLBI observations with the HighSensitivity Array (HSA) revealed that the maser features are distributed along a line, with avelocity gradient, strongly suggesting a nearly edge-on molecular gas disk. The radius andthickness of the disk are r = 2.8-14.0 pc and 2H = 1.5-4.2 pc, respectively, which are thelargest among the maser disks detected in active galactic nuclei. The disk is rotating at Vrot =124-168 km s-1, having a large velocity dispersion of ∆V≈31 km s-1. The rotation curve of thedisk is sub-Keplerian (Vrot ∼ r-0.19±0.04), indicating a massive disk. The disk mass is estimatedto be (4.3±0.3) ×107 M⦿and the mass of a putative central black hole is <107 M⦿. The massive
disk is gravitationally unstable. A radio continuum source was also detected to be offset fromthe maser disk by 1.6 pc.
Marsher, A., S. Jorstad, D. Murphy, D. Meier, R. Preston, S. Unwin, K. Kellermann, J. Wrobel,
J. Romney, D. Homan, M. Lister, G. Piner, L. Greenhill, M. Reid, G. Taylor, A. Weshrle, D.
Roberts, A. Readhead, M. Böttcher, M. Georganopoulos, S. Bloom, K. Johnston, C. C. Cheung,
T. Krichbaum, M. Tsuboi, M. Inoue, and S. Kameno [2009], "Exploring the Most Compact
Regions of Relativistic Jets with the Ultra-High Angular Resolution of Space VLBI,"
Astro2010: The Astronomy and Astrophysics Decadal Survey, Science White Papers, no.
193-1-8.
Without abstract
Maruta, H., F. Nakamura, R. Nishi, N. Ikeda, and Y. Kitamura [2010], "Physical Properties of

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Dense Cores in the Ophiuchi Main Cloud and A Signiﬁcant Role of External Pressures in
Clustered Star Formation," Astrophys. J., vol.714, pp.680-698.
Using the archive data of the H13CO+ (J = 1-0) line emission taken with the Nobeyama 45 mradio telescope with a spatial resolution of ~ 0.01 pc, we have identified 68 dense cores in thecentral dense region of theρOphiuchi main cloud. The H13CO+ data also indicate that thefractional abundance of H13CO+ relative to H2 is roughly inversely proportional to the squareroot of the H2 column density with a mean of 1.72 ×10-11. The mean radius, FWHM line width,and LTE mass of the identified cores are estimated to be 0.045 ± 0.011 pc, 0.49 ± 0.14 km s-1,
and 3.4 ± 3.6 M sun, respectively. The majority of the identified cores have subsonic internalmotions. The virial ratio, the ratio of the virial mass to the LTE mass, tends to decrease withincreasing LTE mass and about 60% of the cores have virial ratios smaller than 2, indicatingthat these cores are not transient structures but self-gravitating. The detailed virial analysis
suggests that the surface pressure often dominates over the self-gravity and thus plays a crucialrole in regulating core formation and evolution. By comparing theρOph cores with those in theOrion A molecular cloud observed with the same telescope, we found that the statisticalproperties of the core physical quantities are similar between the two clouds if the effect of thedifferent spatial resolutions is corrected. The line widths of theρOph cores appear to be nearly
independent of the core radii over the range of 0.01-0.1 pc and deviate upward from the Heyer& Brunt relation. This may be evidence that turbulent motions are driven by protostellar
outflows in the cluster environment.
Matsumoto, K., S. Goossens, Q. Liu, T. Iwata, N. Namiki, H. Noda, H. Hanada, F. Kikuchi, Y.
Ishihara, N. Kawano, S. Tsuruta, K. Asari, T. Ishikawa, and S. Sasaki [2008a], "Current Statusof Acquisition and Processing of Tracking Data from SELENE (Kaguya) Satellites for Lunar
Gravity Field Estimation," 39th Lunar and Planetary Science Conference, (Lunar andPlanetary Science XXXIX), held March 10-14, 2008 in League City, Texas. LPI Contribution
No. 1391, p.1541.
This presentation summarizes the current status of acquisition and processing of tracking datafrom Kaguya. A special emphasis will be on the four-way Doppler data coverage over the
lunar far-side and its impact on lunar gravity field estimation.
Matsumoto, K., H. Hanada, N. Namiki, T. Iwata,S. Goossens, S. Tsuruta, N. Kawano, and D. D.
Rowlands [2008b], "A Simulation Study for Anticipated Accuracy of Lunar Gravity Field
Model by SELENE Tracking Data," Adv. Sp. Res., vol.42, pp.331-336.
Results of numerical simulations are presented to examine the global gravity field recovery
capability of the Japanese lunar exploration project SELENE (SELenological and ENgineering
Explorer) which will be launched in 2007. New characteristics of the SELENE lunar
gravimetry include 4-way satellite-to-satellite Doppler tracking of main orbiter and differential
VLBI tracking of two small free-flier satellites. It is shown that the proposed satellite
constellation will provide the first truly global satellite tracking data coverage. The expected
results from these data are; (1) drastic reduction in far-side gravity error, (2) estimation ofmany gravity coefficients by the observation, not by a priori information, and (3) one order ofmagnitude improvement over existing gravity models for low-degree field.
Matsumoto, K., S. Goossens, Y. Ishihara, Q. Liu, T. Iwata, N. Namiki, H. Noda, H. Hanada, F.
Kikuchi, N. Kawano, S. Tsuruta, K. Asari, T. Ishikawa, and S. Sasaki [2008c], "Initial Resultsof Global Lunar Gravity Field Recovery from SELENE Tracking Data," 37th COSPAR
Scientific Assembly, held 13-20 July 2008, in Montreal, Canada, p.1953.
Two small spin-stabilized sub-satellites, Rstar (OKINA) and Vstar (OUNA), have successfully
been separated from Main satellite of SELENE (KAGUYA) and inserted into planned ellipticalorbits on October 9 and 12, 2007, respectively. These spacecraft are dedicated to improving
our knowledge of the global lunar gravity field with the mission instruments on-board, i.e.,

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RSAT (a satellite-to-satellite Doppler tracking sub-system) and VRAD (artificial radio sources
for VLBI). We have started collecting new types of tracking data for the lunar-orbiting
satellites, i.e., 4-way Doppler tracking between the Main satellite and Rstar (i.e., a direct
far-side gravity observation), and multi-frequency differential VLBI tracking between Rstar
and Vstar. A global lunar gravity field with unprecedented accuracy is expected to be estimatedthrough precision orbit determination by using these tracking data. A preliminary global lunar
gravity field model (degree and order up to 60) was developed from about 3-month of
SELENE tracking data which include 2-way Doppler, 2-way range, and 4-way Doppler data.
Although the current far-side data coverage is incomplete and a Kaula-type a priori constraint
is necessary for meaningful inversion, some of ring-shaped gravity anomalies are more clearly
resolved in the far-side compared with existing lunar gravity models. We will present conceptof tracking data acquisition scheduling, current status of tracking data acquisition, andpreliminary results of global lunar gravity filed recovery.
Matsumoto, K., S. Goossens, Y. Ishihara, Q. Liu, F. Kikuchi, T. Iwata, H. Noda, H. Hanada, N.
Kawano, F. G. Lemoine, and D. D. Rowlands [2010], "An Improved Lunar Gravity Field
Model from SELENE and Historical Tracking Data: Revealing the Farside Gravity Features,J" .
Geophys. Res., vol.115, pp.E06007(1-20).
A new spherical harmonic solution of the lunar gravity field to degree and order 100, called
SGM100h, has been developed using historical tracking data and 14.2 months of SELENE
tracking data (from 20 October 2007 to 26 December 2008 plus 30 January 2009). The latterincludes all usable 4-way Doppler data collected which allowed direct observations of thefarside gravity field for the first time. The new model successfully reveals farside features infree-air gravity anomalies which are characterized by ring-shaped structures for large impact
basins and negative spots for large craters. SGM100h produces a correlation with
SELENE-derived topography as high as about 0.9, through degree 70. Comparison between
SGM100h and LP100K (one of the pre-SELENE models) shows that the large gravity errors
which existed in LP100K are drastically reduced and the asymmetric error distribution
between the nearside and the farside almost disappears. The gravity anomaly errors predictedfrom the error covariance, through degree and order 100, are 26 mGal and 35 mGal for thenearside and the farside, respectively. Owing to the 4-way Doppler measurements the gravity
coefficients below degree and order 70 are now determined by real observations with
contribution factors larger than 80 percent. With the SELENE farside data coverage, it ispossible to estimate the gravity field to degree and order 70 without applying any a priori
constraint or regularization. SGM100h can be used for global geophysical interpretation
through degree and order 70.
Matsumoto, N., T. Omodaka, H. Imai, R. Shimizu, T. Bushimata, Y. K. Choi, T. Hirota, M.
Honma, N. Inomata, K. Iwadate, T. Jike, S. Kameno, O. Kameya, R. Kamohara, Y. Kan-ya, N.
Kawaguchi, H. Kobayashi, S. Kuji, T. Kurayama, T. Maeda, S. Manabe, T. Miyaji, A.
Nakagawa, T. Nagayama, K. Nakashima, K., C. S. Oh, T. Oyama, S. Sakai, S. Sakakibara, T.
Sasao, K. Sato, K. M. Shibata, M. Shintani, Y. Sofue, K. Sora, H. Suda, Y. Tamura, M.
Tsushima, and K. Yamashita [2008], "Variable Asymmetry of the Circumstellar Envelope in IK
Tauri Traced by SiO Maser Emission," Publ. Astron. Soc. Japan, vol.60, pp.1039-1050.
We observed the SiO (ν=1 andν=2, J=1-0) maser emissions toward the Mira variable IK Tauri(IK Tau, NML Tau, IRC+10050) over nine epochs from 2002 November to 2005 April using
the VLBI Exploration of Radio Astrometry (VERA) telescope array. We found that the SiO
maser distributions around IK Tau are highly variable, depending on the stellar pulsation phase.
The velocity structures were complex and also time-variable, and are inconsistent with asimply rotating shell that was suggested by previous observations. Based on fittings of the SiO
maser distributions to elliptical ring models, we found that the ring size seems to vary in

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correlation with the pulsation phase, as previously found for TX Cam. Comparisons of theν=1
andν=2 maser distributions reveal that 42-50% of the maser pairs have a positional offset lessthan 0.5 mas, suggesting that the maser pumping in these spots is likely to be dominated byline overlapping or collisional pumping, rather than pure radiative pumping. In order to model
the velocity structure of the spoke-like features observed in IK Tau, we propose aballistic-orbit model, in which a gas clump ejected from the stellar surface moves radiallyoutward with a gravitational deceleration, and argue that the stellar mass can be deduced fromthat model.
Matsushita, S., A. L. Tsai, R. Kawabe, K. Nakanishi, B. Vola-Vilaro, K. Kohno, T. Inui, H.
Matsumoto, T. G. Tsuru, and A. B. Peck [2008], "Molecular Bubbles and Outflows in the
Edge-on Starburst Galaxies M82 and NGC 2146," Proc. of the "Mapping the Galaxy and
Nearby Galaxies", eds. Wada, K., and Combes, F., p.352.
Without abstract
Matsushita, S., R. Kawabe, K. Kohno, T. Tosaki, and B. Vila-Vilaro [2010], "Dense and Warm
Molecular Gas and Warm Dust in Nearby Galaxies," Publ. Astron. Soc. Japan, vol.62,
pp.409-421.
We performed 12CO(1-0), 13CO(1-0), and HCN(1-0) single-dish observations (beam size ~14"-18") toward nearby starburst and non-starburst galaxies using the Nobeyama 45 m telescope.
The 13CO(1-0) and HCN(1-0) emissions were detected from all the seven starburst galaxies,
with the intensities of both lines being similar (i.e., the ratios are around unity). On the other
hand, for case of the non-starburst galaxies, the 13CO(1-0) emission was detected from all threegalaxies, while the HCN(1-0) emission was weakly or not detected in past observations. This
result indicates that the HCN/13CO intensity ratios are significantly larger (~1.15±0.32) in the
starburst galaxy samples than the non-starburst galaxy samples (< 0.31 ± 0.14). The
large-velocity-gradient model suggests that the molecular gas in the starburst galaxies havewarmer and denser conditions than that in the non-starburst galaxies, and thephoton-dominated-region model suggests that the denser molecular gas is irradiated bystronger interstellar radiation field in the starburst galaxies than that in the non-starburst
galaxies. In addition, HCN/13CO in our sample galaxies exhibit strong correlations with the
IRAS 25μm flux ratios. It is a well established fact that there exists a strong correlation
between dense molecular gas and star formation activities, but our results suggest thatmolecular gas temperature is also an important parameter.
Migita, E., H. Araki, H. Noda, S. Tazawa, Y. Ishihara, and T. Iwata [2009], "Laser Altimeter
Lunar Crater Measurement by SELENE (Kaguya)," 40th Lunar and Planetary Science
Conference, (Lunar and Planetary Science XL), held March 23-27, 2009 in The Woodlands,
Texas, id.1981.
Laser Altimeter (LALT) on board SELENE (Kaguya) can determine anew crater diameter.
LALT data is accurate as compared with Clementine LIDAR data. Especially, central peaks
seen in LALT data are clearer than those seen in LIDAR data.
Minamidani, T., N. Mizuno, Y. Mizuno, A. Kawamura, T. Onishi, T. Hasegawa, K. Tatematsu,
M. Ikeda, Y. Moriguchi, N. Yamaguchi, J. Ott, T. Wong, E. Muller, J. L. Pineda, A. Hughes, L.
Staveley-Smith, U. Klein, A. Mizuno, S. Nikolic, R. S. Booth, A. Heikkila, L. A. Nyman, M.
Lerner, G. Garay, S. Kim, M. Rubio, and Y. Fukui [2008a], "An Observational Study of the
GMCs in the Magellanic Clouds in Millimeter and Submillimeter Wavelengths," Proc. of the"Galaxies in the Local Volume", eds. B. S. Koribalski and H. Jerjen, Astrophys. Sp. Sci. Proc.,
pp.311-312.
Not Available
Minamidani, T., N. Mizuno, Y. Mizuno, A. Kawamura, T. Onishi, T. Hasegawa, K. Tatematsu,
M. Ikeda, Y. Moriguchi, N. Yamaguchi, J. Ott, T. Wong, E. Muller, J. L. Pineda, A. Hughes, L.

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Staveley-Smith, U. Klein, A. Mizuno, S. Nikolic, R. S. Booth, A. Heikkilä, L.-A. Nyman, M.
Lerner, G. Garay, S. Kim, M. Fujishita, T. Kawase, M. Rubio, and Y. Fukui, ]2008b],"Sub-millimeter Observations of Giant Molecular Clouds in the Large Magellanic Cloud:Temperature and Density as Determined from J=3-2 and J=1-0 transitions of CO," Astrophys. J.
Suppl. Ser., vol.175, pp.485-508.
We have carried out submillimeter 12CO(J=3-2) observations of six giant molecular clouds(GMCs) in the Large Magellanic Cloud (LMC) with the ASTE 10 m submillimeter telescopeat a spatial resolution of 5 pc and very high sensitivity. We have identified 32 molecular
clumps in the GMCs and revealed significant details of the warm and dense molecular gas withn(H2)~103-105 cm-3 and K. These data are combined with 12CO(J=1-0) and 13CO(J=1-0) results
and compared with LVG calculations. The results indicate that clumps that we detected are
distributed continuously from cool (~10-30 K) to warm ( 30-200 K), and warm clumps are
distributed from less dense (103 cm−3) to dense (103.5-105 cm-3). We found that the ratio of
12
CO(J=3-2) to 12CO(J=1-0) emission is sensitive to and is well correlated with the local Hαflux. We infer that differences of clump properties represent an evolutionary sequence of
GMCs in terms of density increase leading to star formation. Type I and II GMCs (starless
GMCs and GMCs with Hii regions only, respectively) are at the young phase of star formation
where density does not yet become high enough to show active star formation, and Type III
GMCs (GMCs with Hii regions and young star clusters) represent the later phase where theaverage density is increased and the GMCs are forming massive stars. The high kinetic
temperature correlated with Hα flux suggests that FUV heating is dominant in the moleculargas of the LMC.
Minamidani, T., N. Mizuno, Y. Mizuno, A. Kawamura, T. Onishi, K. Tatematsu, T. Hasegawa,
M. Ikeda, and Y. Fukui [2009], "An Observational Study of GMCs in the Magellanic Clouds
with the ASTE Telescope," Proc. of the IAU Symp. 256, "The Magellanic System: Stars, Gas,
and Galaxies", eds. Van Loon. Borin, Joana M. Oliveira, pp.256-260.
We report the results of the submillimeter observations with the ASTE 10 m telescope toward
the giant molecular clouds (GMCs) in the Magellanic Clouds to reveal the physical propertiesof dense molecular gas, the principle sites of star and cluster formation. Six GMCs in the
Large Magellanic Cloud have been mapped in the 12CO(J = 3-2) transition and 32 clumps are
identified in these GMCs at a resolution of 5 pc. These data are combined with 12CO(J = 1-0)
and 13CO(J = 1-0) results and compared with LVG calculations to derive the density andtemperature of clumps. The derived density and temperature are distributed in wide ranges. We
have made small mapping observations in the 13CO(J = 3-2) transition toward 9 representative
peak positions of clumps to determine the density and temperature of clumps. These physicalproperties are constrained well and there are differences in density and temperature among
clumps. We suggest that these differences of clump properties represent an evolutionary
sequence of GMCs in terms of density increase leading to star formation.
Miura, R., Y. Tamura, S. K. Okumura, R. Kawabe, T. Tosaki, N. Kuno, K. Nakanishi, S.
Sakamoto, and T. Hasegawa [2008], "Dense Clouds and Star Formation on Spiral Arm in M33-deep CO and HCN Observation in NGC604-," Proc. of the "Mapping the Galaxy and Nearby
Galaxies", eds. Wada, K., and Combes, F., p.354.
Without abstract
Miyawaki, R., M. Hayashi, and T. Hasegawa [2009], "A Large-Scale 13CO Mapping of the
W49A molecular Cloud Complex," Publ. Astron. Soc. Japan, vol.61, pp.39-49.
We present 13CO (J = 1-0) and C18O (J = 1-0) maps of the W 49 A molecular cloud complex
observed at a resolution of 1700 (HPBW). Fourteen features (MHH-1 to MHH-14) wereidentiﬁed in the 13CO velocity channel maps, most of them distributed within an area of 60 (20pc) in diameter with their total mass amounting to 1.7x 106 M ⦿. The features have a

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three-dimensional velocity dispersion of 8 km s-1, which leads to a mean free time per featureof 106 yr. This suggests that they are interacting one another in a region of ~20 pc in diameter.
The feature MHH-1, which corresponds to W 49 N, is unique in that it exhibits a large velocity
width (15 km s-1 FWHM) and is compact in size (2.3 pc x 3.0 pc FWHM), while containing alarge mass of 2.4 x105 M⦿. This indicates that the free-fall time of MHH-1 is on the order of
105 yr, an order of magnitude smaller than that of the entire complex. It has turned out thatMHH-1 has a smaller spatial width at VLSR ∼ 8 km s-1 than at ∼ 8 km s-1. This result, together
with the line-pro ﾞ le characteristics of various optically thin lines, suggests that at least two
massive clouds with different radial velocities exist toward MHH-1. The massive compact
feature may have been produced by the interaction of the two different velocity clouds.
Miyazaki, A., Z.-Q. Shen, M. Miyoshi, M. Tsuboi, and T. Tsutsumi [2008], "Flux variability of
Sgr A* at Short Millimeter Wavelengths," Proc. of the "Mapping the Galaxy and Nearby
Galaxies", eds. Wada, K., and Combes, F., p.355.
Without abstract
Miyazaki, A., Z.-Q. Shen, J. Li, M. Miyoshi, M. Tsuboi, and T. Tsutsumi [2009], "Flux
Variability of Sagittarius A* at Short mm-wavelengths," Proc. of the "Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara,
Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.376-379.
We performed the monitoring observations of the flux density toward Sgr A*, which is acompact radio source associated with a super-massive black hole located at the dynamical
center of the Galaxy, using the Nobeyama Millimeter Array (NMA) and the Australia
Telescope Compact Array (ATCA) at mm-wavelengths. Since 1996, the flux monitoring
observations using the NMA were carried out in the 3- and 2-mm bands. Then we detected
several flares of Sgr A* with typical durations of a few weeks. We also found some intraday
variations (IDVs) of Sgr A* in both observing bands. The 3-mm flux observations of Sgr A*
using the ATCA in the southern hemisphere were also carried out to detect IDVs with a longer
observing window. In the ATCA observations, we detected IDVs of Sgr A* with timescale of afew hour. In these IDVs, the short flux-doubling timescale was estimated to be a few hours,
constraining the physical size of flare-emitting region within about a few tens of AU.
Miyoshi, M., S. Kameno, J. K. Ishitsuka, Z.-Q. Shen, R. Takahashi, and S. Horiuchi [2007],"An Approach Detecting the Event Horizon of Sgr A*," Publ. Natl. Obs. Japan, vol.10,
pp.15-23.
Imaging the vicinity of a black hole is one of the ultimate goals of VLBI astronomy. The
closest massive black hole, Sgr A*, located at the Galactic center, is the leading candidate forsuch observations. Combined with recent VLBI recording technique and submillimeter radio
engineering, we now have sufficient sensitivity for the observations. Here we show
performance simulations simulations of submilllimeter VLBI arrays for imaging Sgr A*. Good
images are obtained from submillimeter VLBI arrays in the southern hemisphere composed ofmore than 10 stations. We also note that even with a small array, we can estimate the shadow
size and then the mass of the black hole from visibility analysis. Now, all we need is toconstruct a submillimeter VLBI array in the southern hemisphere if we wish unveil the blackhole environment of Agr A*.
Miyoshi, M. [2008], "Slit-Modulation Imaging Method for Detecting Any Periodic Structure
Change in Interferometric Data," Publ. Astron. Soc. Japan, vol.60, pp.1371-1386.
We propose a slit-modulation imaging (SMI) method, a new imaging technique for detecting
shorter periodic structural changes of interferometric data. Using simulations with artiﬁcial
visibility data, we show that the SMI method is highly effective in detecting periodic change
patterns, of which period is shorter than the observing time span, of interferometric data.
Miyoshi, M. [2009a], "Re-Analysis of the First Fringe with 2-Beam in the VERA System from

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the Archive Data," Publ. Natl. Astron. Obs. Japan, vol.12, pp.1-9.
We report results from re-analysis of the visibility data of the first 2-beam observations with
VERA (VLBI Exploration of Radio Astrometry), previously reported by Honma et al., 2003
(hereafter A2003). Independently we checked the archival data and found the features noted in
A2003 were not from the effect of phase referencing by simultaneous differential VLBI but
mainly from a removal of large phase change by subtracting an arbitrary fitted curve to thephase variations. The differential phase of the observed H2O masers between W49 North(W49N) and OH~43.8-0.1 did not show a sinusoidal variation with a period of one sidereal
day due to a positional offset from the real celestial positions. We therefore could not
reproduce the results in A2003 by a normal positional correction estimated from all time data,
but could reproduce almost the same phases only for the first hour by adjusting parameters.
Using the parameters, we could not suppress the large amount of phase variations for the
successive time data that A2003 did not show in their paper. It is appropriate to regard theanalysis in A2003 as not being proper for showing the performance of the instrument for phasereferencing, which should be demonstrated by other experiments observing several pairs ofcontinuum sources.
Miyoshi, M., S. Kameno, J. K. Ishitsuka, Z.-Q. Shen, R. Takahashi, and S. Horiuchi [2009b],"An Approach to Detect the Event Horizon in SgrA* Using Ground Based Submillimeter
VLBI Array," Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2:
Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y.,
ASP Conf. Ser. vol.402, pp.380-383.
We present here ground-based array simulations for detecting the black hole shadow in Sgr A*.
With modest super resolutions, it is easy to obtain the detection and imaging the black holeshadow. Also it is noteworthy that the visibilities from short baselines ranging from 1000 to2000 km are quite important to the detection. Miyoshi et al. (2007) show the details.
Mizuno, N. [2009], "The Properties of Molecular Clouds Across the Magellanic System," Proc.
of the IAU Symp. 256, "The Magellanic System: Stars, Gas, and Galaxies", eds. Van Loon.
Borin, Joana M. Oliveira, pp.203-214.
Most stars form in Giant Molecular Clouds (GMCs) and regulate the evolution of galaxies invarious respects. The formed stars affect the surrounding materials strongly via their UVphotons, stellar winds, and supernova explosions, which lead to trigger the formation of
next-generations of stars in the GMCs. It is therefore crucial to reveal the distribution andproperties of GMCs in a galaxy. The Magellanic System is a unique target to make suchdetailed comprehensive study of GMCs. This is because it is nearby and the LMC is nearlyface-on, making it feasible to unambiguously identify associated young objects within GMCs.
Recent millimeter and sub-millimeter observations in the Magellanic System have started toreveal the distribution and properties of the individual GMCs in detail and their relation to starformation activities. From the NANTEN CO surveys, three types of GMCs can be classified interms of star formation activities; Type I is starless, Type II is with H ii regions only, and TypeIII is associated with active star formation indicated by huge H ii regions and young starclusters. The further observations to obtain detailed structure of the GMCs by Mopra and
SEST and to search for the dense cores by ASTE and NANTEN2 in higher tansition lines of
CO have been carried out with an angular resolution of about 5 to 10 pc. These observations
revealed that the differences of the physical properties represent an evolutionary sequence of
GMCs in terms of density increase leading to star formation. Type I and II GMCs are at theearly phase of star formation where density does not yet become high enough to show active
star formation, and Type III GMCs represent the later phase where the average density is
increased and the GMCs are forming massive stars.
Mizuno, Y., A. Kawamura, T. Onishi, T. Minamidani, E. Muller, H. Yamamoto, T. Hayakawa,

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N. Mizuno, A. Mizuno, J. Stutzki, J. L. Pineda, U. Klein, F. Bertoldi, B.-C. Koo, M. Rubin, M.
Burton, A. Benz, H. Ezawa, N. Yamaguchi, K. Kohno, T. Hasegawa, K. Tatematsu, M. Ikeda, J.
Ott, T. Wong, A. Hughes, M. Meixner, R. Indebetouw, K. D. Gordon, B. Whitney, J.-P. Bernard,
and Y. Fukui [2010], "Warm and dense Molecular Gas in the N159 Region: 12CO J=4-3 and
13
CO J=3-2 Observations with NANTEN2 and ASTE," Publ. Astron. Soc. Japan, vol.62,
pp.51-67.
New 12CO J = 4-3 and 13CO J = 3-2 observations of the N 159 region, an active site of massive
star formation in the Large Magellanic Cloud, have been made with the NANTEN2 and ASTE
submillimeter telescopes, respectively. The 12CO J = 4-3 distribution is separated into threeclumps, each associated with N 159 W, N 159 E, and N 159 S. These new measurements
toward the three clumps are used in coupled calculations of molecular rotational excitation andline radiation transfer, along with other transitions of the 12CO J = 1-0, J = 2-1, J = 3-2, and J =7-6 as well as the isotope transitions of 13CO J = 1-0, J = 2-1, J = 3-2, and J = 4-3. The 13CO J= 3-2 data were newly taken for the present work. The temperatures and densities were foundto be ~70-80 K and ~3 x 103 cm-3 in N 159 W and N 159 E, and ~30 K and ~1.6 x 103 cm-3 in
N 159 S. These results were compared with the star-formation activity based on data of youngstellar clusters and H II regions as well as midinfrared emission obtained with the Spitzer
MIPS. The N 159 E clump is associated with cluster(s) embedded, as observed at 24 μm by the
Spitzer MIPS, and the derived high temperature, 80 K, is interpreted as being heated by thesesources. The N 159 E clump is likely to be responsible for a dark lane in a large H II region by
dust extinction. On the other hand, the N 159 W clump is associated with clusters embedded
mainly toward the eastern edge of the clump only. These clusters show offsets of 20" -40" fromthe 12CO J = 4-3 peak, and are probably responsible for heating indicated by the derived hightemperature, 70 K. The N 159 W clump exhibits no sign of star formation toward the 12CO J =4-3
peak position and its western region that shows enhanced R4-3/1-0 and R3-2/1-0 ratios. We
therefore suggest that the N 159 W peak represents a pre-star-cluster core of~105 M⦿ which deserves further detailed studies. The N 159 S clump shows little sign of starformation, as is consistent with the lower temperature, 30 K, and has a somewhat lower
density than N 159 W and N 159 E. The N 159 S clump is also a candidate for future starformation.
Mochizuki, N., K. Hachisuka, and T. Umemoto [2009], "Survey of Outer Galaxy Molecular
Lines Associated with Water Masers," Proc. of the "Approaching Micro-Arcsecond Resolution
with VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M.,
and Murata, Y., ASP Conf. Ser. vol.402, pp.384-387.
H2O masers in Young stellar objects (YSOs) in our Galaxy are one of the targets of the
VSOP-2 science. The advantage of VSOP-2 observation is the highest angular resolution
which can detect a proper motion of H2O masers for distant objects over short time intervals.
To find candidate sources, we observed H2O maser sources in the outer Galaxy using the VLA,
and we surveyed the molecular lines toward these sources to understand the environment of
YSOs. Higher H2 column densities of YSOs were found for objects with active H2O masers.
Momose, M., M. Hiramatsu, T. Tsukagoshi, Y. Shimajiri, N. Ikeda, Y. Kitamura, K. Kamegai,
H. Ezawa, R. Kawabe, and M. Saito, [2009], "Wide-field Imaging Survey of Dust Continuum
Emissions atλ= 1.1 mm toward the Chamaeleon and Lupus Regions with AzTEC on ASTE,"
Proc. of the "Exoplanets and disks: their formation and diversity", eds. Usuda, T., Tamura, M.,
and Ishii, M., AIP Conf. Proc., vol.1158, pp.141-142.
We carried out an imaging survey of dust continuum emissions toward the Chamaeleon andLupus regions. Observations were made with the 144-element bolometer array camera AzTEC
mounted on the 10-meter sub-millimeter telescope ASTE during 2007-2008. The preliminary

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results of disk search and the cloud structure of Lupus III are presented.
Momose, R., S. K. Okumura, J. Koda, and T. Sawada [2010], "Star Formation Efficiency in the
Barred Spiral Galaxy NGC 4303," Astrophys. J., vol.721, pp.383-394.
We present new 12CO (J = 1 - 0) observations of the barred galaxy NGC 4303 using theNobeyama 45 m telescope (NRO45) and the Combined Array for Research in Millimeter-wave
Astronomy (CARMA). The Hα images of barred spiral galaxies often show active starformation in spiral arms, but less so in bars. We quantify the difference by measuring starformation rate (SFR) and star formation efficiency (SFE) at a scale where local star formationis spatially resolved. Our CO map covers the central 2'3 region of the galaxy; the combinationof NRO45 and CARMA provides a high fidelity image, enabling accurate measurements ofmolecular gas surface density. We find that SFR and SFE are twice as high in the spiral arms asin the bar. We discuss this difference in the context of the Kennicutt-Schmidt (KS) law, whichindicates a constant SFR at a given gas surface density. The KS law breaks down at our native
resolution (~250 pc), and substantial smoothing (to 500 pc) is necessary to reproduce the KS
law, although with greater scatter.
Morita, K.-I., and M. A. Holdaway [2008], "The Array Configuration Design of the Atacama
Compact Array," Proc. of the SPIE, vol.7012, pp.701200-1-12.
The Atacama Compact Array (ACA) is an array composed of twelve 7-m dishes and four 12-m
dishes. The ACA is designed for use as a part of the ALMA (Atacama Large Millimeter /Submillimeter Array) to provide high fidelity imaging capability for large extended objects.
Basic parameters of the array configuration of the ACA were selected based on the analysis of
the sensitivity in uv plane for mosaicing observations with the ACA and the ALMA. For
detailed design of the sub-array with 7-m dishes (7-m Array), we adopted the compact spiralconcept, which realizes higher uv response at the short uv spacings and better sidelobe
performance. To satisfy the sky coverage requirement, the north-south elongation is needed.
The 7-m Array was designed to have two configurations, one (Inner Array) is a compact spiralarray with small north-south elongation (×1.1) and the other (NS Array) is a dedicatedconfiguration with large north-south elongation (×1.7). In actual design, inner 6 antenna pads
are shared by both configurations because of construction constraints.
Morota, T., J. Haruyama, C. Honda, M. Ohtake, Y. Yokota, J. Kimura, T. Matsunaga, Y. Ogawa,N. Hirata, H. Demura, A. Iwasaki, H. Miyamoto, R. Nakamura, Y. Ishihara, and S. Sasaki[2009a], "Ages and Thicknesses of Mare Basalts in Mare Moscoviense: Results from SELENE(KAGUYA) Terrain Camera Data," 40th Lunar and Planetary Science Conference, (Lunar andPlanetary Science XL), held March 23-27, 2009 in The Woodlands, Texas, id.1280. We
investigate ages and thicknesses of mare basalts in Mare Moscoviense, which is in the northernhemisphere of the lunar farside, using high-resolution images and digital terrain models(DTMs) obtained by SELENE Terrain Camera (TC).
Morota, T., J. Haruyama, C. Honda, M. Ohtake, Y. Yokota, J. Kimura, T. Matsunaga, Y. Ogawa,N. Hirata, H. Demura, A. Iwasaki, H. Miyamoto, R. Nakamura, H. Takeda, Y. Ishihara, and S.
Sasaki [2009b], "Mare Volcanism in the Lunar Farside Moscoviense Region: Implication for
Lateral Variation in Magma Production of the Moon," Geophys. Res. Letters, vol.36, CiteID
L21202-1-5.
Accurate estimates of the duration and volume of extrusive volcanism of the Moon are
essential for understanding the lunar thermal evolution. Here, using new high-resolution
images obtained by the SELENE Terrain Camera, we determined the thicknesses and ages ofbasalts in Mare Moscoviense, one of the most prominent mare deposits on the farside. Marevolcanism in Mare Moscoviense was active for at least ~1.5 Ga following the formation of the
Moscoviense basin. Mare basalts are estimated to be at least 600 m thick, corresponding to a
total volume of 9,500-16,000 km3. The long duration and large volume of extrusive volcanism

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are plausibly attributed to the thinner crust of the Moscoviense basin relative to those of otherfarside basins. From a comparison with mare volume within a same-sized nearside basin, we
concluded that a magma production in the farside mantle was 3-10 times less than that of thenearside.
Morota, T., J. Haruyama, M. Ohtake, T. Matsunaga, Y. Yokota, C. Honda, T. Sugihara, J.
Kimura, Y. Ishihara, T. Kawamura, A. Iwasaki, K. Saiki, and H. Takeda [2010], "MareVolcanism on the Farside and in the Oriental Region of the Moon," LPI Contribution No. 1533,
p.1309.
Dating of lunar mare basalts is necessary for understanding the volcanic history of the Moon.
Here we performed new crater counts in mare deposits on the farside and in the Orientale
region, using new images obtained by SELENE Terrain Camera.
Motogi, K., Y. Watanabe, K. Sorai, M. Honma, H. Imai, A. Yamauchi, H. Kobayashi, K.
Fujisawa, T. Omodaka, H. Takaba, K. M. Shibata, T. Minamidani, K. Wakamatsu, H. Sudou, E.
Kawai, and Y. Koyama [2008], "Microstructure and Kinematics of H2O Masers in the Massive
Star Forming Region IRAS 06061+2151," Mon. Not. Roy. Astron. Soc., vol.390, pp.523-234.
We have made multi-epoch very long baseline interferometer (VLBI) observations of H2O
maser emission in the massive star-forming region IRAS 06061+2151 with the Japanese VLBI
network (JVN) from 2005 May to 2007 October. The detected maser features are distributed
within a 1 x 1 arcsec2 area (2000 x 2000 au2 at the source position) around the ultracompact
Hii region seen in radio continuum emission. The bipolar morphology and expanding motion
traced through their relative proper motions indicate that they are excited by an energetic
bipolar outflow. Our three-dimensional model fitting has shown that the maser kinematicalstructure in IRAS 06061+2151 can be explained by a biconical outflow with a large opening
angle (>50°). The position angle of the flow major axis coincides very well with that of thelarge-scale jet seen in 2.1μm hydrogen emission. This maser geometry indicates the existenceof dual structures composed of a collimated jet and a less collimated massive molecular flow.
We have also detected a large velocity gradient in the southern maser group. This can be
explained by a very small (on a scale of several tens of astronomical units) and clumpy (thedensity contrast by an order of magnitude or more) structure of the parental cloud. Such astructure may be formed by strong instability of the shock front or splitting of the high density
core.
Muller, E., J. Ott, A. Hughes, J. Pineda, T. Wong, N. Mizuno, A. Kawamura, Y. Mizuno, Y.
Fukui, T. Onishi, and M. Rubio [2010], "Characterizing the Low-Mass Molecular Component
in the Northern Small Magellanic Cloud," Astrophys. J., vol.712, pp.1248-1258.
We present here the first results from a high-resolution survey of the 12CO(J=1-0) emission
across the northern part of the poorly enriched Small Magellanic Cloud (SMC), made with the
ATNF Mopra telescope. Three molecular complexes detected in the lower resolution
NANTEN survey are mapped with a beam FWHM of ~42'', to sensitivities of approximately
210 mK per 0.9 km s-1 channel, resolving each complex into 4-7 small clouds of masses in therange of Mvir ~ 103-104 Msun and with radii no larger than 16 pc. The northern SMC CO clouds
follow similar empirical relationships to the southern SMC population, yet they appear
relatively under-luminous for their size, suggesting that the star-forming environment in the
SMC is not homogeneous. Our data also suggests that the CO cloud population has little or no
extended CO envelope on scales gsim30 pc, further evidence that the weak CO component in
the north SMC is being disassociated by penetrating UV radiation. The new high-resolution
data provide evidence for a variable correlation of the CO integrated brightness with integrated
H I and 160 μm emission; in particular CO is often, but not always, found coincident withpeaks of 160 μm emission, verifying the need for matching-resolution 160 μm and H I data for
a complete assessment of the SMC H2 mass.

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Muraoka, K., K. Kohno, T. Tosaki, N. Kuno, K. Nakanishi, K. Sorai, and S. Sakamoto [2008],"CO(3-2) Wide Area Imaging of M83 with ASTE: Correlation between CO(3-2)/CO(1-0)
Ratios and Star Formation Efficiencies," Proc. of the "Mapping the Galaxy and Nearby
Galaxies", eds. Wada, K., and Combes, F., p.357.
Without abstract
Muraoka, K., K. Kohno, T. Tosaki, N. Kuno, K. Nakanishi, K. Sorai, S. Ishizuki, T. Handa, andT. Okuda, [2009a], "Nobeyama Millimeter Array Observations of the Nuclear Starburst of
M83: A GMA Scale Correlation between Dense Gas Fraction and Star Formation Efficiency,"
Publ. Astron. Soc. Japan, vol.61, pp.163-176.
We present aperture synthesis high-resolution ( ~7"x3") observations in CO (J = 1-0), HCN (J= 1-0), and 95 GHz continuum emission toward the central (~1.5 kpc) region of the nearby
barred spiral galaxy M 83 with the Nobeyama Millimeter Array. Our high-resolution CO (J =1-0) mosaic map depicts the presence of molecular ridges along the leading sides of the stellar
bar and a nuclear twin peak structure, whereas the distributions of the HCN (J = 1-0) emissionthat traces dense molecular gas (nH2 > a few x 104 cm-3) and the 95 GHz continuum emissionthat traces massive starburst show nuclear single-peak structures. The HCN (J = 1-0) and the
95 GHz continuum peaks are not spatially coincident with the optical starburst regions tracedby the HST V -band image, suggesting the existence of deeply buried ongoing starburst due tostrong extinction (AV ~ 5 mag) near these peaks. We found that the HCN (J = 1-0)/CO (J =1-0) intensity ratio, RHCN/CO correlates well with the extinction-corrected star formation
efﬁciency (SFE) in the central region of M 83 at a resolution of 7".5 (~160 pc). This suggeststhat SFE is controlled by a dense gas fraction traced by RHCN/CO, even on a Giant Molecular
cloud Association (GMA) scale. Moreover, the correlation between RHCN/CO and SFE in M 83
seems to be almost coincident with that among the Gao and Solomon (2004a, ApJ, 606, 271)
sample. This suggests that the correlation between RHCN/CO and the SFE on a GMA (~160 pc)
scale found in M 83 is the origin of the global correlation on a few kpc scale shown by Gao
and Solomon (2004a).
Muraoka, K., K. Kohno, T. Tosaki, N. Kuno, K. Nakanishi, K. Sorai, T. Sawada, K. Tanaka,
T. Handa, M. Fukuhara, H. Ezawa, and R. Kawabe, [2009b], "ASTE CO(3-2) Mapping toward
the Whole Optical Disk of M 83: Properties of Inter-arm Giant Molecular-Cloud
Associations," Astrophys. J., vol.706, pp.1213-1225.
We present a new on-the-fly mapping of CO (J = 3-2) line emission with the Atacama
Submillimeter Telescope Experiment toward the 8'x8' (or 10.5x10.5 kpc at the distance of 4.5
Mpc) region of the nearby barred spiral galaxy M 83 at an effective resolution of 25''. Due toits very high sensitivity, our CO (J = 3 - 2) map can depict not only spiral arm structures but
also spur-like substructures extended in inter-arm regions. This spur-like substructures in CO(J = 3-2) emission are well coincident with the distribution of massive star-forming regions
traced by Hα luminosity and Spitzer/Infrared Array Camera 8 m emission. We haveidentified 54 CO (J = 3-2) clumps as Giant Molecular-cloud Associations (GMAs) employing
the CLUMPFIND algorithm, and have obtained their sizes, velocity dispersions, virial masses,
and CO luminosity masses. We found that the virial parameter α, which is defined as the ratioof the virial mass to the CO luminosity mass, is almost unity for GMAs in spiral arms, whereas
there exist some GMAs whose are 3-10 in the inter-arm region. We found that GMAs withhigher α tend not to be associated with massive star-forming regions, while other virialized
GMAs are. Since α mainly depends on velocity dispersion of the GMA, we suppose that theonset of star formation in these unvirialized GMAs with higher α are suppressed by an increase
in internal velocity dispersions of giant molecular clouds within these GMAs due to shear
motion.
Murata, Y., N. Mochizuki, H. Saito, H. Hirabayashi, M. Inoue, H. Kobayashi, P. D. Edwards,

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and the Next Generation Space VLBI Working Group [2008], "The Next Generation SpaceVLBI Project, VSOP-2," Proc. of the IAU Symp. 242, "Astrophysical Masers and their
Environments", eds. Jessica Chapman and Willem Baan, pp.517-521.
The first dedicated space-VLBI project, the VLBI Space Observatory Programme (VSOP),
commenced with the successful launch of radio-astronomical satellite HALCA in 1997. Plans
for a second generation space-VLBI project have been made by a working group over anumber of years. This project, VSOP-2, has now been approved by Japan's space agency,
JAXA, as the ASTRO-G project. It is planned for the spacecraft to observe in the 8, 22 and 43
GHz bands with cooled receivers for the two higher bands, which include important maserlines. It will have a maximum angular resolution at 43 GHz (7 mm) of about 40
micro-arcseconds. Although the VSOP project mainly observed continuum emission from
active galactic nuclei (AGN), VSOP-2/ASTRO-G is expected to enable a variety of highangular resolution maser line observations.
Nagai, H., M. Inoue, K. Asada, S. Kameno, and A. Doi [2008], "Kinematic Aging and Spectral
Aging in Young Radio Galaxies," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds.
Wada, K., and Combes, F., p.358.
Without abstract
Nagai, H., K. Asada, A. Doi, M. Kino, S. Kameno, and VSOP-2 Science Working Group[2009], "Disk-Jet Connection in the Nearby Low Luminosity AGN M 81: A Proposal for
VSOP-2 Key Science Program," Proc. of the "Approaching Micro-Arcsecond Resolution with
VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and
Murata, Y., ASP Conf. Ser. vol.402, pp.110-111.
We propose a monitoring observation to probe the disk-jet connection in the nearby low
luminosity AGN M 81 with VSOP-2 and an X-ray telescope. M 81 is the nearest Active
Galactic Nuclei and VSOP-2 can resolve the region near the central black hole andjet-launching region. This proposal is one of the Key Science Programs.
Nagai, H., K. Suzuki, K. Asada, M. Kino, S. Kameno, A. Doi, M. Inoue, J. Kataoka, U. Bach,
T. Hirota, N. Matsumoto, M. Honma, H. Kobayashi, and K. Fujisawa [2010], "VLBI
Monitoring of 3C 84 (NGC 1275) in Early Phase of the 2005 Outburst," Publ. Astron. Soc.
Japan, vol.62, pp.L11-L15.
Multi-epoch Very Long Baseline Interferometry (VLBI) study of a sub-pc scale jet of 3C 84 ispresented. We carried out 14-epoch VLBI observations during 2006-2009 with the Japanese
VLBI Network and the VLBI Exploration of Radio Astrometry, immediately following a radio
outburst that began in 2005. We confirmed that the outburst was associated with the central ~1
pc core accompanying the emergence of a new component. This is striking evidence of therecurrence of jet activity. The new component became brighter during 2008, in contrast to
constant γ-ray emission that was observed with the Fermi Gamma-ray Space Telescope during
the same time. We found that the projected speed of the new component was 0.23 c from2007/297 (2007 October 24) to 2009/114 (2009 April 24). The direction of movement of thiscomponent differs from that of the pre-existing component by ~40°. This was the firstmeasurement of the kinematics of a sub-pc jet in a γ-ray active phase. A possible detection ofjet deceleration and the jet kinematics in connection with theγ-ray emission is discussed.
Nagai, M., T. Oka, S. Yamamoto, Y. Moriguchi, Y. Fukui, and Y. Sekimoto [2008], "High-Velocity [CI] Wing Emission Toward the M71 Molecular Cloud," Proc. of the "Mapping
the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F., 359.
Without Abstract
Nagayama, T., T. Omodaka, T. Handa, T. Sawada, H. B. Iahak, and N. Matsuyama [2008a], "A
Wide Survey in NH3 Lines of the Central 200 pc Around the Galactic Center with Kagoshima
6 Meter Radio Telescope," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds. Wada,

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K., and Combes, F., p.361.
Without abstract
Nagayama, T., A. Nakagawa, H. Imai, T. Omodaka, and Y. Sofue [2008b], "VLBI
Observations of Water Masers in Onsala1: Massive Binary Star-Forming Site?," Publ. Astron.
Soc. Japan, vol.60, pp.183-190.
We present the proper motions of water masers toward the Onsala 1 star-forming region,
observed with the Japanese VLBI network at three epochs spanning 290 days. We found that
there are two-water maser clusters (WMC1 and WMC2) separated from each other by 1".6(2900 AU at a distance of 1.8 kpc). A proper-motion measurement reveals that WMC1 isassociated with a bipolar outflow elongated in the east-west direction with an expansion
velocity of 69±11 km s-1. WMC1 and WMC2 are associated with two 345 GHz continuum
dust emission sources, which were located 2" (3600 AU) east from the core of an ultracompact
HII region traced by 8.4 GHz radio continuum emission. This indicates that the star-formation
activity of Onsala 1 could move from the west side of the ultracompact HII region to the eastside of two young stellar objects associated with the water masers. We have also find that
WMC1 and UC HII regions could be gravitationally bound. Their relative velocity along theline of sight is ~3 km s-1, and total mass is ~37 Mo. Onsala 1 seems to harbor a binary star at adifferent evolutionary stage.
Nagayama, T., K. Takeda, T. Omodaka, H. Imai, S. Kameno, Y. Sofue, A. Doi, K. Fujisawa, A.
Habe, M. Honma, N. Kawaguchi, E. Kawai, H. Kobayashi, Y. Koyama, Y. Murata, K. Sorai, H.
Sudou, H. Takaba, S. Tamura, and K. Wakamatsu [2008c], "H2O Maser Outflow from the Red
Supergiant Star NML Cygni Observed with Japanese VLBI Network," Publ. Astron. Soc.
Japan, vol.60, pp.1069-1075.
We present the proper motions of H20 masers in NML Cygni, observed with the Japanese VLB
Network at three epoch spanning 455 d. We detected about 15 maser features at each epoch.
Overall, 13 features that were detected at least twice were tracked by their radial velocities andproper motions. The three-dimensional kinematics of the maser features indicate the presenceof an expanding outflow. The major axis of the outflow is estimated to be at a position angle of~ 108°, and an inclination angle of ~ 8° with respect to the line of sight. The H2O masers arelocated between an apparent minimum radius of ~ 9.6 x 1012 m (64 AU) and a maximum
radius of ~ 3.0 x 1013 m (202 AU), where the expansion velocity increases from 12 to 27 km s-1.
A comparison with the distributions of SiO, H2O, and OH masers suggests that the outflow of
NML Cygni is expanding outside a radius of ~ 1.5 x 1013 m (100 AU). This radius corresponds
to 6 stellar radii, and is consistent with the radius of the inner boundary for the dust shell.
Nagayama, T., S. Sato, S. Nishiyama, Y. Murai, T. Nagata, H. Hatano, M. Kurita, M. Tamura,
Y. Nakajima, K. Sugitani, T. OKa, and Y. Sofue [2009a], "A Chain of Dark Clouds in
Projection Against the Galactic Center," Publ. Astron. Soc. Japan, vol.61, pp.283-290.
In a J, H, and KS band survey of the Galactic center region over an area of 2°
x 5°, we have found many dark clouds, among which a distinguished chain of dark clouds canbe identiﬁed with a quiescent CO cloud. The distances of the clouds are estimated to be
3.2-4.2kpc, corresponding to the Norma arm, by our new method for determining the distances
to dark clouds using the cumulative number of stars against the J - KS color. By adopting theseestimated distances, the size and total mass of the cloud are estimated to be ~70 pc in lengthand 6 x 104 M⦿,respectively. Three compact H II regions exist in the cloud, indicating that star forming
activities are going on at the cores of the quiescent CO cloud on the spiral arm.
Nagayama, T., T. Omodaka, T. Handa, H. Toujima, Y. Sofue, T. Sawada, H. Kobayashi, and Y.
Koyama [2009b], "NH3 in the Galactic Center is formed Cool Contributions," Publ. Astron.
Soc. Japan, vol.61, pp.1023-1037.

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It is an open question as to why the temperature of molecular gas in the Galactic center regionis higher than that of dust. To address this problem, we made simultaneous observations in the
NH3 (J,K) = (1, 1), (2, 2), and (3, 3) lines of the central molecular zone (CMZ) using theKagoshima 6-m telescope. The ortho-to-para ratio of NH3 molecules in the CMZ is 1.5-3.5 atmost in the observed area. This ratio is higher than the statistical equilibrium value, andsuggests that the formation temperature of NH3 is 11-20 K. This temperature is similar to thedust temperature estimated from the submillimeter and infrared continuum. This result
suggests that the NH3 molecules in the CMZ were produced on dust grains with the currently
observed temperature (11-20 K), and they were released into the gas phase by supernova
shocks or collisions of dust particles. The discrepancy between warm molecular gas and cold
dust can be explained by transient heating of the interstellar media in the CMZ approximately
105 yr ago when NH3 molecules were released from the dust.
Nakagawa, A., T. Omodaka, K. M. Shibata, T. Kurayama, H. Imai, S. Kameno, M. Tsushima,
M. Shintani, N. Matsumoto, M. Matsui, S. Oizumi, T. Yasuda, and Y. Arao [2008a], "VLBI
Monitoring of Mira Variables with VERA," Proc. of the IAU Symp. 242, "Astrophysical
Masers and their Environments", eds. Jessica Chapman and Willem Baan, pp.326-327.
We have started a VLBI monitoring program for Asymptotic Giant Branch (AGB) stars at 22
and 43 GHz as part of a project of the VLBI Exploration of Radio Astrometry (VERA) for
precisely obtaining the period-luminosity (PL) relation of Galactic Mira variables. Using
accurate distances measured with VERA, we reveal PL relation in the Galaxy based on theabsolute magnitudes of the sources. We selected the sources for VLBI monitoring so that they
have a good coverage of various pulsation periods. Photometry in the infrared J, H, and K
bands for over 600 AGB stars has also started since 2003 with the 1m telescope of Kagoshima
University to obtain the pulsation periods and magnitudes. Current analysis of the phasereferencing VLBI observations of S Crt shows that the parallax of 2.3±0.2 milliarcsec (mas)corresponds to a distance of 435+41-35 pc. From the infrared monitoring data, pulsation periods
and magnitudes in K band for 248 sources were obtained.
Nakagawa, A., T. Omodaka, K. M. Shibata, T. Kurayama, H. Imai, S. Kameno, M. Tsushima,
N. Matsumoto, and M. Matsui [2008b], "Parallax Measurement of the Galactic Mira Variables
with VERA," Proc. of the IAU Symp. 248, "A Giant Step: from Milli- to Micro-arcsecond
Astrometry", eds. Wenjing Jin, Imants Platais, Michael A. C. Perryman, pp.206-207.
Parallax measurements of the Galactic Mira variables with VERA have started since 2004 to
establish their Period-Luminosity (PL) relationship in the Galaxy. Multi-epoch VLBI
observations of a semiregular variable S Crt yielded an accurate parallax of 2.27±0.14 mascorresponding to the distance of 441+29-24 pc. In addition to the distance, we obtained physicalproperties of S Crt. Temperature of the photosphere was found to be ~3000 K by fitting theinfrared spectrum with a blackbody radiation. The stellar radius was obtained based on the
distance, apparent magnitude, and the temperature. Internal proper motions ofcircularly-arranged maser spots in S Crt were detected for the first time. Observations of theother Mira variables, such as R UMa, SY Scl, AP Lyn, and WX Psc are in progress.
Nakagawa, A., M. Tsushima, K. Ando, T. Bushimata, Y. K. Choi, T. Hirota, M. Honma, H.
Imai, K. Iwadate, T. Jike, S. Kameno, O. Kameya, R. Kamohara, Y. Kan-Ya, N. Kawaguchi, M.
Kijima, M. K. Kim, H. Kobayashi, S. Kuji, T. Kurayama, T. Maeda, S. Manabe, K. Maruyama,
M. Matsui, N. Matsumoto, T. Miyaji, T. Nagayama, K. Nakamura, D. Nyu, C. S. Oh, T.
Omodaka, T. Oyama, N. Pradel, S. Sakai, T. Sasao, K. Sato, M. Sato, K. M. Shibata, H. Suda,
Y. Tamura, K. Ueda, Y. Ueno, and K. Yamashita [2008c], "VLBI Astrometry of AGB
Variables with VERA - A Semiregular Variable S Crateris -," Publ. Astron. Soc. Japan, vol.60,
pp.1013-1021.
We present a distance measurement for the semiregular variable S Crateris (S Crt) based on its

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annual parallax. With the unique dual beam system of the VLBI Exploration for Radio
Astrometry (VERA) telescopes, we measured the absolute proper motion of a water maser spot
associated with S Crt, referred to the quasar J1147-0724 located at an angular separation of
1.°23. In observations spanning nearly two years, we detected the maser spot at an LSR
velocity of 34.7 km s-1, for which we measured an annual parallax of 2.33±0.13 mas,corresponding to a distance of 430+25-23 pc. This measurement has an accuracy one order ofmagnitude better than the parallax measurements of HIPPARCOS. The angular distribution
and three-dimensional velocity field of maser spots indicate a bipolar outflow with the flow
axis along the northeast-southwest direction. Using the distance and photospheric temperature,
we estimate the stellar radius of S Crt and compare it with those of Mira variables.
Nakagawa, H., Y. Kasaba, H. Maezawa, A. Hashimoto, H. Sagawa, I. Murata, S. Okano, S.
Aoki, N. Moribe, A. Mizuno, M. Momose, T. Ohnishi, N. Mizuno, and T. Nagahama [2009],"Search of SO2 in the Martian Atmosphere by Ground-Based Submillimeter Observation,"
Planetary and Sp. Sci., vol.57, pp.2123-2127.
We searched sulfur oxide (SO2 and SO) in the Martian atmosphere by the Atacama
Submillimeter Telescope Experiment (ASTE). Sulfur oxide is one of the most evident species
in terrestrial volcanic gases. Although it has not yet been detected at Mars, this detection canconstraint the Martian crustal and volcanic activities. We observed northern winter of Mars on
26 December 2007 (Ls=8.1°) in 346 GHz range with ~1h integration. We get the upper limit of
the SO2 mixing ratio, 2 ppb. This is mostly equivalent to the value observed in northernsummer (Ls=205°) (Krasnopolsky, 2005). We concluded that the crustal or volcanic gas
produced into the atmosphere is tenuous in northern winter. Even at Mars, it can be expectedthat the crustal or volcanic gas includes non-negligible amount of SO2 produced asdegasification from the magma. Our result and recent detections of CH4 suggest a possibilityof some kind of carbon hydride sources under the ground reservoir, independent of usual
crustal and volcanic activities.
Nakagawa, H., Y. Kasaba, S. Aoki, I. Murata, H. Maezawa, S. Okano, H. Sagawa, and Y. Kasai[2010], "High Spectral Resolution Observations of Martin Atmosphere in Infrared Submillimeter Rang from Ground-Based Instruments," Geophys. Res. Abstracts, vol.12,
pp.EGU2010-2010-1.
With increased knowledge on our “neighbor” planets Mars and Venus, based on recent
aggressive explorations by the US and Europe, our image on them is changing significantly. In
particular, Mars is called ‘a frozen water planet’. It is almost certain that Mars once had
duration with warm and wet climate [Head et al., 1999; Donahue, 1995; Parker et al., 1993]. It
still conserves a large amount of water ice under the surface [Boynton et al., 2002; Mitrofanov
et al., 2002; Feldman et al., 2002]. The question “Why and when did they diverge?” isessential for their environments which potentially could create and keep the life or not. Many
molecules in planetary atmospheres show transitions in the mid infrared - submillimeter region.
Thus, high-resolution spectroscopy in this region is significantly indispensable to study
planetary atmospheres.
We searched sulfur oxide (SO2 and SO) in the Martian atmosphere by the Atacama
Submillimeter Telescope Experiment (ASTE). Sulfur oxide is one of the most evident species
in terrestrial volcanic gases. Although it has not yet been detected at Mars, this detection canconstraint the Martian crustal and volcanic activities. We observed northern winter of Mars on
26/Dec./2007 (Ls=8.1) in 346 GHz range with ~1h integration, and got the upper limit of theSO2 mixing ratio, 2 ppb. We concluded that the crustal or volcanic gas produced into theatmosphere is tenuous in northern winter [Nakagawa et al., 2009].
Infrared heterodyne spectroscopy has proven to be a powerful tool for astrophysical studies. To
achieve highest spectral resolution and sensitivity as well as compact instrumentation

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heterodyne systems are advantageous over direct-detection methods. Our group in Tohoku
University has developed own heterodyne system for infrared spectrometer for Earth’s
atmosphere over the past 20 years. The failure of earlier attempts to build tunable systems
using tunable diode lasers was due mostly to insufficient laser power. Recently, quantum
cascade lasers (QCLs) offer sufficient optical output power of several milliwatts to guarantee
an efficient heterodyning process and high system sensitivity. The use of QCLs in our system
led to a breakthrough giving the heterodyne infrared spectrometer for planetary atmosphere.
We report experiments evaluating the feasibility of QCLs at mid-infrared wavelengths for use
as local oscillator (LO) in a heterodyne receiver. Performance tests with the QCL provided byHamamatsu Photonics (operating at 7.7 um), and QCL provided by Maxion
Technologies(operating at 10.6 um in room temperature) were evaluated.
Nakajima, T., T. Sakai, S. Asayama, K. Kimura, M. Kawamura, Y. Yonekura, H. Ogawa, N.
Kuno, T. Noguchi, M. Tsuboi, and R. Kawabe [2008a], "Development of a Waveguide-Type
Dual-Polarization Sideband-Separating SIS Receiver System in 100 GHz Band for the NRO
45-m Radio Telescope," Proc. of the 19th International Symposium on Space THz Technology,
ed. Wolfgang Wild, pp.286-291.
We developed a waveguide-type dual-polarization sideband-separating SIS receiver system of
the 100-GHz band for the 45-m radio telescope at the Nobeyama Radio Observatory, Japan.
This receiver is composed of an ortho-mode transducer and two sideband-separating SIS
mixers, which are both based on the waveguide technique. The receiver has four intermediate
frequency (IF) bands of 4.0-8.0 GHz. Over the radio frequency range of 80-120 GHz, thesingle-sideband receiver noise temperatures are 50-100 K and the image rejection ratios are
greater than 10 dB. The new receiver system was installed in the telescope, and we
successfully observed the 12CO, 13CO, C18O and the other emission lines simultaneously
toward the Sagittarius B2 region to confirm the performance of the receiver system.
Nakajima, T., T. Sakai, S. Asayama, K. Kimura, M. Kawamura, Y. Yonekura, H. Ogawa, N.
Kuno, T. Noguchi, M. Tsuboi, and R. Kawabe [2008b], "A New 100-GHz Band Front-End
System with a Waveguide-Type Dual-Polarization Sideband-Separating SIS Receiver for the
NRO 45-m Radio Telescope," Publ. Astron. Soc. Japan, vol.60, pp.435-443.
We developed a waveguide-type dual-polarization sideband-separating SIS receiver system of
the 100-GHz band for the 45-m radio telescope at the Nobeyama Radio Observatory, Japan.
This receiver is composed of an ortho-mode transducer and two sideband-separating SIS
mixers, which are both based on the waveguide technique. The receiver has four intermediate
frequency bands of 4.0-8.0 GHz. Over the radio frequency range of 80-120 GHz, thesingle-sideband receiver noise temperatures are 50-100 K and the image rejection ratios are
greater than 10 dB. We developed new matching optics for the telescope beam as well as new
IF chains for the four IF signals. The new receiver system was installed in the telescope, andwe successfully observed the 12CO, 13CO and C18O emission lines simultaneously toward the
Sagittarius B2 region to confirm the performance of the receiver system. The SSB noise
temperature of the system, including the atmosphere, became approximately half of that of theprevious receiver system. The Image Rejection Ratios (IRRs) of the two 2SB mixers were
calculated from the 12CO and HCO+ spectra from the W51 giant molecular cloud, resulting in> 20 dB for one polarization and > 12 dB for the other polarization.
Nakajima, T., T. Sakai, N. Kuno, and H. Ogawa [2010], "Development of the Measurement
System of Image Rejection Ratio for the Sideband-Separating Receiver," J. Infrared Milli.
Terahz. Waves, vol.31, pp.143-150.
We developed a measurement system of image rejection ratio for the sideband-separatingreceiver. This system comprises a horn moved by a motor slider, a harmonic mixer and a signal
generator. We have installed the system on the Nobeyama 45-m millimeter telescope and

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compared the image rejection ratio measured by this system with that obtained from molecularline observations of celestial objects. We confirmed that we can measure image rejection ratiowith an accuracy of ±10% with our system. By using the system, we can tune the applied bias
voltage of mixer chips to the best performance of image rejection ratio and accurate calibrationof the intensity of molecular line observations becomes possible. This is the first IRR
measurement system developed for practical use with the 2SB receiver system.
Nakanishi, K., N. Sato, N. Kuno, S. K. Okumura, R. Kawabe, K. Kohno, A. Yamauchi, andN.Nakai [2008], "Radio Continuum and Water Vapor Maser Monitoring Toward the Luminous
Infrared Galaxy NGC 6240," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds.
Wada, K., and Combes, F., p.364.
Without abstract
Nakashima, J., and S. Deguchi [2007], "Correlation between Infrared Colors and Intensity
Ratos of SiO Maser Lines," Astrophys. J., vol.669, pp.446-458.
We present the results of SiO millimeter line observations of a sample of known SiO maser
sources covering a wide dust temperature range. A cold part of the sample was selected fromthe SiO maser sources found in our recent SiO maser survey of cold dusty objects. The aim of
the present research is to investigate the causes of the correlation between infrared colors and
SiO maser intensity ratios among different transition lines. In particular, the correlation
between infrared colors and SiO maser intensity ratio among the J=1-0 v=1, 2, and 3 lines are
our main concern in this paper. We observed in total 75 SiO maser sources with the Nobeyama
45 m telescope quasi-simultaneously in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines.
We also observed the sample in the 29SiO J=1-0 v=0 and J=2-1 v=0 lines, 30SiO J=1-0 v=0 line,
and the H2O 61,6-52,3 line. As reported in previous papers, we confirmed that the intensity ratiosof the SiO J=1-0 v=2 to v=1 lines clearly correlate with infrared colors. In addition, we foundpossible correlation between infrared colors and the intensity ratios of the SiO J=1-0 v=3 tov=1 and 2 lines. Two overlap lines of H2O (i.e., 116,6 ν2=1→127,5 ν2=0 and 50,5 ν2=2→63,4
ν2=1) might explain this correlation if these overlap lines become stronger with an increaseof infrared colors, although the phenomena also might be explained in more fundamental ways
if we take into account the variation of opacity from object to object.
Nakashima, J., and S. Deguchi [2008a], "SiO Maser Observations of a Wide Dust-Temperature
Range Sample," Proc. of the IAU Symp. 242, "Astrophysical Masers and their Environments",
eds. Jessica Chapman and Willem Baan, pp.266-270.
We present the results of SiO line observations of a sample of known SiO maser sources
covering a wide dust-temperature range. The aim of the present research is to investigate thecauses of the correlation between infrared colors and SiO maser intensity ratios among
different transition lines. We observed in total 75 SiO maser sources with the Nobeyama 45m
telescope quasi-simultaneously in the SiO J = 1-0 v = 0, 1, 2, 3, 4 and J = 2-1 v = 1, 2 lines. We
also observed the sample in the 29SiO J = 1-0 v = 0 and J = 2-1 v = 0, and 30SiO J = 1-0 v = 0
lines, and the H2O 61,6-52,3 line. As reported in previous papers, we confirmed that the intensity
ratios of the SiO J = 1-0 v = 2 to v = 1 lines clearly correlate with infrared colors. In addition,
we found possible correlation between infrared colors and the intensity ratios of the SiO J =1-0 v = 3 to v = 1&2 lines.
Nakashima, J., S. Deguchi, H. Imai, and A. Kembell [2008b], "Molecular Line Observations of
the SiO Maser Source IRAS 19312+1950," Proc. of the IAU Symp. 251, "Organic Matter inSpace", eds. S. Kwok, and S. Sandford, pp.165-166.
IRAS 19312+1950 is a unique SiO maser source, exhibiting a rich set of molecular radio lines,
although SiO maser sources are usually identified as oxygen-rich evolved stars, in which
chemistry is relatively simple comparing with carbon-rich environments. The rich chemistry of
IRAS 19312+1950 has raised a problem in circumstellar chemistry if this object is really an

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oxygen-rich evolved star, but its evolutional status is still controversial. In this paper, we
briefly review the previous observations of IRAS 19312+1950, as well as presenting
preliminary results of recent VLBI observations in maser lines. PDF file of the poster isavailable from http://www.geocities.jp/nakashima_junichi/
Namiki, N., T. Iwata, K. Matsumoto, H. Hanada, H. Noda, M. Ogawa, N. Kawano, K. Asari, S.
Tsuruta, S. Goossens, Q. Liu, F. Kikuchi, Y. Ishihara, T. Ishikawa, S. Sasaki, and C. Aoshima[2008a], "Initial Results of Gravity Experiment by Four-Way Doppler Measurement of Kaguya(SELENE)," 39th Lunar and Planetary Science Conference, (Lunar and Planetary Science
XXXIX), held March 10-14, 2008 in League City, Texas. LPI Contribution No. 1391, p.1596.
Current lunar gravity field models include large uncertainties on the far side of the Moon. We
developed a satellite-to-satellite Doppler tracking sub-system on Kaguya. New results of direct
tracking data on the far side will be discussed.
Namiki, N., H. Hanada, T. Iwata, Rsat Team, Vrad Team, and Lalt Team [2008b], "Lunar Far
Side Gravity from the Kaguya (SELENE) Mission and Dichotomy of the Moon," Meteoritics
and Planetary Sci. Suppl., 43, paper id. 5193, 2008.
Not Available
Namiki, N., H. Hanada, T. Iwata, R. Team, V. Team, and L. Team [2008c], "Lunar Far Side
Gravity From SELENE Mission And Dichotomy of the Moon," American Geophysical Union,
Fall Meeting 2008, abstract #P13E-02.
Current lunar gravity field models include large uncertainties on the far side of the Moon. We
developed a satellite-to-satellite Doppler tracking sub-system (RSAT) on SELENE(KAGUYA). Main function of RSAT is to relay Doppler tracking signals between the main
orbiter (MAIN) over the far side and ground-based antenna. When MAIN is orbiting over thefar side of the Moon, tracking signal in S band is relayed by Rstar to MAIN. Then MAIN
returns the tracking signal to Rstar to downlink a coherent Doppler signal to the antenna.
RSAT realizes the first direct observation of the gravity field over the far side of the moon. The
most recent lunar gravity models from SELENE enable global gravity anomaly mapping of theMoon up to degrees as high as 100. Gravity anomaly of our new models on the near side isalmost identical with that of Lunar Prospector, however, gravity anomaly map on the far side
reveals dramatic improvement. Gravity signatures over far-side basins that used to berecognized as linear features are now identified as circular anomaly. New gravity model
reveals a marked difference of gravity signatures between the near side and the far side. It has
been well known that near-side gravity anomaly is dominated by mascons, that is, positive
gravity anomaly indicating mantle uplift beneath basins. In contrast, far-side gravity field ischaracterized by rings of negative free-air anomaly over basins and large craters. Bouguer
gravity anomaly map shows that such negative anomaly can be mostly attributed totopographic depression of basin, and that contribution of Moho variation is minor. Our newmodels suggest that elastic thickness of lithosphere was thin on the near side while was thickon the far side, and propose an important constraint on the origin of dichotomy.
Namiki, N., T. Iwata, K. Matsumoto, H. Hanada, H. Noda, S. Goossens, M. Ogawa, N.
Kawano, K. Asari, S. Tsuruta, Y. Ishihara, Q. Liu, F. Kikuchi, T. Ishikawa, S. Sasaki, C.
Aoshima, K. Kurosawa, S. Sugita, and T. Takano [2009a], "Farside Gravity Field of the Moon
from Four-Way Doppler Measurements of SELENE (Kaguya)," Science, vol.323, pp.900-905.
The farside gravity field of the Moon is improved from the tracking data of the Selenologicaland Engineering Explorer (SELENE) via a relay subsatellite. The new gravity field model
reveals that the farside has negative anomaly rings unlike positive anomalies on the nearside.
Several basins have large central gravity highs, likely due to super-isostatic, dynamic uplift ofthe mantle. Other basins with highs are associated with mare fill, implying basalt eruption
facilitated by developed faults. Basin topography and mantle uplift on the farside are supported

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by a rigid lithosphere, whereas basins on the nearside deformed substantially with eruption.
Variable styles of compensation on the near- and farsides suggest that reheating and weakeningof the lithosphere on the nearside was more extensive than previously considered.
Namiki, N., S. Sugita, K. Matsumoto, S. Goossens, Y. Ishihara, H. Noda, S. Sasaki, T. Iwata, H.
Hanada, H. Araki, K. Kurosawa, M. Matsumura, M. Yokoyama, S. Kamata, N. Kubo, A. Mori,
and M. Sato [2009b], "Comparative Study of Compensation Mechanism of Lunar Impact
Basins from New Gravity Field Model of SELENE (Kaguya)," 40th Lunar and Planetary
Science Conference, (Lunar and Planetary Science XL), held March 23-27, 2009 in The
Woodlands, Texas, id.1519.
Based on the gravity model of the Moon by SELENE, we propose new classification andcompensation mechanism of lunar impact basins. Impact basins on lunar far side are classified
into two types depending on free-air and Bouguer gravity anomalies.
Namiki, N., T. Iwata, H. Hanada, K. Matsumoto, S. Goossens, Y. Ishihara, S. Sugita, H. Noda,
S. Sasaki, and H. Araki [2009c], "Study of Compensation Mechanism of Lunar Impact Basinsfrom New Gravity and Topographic Data of Kaguya," American Astronomical Society, DPS
meeting #41, #26.03.
On the basis of the gravity model of the Moon developed by SELENE (Kaguya), we propose
new classification and compensation mechanism of lunar impact basins. Impact basins on
lunar far side and limb are classified into Type I and II basins depending on the magnitude ofcentral gravity high in free-air and Bouguer gravity anomalies. Among previously known
gravity anomalies, most typical mascons are referred as primary mascon basins. Topographic
depression and rim of both Type I and II basins show good correlation between topography
and free-air gravity anomaly suggesting elastic support of lunar lithosphere. Central gravity
high of Type I basin is inferred to be a result of mantle uplift at the time of basin formation,and is elastically supported, too. On the other hand, free-air anomalies at the center of Type II
basins are lower than Bouguer anomalies indicating brittle deformation of the basins.
Topographic depression and rim of primary mascon basins on near side of the Moon show
little to no free-air gravity anomalies. This indicates a result of elastic relaxation that occurred
probably after eruption of mare basalts. Plateau-like signature of gravity anomalies of primarymascon basins implies viscous relaxation at crust-mantle boundary beneath the basins andsignificant heat (or volatile) transport by basaltic magma.
Naruse, M., T. Ito, Y. Sekimoto, H. Toba, N. Satou, M. Sugimoto, W. Shan, Y. Iizuka, T.
Kamba, M. Kamikura, and Y. Serizawa [2009], "Near-Field Beam Pattern Measurement of
Qualification Model of ALMA Band 8 (385-500 GHz) Cartridge Receiver," Experimental
Astron., vol.24, pp.89-107.
We have developed a near-field vector beam measurement system covering the range of
frequencies from 385 to 500 GHz. The measurement set-up is capable of measurements withdynamic range exceeding 50 dB and amplitude and phase stability respectively of 0.1 dB/h and1 degree/5 min at room temperature. Beam patterns of the ALMA band 8 corrugated horns andreceiver optics block were measured at room temperature and lately compared with physical
optics calculations obtained in the far-field. Both co-polar and cross-polar beam patterns of aqualification model of the ALMA band 8 cartridge cooled in a cartridge-test cryostat have also
been measured in the near-field as a detector of a submillimeter vector network analyzer. The
measurements presented in this work refer to the lowest, middle and upper frequencies of band
8. The comparisons between software model and experimental measurements at thesefrequencies show good agreement down to -30 dB for the main polarization component. The
cross polarization level of the beam propagating through the receiver optics block was alsocharacterized. We found that a cross-polarization level better than -28 dB can be achieved at allmeasured frequencies. The measured beam pattern of this receiver corresponds to efficiency of

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greater than 92% at the sub reflector(diameter of 750 mm) of the ALMA 12 m optics.
Niinuma, K., T. Daishido, N. Matsumura, K. Takefuji, M. Kuniyoshi, K. Asuma, S. Kida, T.
Tanaka, T. Aoki, S. Ishikawa, K. Hirano, H. Uehara, and S. Nakagawa, [2009], "Discovery of
Two Radio Transients at a High Galactic Latitude in A 1.4 GHz Drift-Scan Survey," Astrophys.
J., vol.704, pp.652-660.
We report two new radio transients at high Galactic latitude, WJN J0951+3300 (α = 09h51m22s± 10s, δ = 33°00' ± 0°.4, b = 50°54.'2) and WJN J1039+3300 (α = 10h39m26s ± 10s, δ =33°00' ± 0°.4, b = 60°58.'5), which were detected by interferometric drift-scan observations at
1.4 GHz at the Waseda Nasu Pulsar Observatory. WJN J0951+3300 was detected at 16:49:32
UT on 2006 January 12 with the flux density of approximately 1760.5 ± 265.9 mJy, and WJN
J1039+3300 was detected at 17:13:32 UT on 2006 January 18 with the flux density of
approximately 2242.5 ± 228.7 mJy. Both of them lasted for a short duration (≤2 days). The
possibility that the distribution of the WJN radio transients is isotropic was suggested in aprevious study. Having re-evaluated the log N-log S relation with the addition of the two new
objects reported in this paper, we find that the slope is consistent with a slope of -1.5 and theprevious result. Additionally, although there are several counterparts to WJN radio transients,
we found that one of the quasar counterparts within the positional error of WJN J0951+3300
could be a radio-loud quasar. We have discussed whether or not WJN J0951+3300 could be ofthis quasar origin.
Nishizuka, N., H. Takasaki, A. Asai, and K. Shibata [2010], "Multiple Plasmoid Ejections andAssociated Hard X-Ray Bursts in the 2000 November 24 Flare," Astrophys. J., vol.711,
pp.1062-1072.
The Soft X-ray Telescope (SXT) on board Yohkoh revealed that the ejection of X-ray emitting
plasmoid is sometimes observed in a solar flare. It was found that the ejected plasmoid isstrongly accelerated during a peak in the hard X-ray (HXR) emission of the flare. In this paper,
we present an examination of the GOES X 2.3 class flare that occurred at 14:51 UT on 2000
November 24. In the SXT images, we found "multiple" plasmoid ejections with velocities in
the range of 250-1500 km s-1, which showed blob-like or loop-like structures. Furthermore, we
also found that each plasmoid ejection is associated with an impulsive burst of HXR emission.
Although some correlation between plasmoid ejection and HXR emission has been discussed
previously, our observation shows similar behavior for multiple plasmoid ejection such thateach plasmoid ejection occurs during the strong energy release of the solar flare. As a result of
temperature-emission measure analysis of such plasmoids, it was revealed that the apparent
velocities and kinetic energies of the plasmoid ejections show a correlation with the peakintensities in the HXR emissions.
Niwa, T., K. Tachihara, Y. Itoh, Y. Oasa, K. Sunada, K. Sugitani, and T. Mukai [2009],"Millimeter-Wave Survey of Molecular Clouds around the W5-East Triggered Star-Forming
Region," Astron. Astrophys., vol.500, pp.1119-1129.
Aims. We examined the physical properties of molecular clouds (morphology, column density,
number density, mass) to investigate the mechanism of triggered star formation by UV
radiation from a massive star.
Methods. We made extensive, high-resolution maps of molecular clouds associated andinteracting with the W5-East H II region using the 45-m telescope at the Nobeyama Radio
Observatory (HPBW= 15".)) in 13CO (J=1-0) and C18O (J=1-0) to reveal details in thehigh-density regions of the molecular clouds. In addition, to investigate the spatial
distributions of young stellar objects (YSOs) in the W5-East H II region, we mapped thespatial distributions of Class I and II candidates.
Results. We identified eight 13CO molecular clouds (three of them are known bright-rimmed
clouds) and nine C18O clumps. The masses of the clouds and clumps range from 460 to 36 000

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M⦿and from 55 to 740 M⦿, respectively. The peak 13CO column densities of the clouds facing
the H II region are twice as large as the others. They have steep density gradients toward the H
II region, indicating interactions with the H II region. We selected 55 Class I candidates and
778 Class II candidates associated with the W5-East H II region from the previous Spitzer
IRAC/MIPS survey. Most Class I candidates are located around integrated intensity peaks of
13
CO, whereas most Class II candidates are distributed along the front sides of the BRC arcs
close to the exciting star.
Conclusions. The alignments of the YSO candidates and the molecular clouds in order of age
indicate that triggered star formation occurs in the W5-East H II region as a result of gas
compression by strong UV radiation. Based on the column densities of 13CO and the spatial
distribution of YSO candidates, we identified a new bright-rimmed cloud candidate on thewest side of the W5-East H II region.
Noda, H., H. Araki, S. Tazawa, Y. Ishihara, Laser Altimeter (Lalt) in Migita, E. Kaguya, N.
Kawano, T. Tsubokawa, I. Kamiya, S. Sasaki, and J. Oberst [2008a], "The First Global Lunar
Topography Mapping by KAGUYA (SELENE) Laser Altimeter (LALT)," 37th COSPAR
Scientific Assembly, held 13-20 July 2008, in Montreal, Canada, p.2245.
The Laser ALTimeter(LALT) aboard Japanese lunar explorer KAGUYA(SELENE) is aranging instrument which measures the distance between the satellite and the lunar surface
with accuracy of 1 m by detecting the timing delay of the reflected laser light. As KAGUYA is
in a polar circular orbit, the first global and precise topographic map will be produced.
Especially, data at high latitude regions above 75 degree are collected for the first time. LALT
data are useful to determine the lunar global figure, especially center-of-mass andcenter-of-figure offset, and to estimate the thickness of the lunar crust in combination withgravity field data obtained by RSAT/VRAD gravity field measurement. It also provides basic
information for the exploration of the lunar polar area. Also, intensity of the returned pulses
contains information concerning inclination and roughness of the footprints, which contributes
to the study of the lunar surface maturity and age. The LALT started normal operation on 30th,
December 2007 after two months' commissioning phase. Measurements have been done withrepetition rate of 1 Hz except the period of unloading of the momentum wheels. As of the
middle of Februrary 2008, a first topographic grid has been accomplished for all areas whichcurrently has a grid spacing of 0.05 degrees (=1.5 km) alongtrack and 0.5 degrees across-tracknear the equator. Especially, data density at high latitude regions is sufficient to produce
detailed elevation map, which is useful to study the illumination condition of the polar regions.
In our talk, the status of the LALT and initial results of the data analysis will be presented.
Noda, H., H. Araki, S. Goossens, Y. Ishihara, K. Matsumoto, S. Tazawa, N. Kawano, and S.
Sasaki [2008b], "Illumination Conditions at the Lunar Polar Regions by KAGUYA(SELENE)
Laser Altimeter," Geophys. Res. Letters, vol.35, pp.L24203 (1 of 5).
The sunlit conditions of the lunar polar regions were estimated by using a digital elevation
model made by the laser altimeter data onboard the Japanese lunar orbiter KAGUYA(SELENE). The result shows that i) there are no peaks of eternal light in either north or southpolar regions, ii) most continuously lit surfaces are 89% for north and 86% for south, iii) there
are permanently shadowed regions. These information will be useful for the long-durable
landing experiments on the Moon and possibly for the human activity on the Moon in the near
future.
Noda, H., H. Arakai, Y. Ishihara, S. Tazawa, S. Sasaki, and N. Kawano [2009], "Lunar Surface
Reflectance by LALT aboard Kaguya," American Geophysical Union, Fall Meeting 2009,
abstract #P23C-1283.
The Laser Altimeter (LALT) aboard Japanese lunar explorer KAGUYA (SELENE) is a ranging
instrument which measures the distance between the satellite and the lunar surface with

accuracy of 1 m by detecting the timing delay of the reflected laser light. The main science
goal of the LALT is to obtain the lunar global topographic data including polar regions for the
study of the origin and the evolution of the Moon [1]. Besides, the LALT is equipped with anintensity monitor of the returned pulses. The intensity of the returned pulses contains
information concerning surface roughness and reflectance of the footprints, which willcontribute to the study of the lunar surface maturity and age. The reflectance at LALT
wavelength (1064nm) is sensitive to the surface maturity and composition. The data should beparticularly important at lunar polar regions where camera instruments should suffer fromphase angle effects in the surface reflectance and moreover cannot obtain reflectance data at
the permanently shadowed area. The normal operation of the LALT began on 30th, December
2007 after two months ﾕ commissioning phase. Before the end of the normal operation phasein October 2008, the LALT measured more than 10 million range data. Unfortunately, due tothe laser power decrease and also possible smaller surface reflectance than the expected value
before launch (15 % at 1 micro meter), the return pulse intensity during the nominal mission
phase is so small that they are not reliable enough to discuss the surface property. During theextended mission phase, which started November 2008, the satellite altitude decreased to 50
km. Due to the malfunction of the reaction wheel and high-voltage instruments were shutdown,
the observation was suspended until 11th of February, 2009. LALT successfully resumed
observation on 12th February and continued observation until the controlled crash of
KAGUYA onto the Moon on 10th of June, 2009. Thanks to the lower orbit during this phase,the return pulse intensity is high enough to be used for the study of the surface property.
Especially, it is of interest whether water ice exists or not on the bottom of the eternal shaded
regions in the polar region. If we assume that the surface roughness within the size of the
footprint is the same inside and the vicinity of a crater, the change of the intensity is due to thevariety of the reflectance. It can be used for possible detection of the water ice if exists. We
will report the initial results of the analysis of derived reflectance, especially of the lunar polar
regions. references [1] H. Araki et. al., Science, 323, 897-900 (2009).
Nyman, L.-Å., P. Andreani, J. Hibbard, and S. K. Okumura [2010], "ALMA Science
Operations,Observatory Operations: Strategies, Processes, and Systems III." Edited by Silva,
David R.; Peck, Alison B.; Soifer, B. Thomas. Proceedings of the SPIE, vol.7737,
pp.77370G-77370G-7.
The ALMA (Atacama Large Millimeter/submillimeter Array) project is an international
collaboration between Europe, East Asia and North America in cooperation with the Republicof Chile. The ALMA Array Operations Site (AOS) is located at Chajnantor, a plateau at analtitude of 5000 m in the Atacama desert in Chile, and the ALMA Operations Support Facility(OSF) is located near the AOS at an altitude of 2900 m. ALMA will consist of an array of 66
antennas, with baselines up to 16 km and state-of-the-art receivers that cover all theatmospheric windows up to 1 THz. An important component of ALMA is the compact array of
twelwe 7-m and four 12-m antennas (the Atacama Compact Array, ACA), which will greatly
enhance ALMA's ability to image extended sources. Construction of ALMA started in 2003
and will be completed in 2013. Commissioning started in January 2010 and Early Science
Operations is expected to start during the second half of 2011. ALMA science operations isprovided by the Joint ALMA Observatory (JAO) in Chile, and the three ALMA Regional
Centers (ARCs) located in each ALMA region - Europe, North America and East Asia. ALMA
observations will take place 24h per day, interrupted by maintenance periods, and will be donein service observing mode with flexible (dynamic) scheduling. The observations are executedin the form of scheduling blocks (SBs), each of which contains all information necessary toschedule and execute the observations. The default output to the astronomer will be
pipeline-reduced images calibrated according to the calibration plan. The JAO is responsible

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for the data product quality. All science and calibration raw data are captured and archived in
the ALMA archive, a distributed system with nodes at the OSF, the Santiago central office andthe ARCs. Observation preparation will follow a Phase 1/Phase 2 process. During Phase 1,
observation proposals will be created using software tools provided by the JAO and submitted
for scientific and technical review. Approved Phase 1 proposals will be admitted to Phase 2
where all observations will be specified as SBs using software tools provided by the JAO. User
support will be done at the ARCs through a helpdesk system as well as face-to-face support.
Oasa, Y., M. Tamura, K. Sunada, and K. Sugita [2008], "Luminosity and Mass Functions at the
Very Low Mass Side in NGC 1333," Astron. J., vol.136, pp.1372-1387.
We present the results of a deep near-infrared (NIR) imaging survey searching for very low
mass young stellar objects (YSOs) in the embedded cluster associated with the Perseus
molecular cloud. Our observations cover an area of ~5'x 5' in the NGC 1333-S region at J-, H-,
and Ks-bands. The 10 limiting magnitudes exceed 18 mag in all three bands. Based on NIR
color-color diagrams, embedded YSO candidates were identified using NIR excesses. The
derived frequency of these YSO candidates with NIR excess emission among all the detectedsources is 58+10-13%. The higher frequency of YSOs with NIR excesses implies that NGC 1333
is an active and young star-forming region. Approximately half of the YSO candidates exhibit
extremely low luminosity, indicating very low mass. Combining the reddening-corrected
luminosity with theoretical evolutionary models, the low-luminosity YSO candidates are
considered to be young substellar-mass objects. Furthermore, some sources could haveplanetary masses. In addition, we carried out CO molecular-line observations of the samecloud region. The results suggested that the YSO candidates are likely formed on the side of
the parent molecular cloud and star-formation activity could be high. The K-band luminosity
function of all the detected sources revealed a significant population of extremely
low-luminosity sources in NGC 1333. The reddening-corrected J-band luminosity function of
the YSO candidates does not clearly decline to the completeness limit and seems to be bimodal.
We also argue that the fraction of substellar objects is larger than those in other young clusters
and the mass function of the YSO candidates appears to be increasing toward thesubstellar-mass regime, similar to that of dust clumps. It implies that substellar-mass
distributions may depend on the initial conditions of the molecular cloud.
Oh, C. S., H. Kobayashi, M. Honma, T. Hirota, K. Sato, and Y. Ueno [2010], "VERA
Observations of H2O Maser Sources in Three Massive Star-Forming Regions and Galactic
Rotation Measurements," Publ. Astron. Soc. Japan, vol.62, pp.101-114.
We present the results of VLBI observations of three H2O maser sources in massive
star-forming regions: IRAS 06058+2138, IRAS 19213+1723, and AFGL 2789. We determined
the annual parallaxes and proper motions for these sources by a phase-referencing method. The
estimated distances to IRAS 06058+2138 and AFGL 2789 are 1.76±0.11 kpc and 3.07±0.30
kpc, which are located in the Perseus spiral arm. The distance to IRAS 19213+1723 is
3.98±0.57 kpc, placing it in the Carina-Sagittarius arm. With estimated 3-dimensional velocity
components, we have shown that the galactic rotation curve is flat in the range of 6.4 kpc≤ R ≤13 kpc as combining with S 269, which was observed with VERA. We have also foundthat the overall rotation curve of the Galaxy do not depend on Θ0 . The maser sources also
show deviations from flat rotation curves by a few kilometers per second. We discuss possible
reasons for these peculiar motions.
Ohama, A., J. R. Dawson, N. Furukawa, A. Kawamura, N. Moribe, H. Yamamoto, T. Okuda, N.
Mizuno, T. Onishi, H. Maezawa, T. Minamidani, A. Mizuno, and Y. Fukui [2010],"Temperature and Density Distribution in the Molecular Gas Toward Westerlund 2: Further
Evidence for Physical Association," Astrophys. J., vol.709, pp.975-982.
Furukawa et al. reported the existence of a large mass of molecular gas associated with the

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super star cluster Westerlund 2 and the surrounding HII region RCW49, based on a strong
morphological correspondence between NANTEN2 12CO(J = 2-1) emission and Spitzer IRAC
images of the HII region. We here present temperature and density distributions in theassociated molecular gas at ~3.5 pc resolution, as derived from a large velocity gradientanalysis of the 12CO(J = 2-1), 12CO(J = 1-0), and 13CO(J = 2-1) transitions. The kinetic
temperature is as high as ~60-150 K within a projected distance of ~5-10 pc from Westerlund 2
and decreases to as low as ~10 K away from the cluster. The high temperature provides robust
verification that the molecular gas is indeed physically associated with the HII region,
supporting Furukawa et al.'s conclusion. The derived temperature is also roughly consistent
with theoretical calculations of photodissociation regions (PDRs), while the low spatial
resolution of the present study does not warrant a more detailed comparison with PDR models.
We suggest that the molecular clouds presented here will serve as an ideal laboratory to test
theories on PDRs in future higher resolution studies.
Ohishi, M. [2008], "Molecular Spectral Line Syrveys and the Organic Molecules in theInterstellar Molecular Clouds," Proc. of the IAU Symp. 251, "Organic Matter in Space", eds. S.
Kwok, and S. Sandford, pp.17-26.
It is known that more than 140 interstellar and circumstellar molecules have so far been
detected, mainly by means of the radio astronomy observations. Many organic molecules arealso detected, including alcohols, ketons, ethers, aldehydes, and others, that are distributed
from dark clouds and hot cores in the giant molecular clouds. It is believed that most of theorganic molecules in space are synthesized through the grain surface reactions, and areevaporated from the grain surface when they are heated up by the UV radiation from adjacentstars.
On the other hand the recent claim on the detection of glycine have raised an important issue
how difficult it is to confirm secure detection of weak spectra from less abundant organic
molecules in the interstellar molecular cloud.
I will review recent survey observations of organic molecules in the interstellar molecular
clouds, including independent observations of glycine by the 45 m radio telescope in Japan,
and will discuss the procedure to securely identify weak spectral lines from organic molecules
and the importance of laboratory measurement of organic species.
Ohta, K., S. Sakamoto, N. Kawai, J. R. Cortes, K. Nakanishi, T. Okuda, K. Muraoka, T. Sakai,
H. Ezawa, N. Yamaguchi, K. Kamegai, R. Kawabe, B. Hatsukade, K. Kohno, A. Endo, and T.
Tosaki [2008], "A Possible Detection of CO(J=3-2) Emission from the Host Galaxy of
GRB980425 with the Atacama Submillimeter Telescope Experiment," Proc. of the "Mapping
the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F., p.331.
Without abstract
Ohtake, M., T. Matsunaga, J. Haruyama, Y. Yokota, T. Morota, C. Honda, Y. Ogawa, M. Torii,
H. Miyamoto, T. Arai, N. Hirata, A. Iwasaki, R. Nakamura, T. Hiroi, T. Sugihara, H. Takeda, H.
Otake, C. M. Pieters, K. Saiki, K. Kitazato, M. Abe, N. Asada, H. Demura, Y. Yamaguchi, S.
Sasaki, S. Kodama, J. Terazono, M. Shirao, A. Yamaji, S. Minami, H. Akiyama, and J.-L.
Josset, [2009], "The Global Distribution of Pure Anothosite of the Moon," Nature, vol.461,
pp.236-240.
It has been thought that the lunar highland crust was formed by the crystallization andfloatation of plagioclase from a global magma ocean, although the actual generation
mechanisms are still debated. The composition of the lunar highland crust is therefore
important for understanding the formation of such a magma ocean and the subsequentevolution of the Moon. The Multiband Imager on the Selenological and Engineering Explorer(SELENE) has a high spatial resolution of optimized spectral coverage, which should allow a
clear view of the composition of the lunar crust. Here we report the global distribution of rocks

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of high plagioclase abundance (approaching 100vol.%), using an unambiguous plagioclase
absorption band recorded by the SELENE Multiband Imager. If the upper crust indeed consistsof nearly 100vol.% plagioclase, this is significantly higher than previous estimates of
82-92vol.% (refs 2, 6, 7), providing a valuable constraint on models of lunar magma ocean
evolution.
Oka, T., T. Hasegawa, G. J. White, F. Sato, M. Tsuboi, and A. Miyazaki [2008], "Aperture
Synthesis Imaging of a High-Velocity Compact Cloud near the Valactic Center," Publ. Astron.
Soc. Japan, vol.60, pp.429-434.
We observed CO J=1-0 and HCN J=1-0 line emission toward a high-velocity, compact
molecular cloud, CO 0.02-0.02, near the center of our Galaxy, using the Nobeyama Millimeter
Array (NMA). A CO velocity-intergrated map with a resolution of 4".3 x 2".4 shows two oval
clumps with sizes of 0.8pc. These clumps are separated by 1.2pc. being located at the easternand southwestern peripheries of the CO0.02-0.02 cloud. The overall distribution of HCN
emission coincides with that taken with the Nobeyama 45m telescope. The HCN
velocity-integrated map with a resolution of 6".1 x 3".4 shows two prominent peaks in thecloud center. Both NMA maps at VLSR ~ 110 km s-1 show an arc-shaped edge in the southeast,
which may correspond to the edge of the "emission cavity" found in the CO J=3-2
integrated-intesity map. We also noticed a faint radio continuum "arc" that encircles the bulk of
the CO 0.02-0.02 cloud. These results support the notion that CO 0.02-0.02 has been
accelerated, heated, and compressed in a series of supernova shocks that occurred within thelast (3-5) x 104 yr. We suggest that a massive compact cluster with an age of 10-30 Myr is
responsible for the formation of the CO 0.02-0.02 cloud.
Okuda, T., J. Koda, K. Nakanishi, K. Kohno, S. Ishizuki, N. Kuno, and S. K. Okumura [2008a],"Nuclear Molecular Gas and Star Formation in Nearby Early-Type Spiral Galaxies," Proc. ofthe "Mapping the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F., p.368.
Without abstract
Okuda, T., and S. Iguchi [2008b], "Performance Measurements of 8-Gsps 1-bit ADCs
Developed for Wideband Radio Astronomical Observations," Publ. Astron. Soc. Japan, vol.60,
pp.315-325.
8-Gsps 1-bit Analog-to-Digital Converters (ADCs) were newly developed toward therealization of the wideband observation. The development of the wideband ADCs is one of themost essential developments for the radio interferometer. To evaluate its performance ininterferometric observations, the time (phase) stability and frequency response were measured
with a noise source and a signal generator. The results of these measurements show that thedeveloped ADCs can achieve the jitter time less than 0.05 ps at a time interval of 1 second, apassband frequency response with a slope less than 0.73 dB/GHz-1 and the ripple less than 1.8
dB, and an aperture time of less than 20 ps. The details of the developed ADC design, themeasurement methods, and the results of these measurements are presented in this paper.
Onodera, S., N. Kuno, T. Tosaki, K. Kohno, K. Nakanishi, T. Sawada, K. Muraoka, S. Komugi,
R. Miura, H. Kaneko, A. Hirota, and R. Kawabe [2010], "Breakdown of Kennicutt-Schmidt
Lawa at GMC Scales in M33," Astrophys. J. (Letters), vol.722, pp.L127-L131.
We have mapped the northern area (30'x20') of a Local Group spiral galaxy M33 in 12CO(J =1-0) line with the 45 m telescope at the Nobeyama Radio Observatory. Along with Hα andSpitzer 24μm data, we have investigated the relationship between the surface density ofmolecular gas mass and that of star formation rate (SFR) in an external galaxy(Kennicutt-Schmidt law) with the highest spatial resolution (~80 pc) to date, which iscomparable to scales of giant molecular clouds (GMCs). At positions where CO issignificantly detected, the SFR surface density exhibits a wide range of over four orders ofmagnitude, from ΣSFR ∼ 10-10 to ~10-6 M∼ yr-1 pc-2, whereas the ΣH2 values are mostly within

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10-40 M∼ pc-2. The surface density of gas and that of SFR correlate well at an ~1 kpc
resolution, but the correlation becomes looser with higher resolution and breaks down at GMC
scales. The scatter of the ΣSFR-ΣH2 relationship in the ~80 pc resolution results from the variety
of star-forming activity among GMCs, which is attributed to the various evolutionary stages of
GMCs and to the drift of young clusters from their parent GMCs. This result shows that theKennicutt-Schmidt law is valid only in scales larger than that of GMCs, when we average thespatial offset between GMCs and star-forming regions, and their various evolutionary stages.
Reid, M. J., K. M. Menten, X. W. Zheng, A. Brunthaler, L. Moscadelli, Y. Xu, B. Zhang, M.
Sato, M. Honma, T. Hirota, K. Hachisuka, Y. K. Choi, G. A. Moellenbrock, and A. Bartkiewicz[2009], "Trigonometric Parallaxes of Massive Star Forming Regions: VI. Galactic Structure,
Fundamental Parameters and Non-Circular Motions," Astrophys. J., vol.700, pp.137-148.
We are using the Very Long Baseline Array and the Japanese VLBI Exploration of Radio
Astronomy project to measure trigonometric parallaxes and proper motions of masers found in
high-mass star-forming regions across the Milky Way. Early results from 18 sources locate
several spiral arms. The Perseus spiral arm has a pitch angle of 16° ± 3°, which favors four
rather than two spiral arms for the Galaxy. Combining positions, distances, proper motions,and radial velocities yields complete three-dimensional kinematic information. We find thatstar-forming regions on average are orbiting the Galaxy ≈15 km s-1 slower than expected forcircular orbits. By fitting the measurements to a model of the Galaxy, we estimate the distanceto the Galactic center R0 = 8.4 ± 0.6 kpc and a circular rotation speed Θ0 = 254 ± 16 km s-1.
The ratio Θ0/R0 can be determined to higher accuracy than either parameter individually, andwe find it to be 30.3 ± 0.9 km s-1 kpc-1, in good agreement with the angular rotation rate
determined from the proper motion of Sgr A*. The data favor a rotation curve for the Galaxy
that is nearly flat or slightly rising with Galactocentric distance. Kinematic distances are
generally too large, sometimes by factors greater than 2; they can be brought into better
agreement with the trigonometric parallaxes by increasing Θ0/R0 from the IAU recommended
value of 25.9 km s-1 kpc-1 to a value near 30 km s-1 kpc-1. We offer a "revised" prescription for
calculating kinematic distances and their uncertainties, as well as a new approach for defining
Galactic coordinates. Finally, our estimates of Θ0 and Θ0/R0, when coupled with direct
estimates of R0, provide evidence that the rotation curve of the Milky Way is similar to that of
the Andromeda galaxy, suggesting that the dark matter halos of these two dominant Local
Group galaxy are comparably massive.
Reznikova, V. E., V. F. Melnikov, K. Shibasaki, S. P. Gorbikov, N. P. Pyatakov, I. N. Myagkova,
and H. Ji [2009a], "Dynamics of Microwave Brightness Distribution in the Giant 24 August
2002 Flare Loop," Proc. of the IAU Symp. 257, "Universal Heliophysical Processes", eds. N.
Gopalswamy and David F. Webb, pp.345-347.
We have found a similar tendency of the spatial dynamics at 34 GHz for all major temporal
sub-peaks of the burst with the re-distribution of the brightness from the footpoints (on therising phase of each peak) to the upper part of the loop (on the decay phase). Observed
dynamics is interpreted by the re-distribution of accelerated electrons number density with
their relative enhancement in the loop top. Results of diagnostics show that the ratio of
non-thermal electron number density in the loop top and in the footpoint changes 7 times fromthe peak to decay phase. Model simulations by solving the Fokker-Planck equation allowed todetermine an injection type which is able to result in necessary dynamics of energetic
electrons.
Reznikova, V. E., V. F. Melnikov, K. Shibasaki, S. P. Gorbikov, N. P. Pyatakov, I. N. Myagkova,
and H. Ji [2009b], "2002 August 24 Limb Flare Loop: Dynamics of Microwave Brightness
Distribution," Astrophys. J., vol.697, pp.735-745.
High-resolution radio observation of Nobeyama Radioheliograph at 17 and 34 GHz allowed

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studying the dynamics of microwave brightness distribution along the giant limb flaring loop
in the event of 2002 August 24. It is found that on the rising phase of the radio burst thebrightness distribution was highly asymmetric, with a strong maximum near the southern
footpoint (SFP) and much weaker brightness enhancements near the loop top (LT) andnorthern footpoint. On the decay phase, the LT gradually became most bright. The similar
dynamics of brightness distribution are shown to happen for all major temporal subpeaks ofthe burst. Results of our diagnostics show two important properties: (1) the number density of
mildly relativistic electrons in the LT is much higher than near the footpoints (FPs) during rise,
maximum and decay of each major peak; and (2) the ratio of the electron number densities inthe LT and an FP increases from the maximum to decay phase. Model simulations with making
use of the nonstationary Fokker-Planck equation have allowed us to find the model explaining
the major properties of the microwave brightness distribution and dynamics. The model ischaracterized by a compact source of electrons located near the center of an asymmetricmagnetic loop; the source is nonstationary, long lasting, and injecting high-energy electrons
with the pitch-angle distribution mostly directed toward the SFP but also having a very weakisotropic component.
This easily explains the observed brightness asymmetry. The observed dynamics comes due to
two reasons: faster precipitation of electrons having their mirror points near the ends of themagnetic trap, and relatively faster decay of the lower energy electrons responsible for thegyrosynchrotron emission near the FPs with higher magnetic ﾞ eld.
Reznikova, V. E., V. Melnikov, H. Ji, and K. Shibasaki [2010], "Topology Dynamics of the
Flaring Loop System on 2005 August 22 Observed in Microwaves and Hard X-Rays," 38th
COSPAR Scientific Assembly, 18-25 July 2010, p.5.
Microwaves generated by mildly relativistic electrons allow us to trace magnetic flaring loops
in their full length including their upper parts. We take advantage of this property and study thespatial dynamics of the system of flaring loops in the 2005 August 22 flare using highres-olution microwave observations of Nobeyama Radioheliograph (NoRH) along with hard
X-ray observations of RHESSI. As complimentary data, magnetograms from SOHO/MDI, Hα
images from SMART at Hida Observatory, as well as EUV images from SOHO/EIT and
TRACE were analyzed. The flare consisted of six temporal emission peaks. During all theemission peaks, the evolution of sizes, footpoint positions and orientations of the observed
microwave loop(s) were analyzed. We have found that the Northern footpoint of the apparent
bright loop moves along the magnetic neutral line, and the position of Southern footpoint isalmost invariable so that the shear angle of the loop steadily decreases during the flare process.
The corresponding contraction of the distance between the footpoints parallel to the magnetic
neutral line is from 25 Mm to 13 Mm. After the first emission peak, the length and altitude ofthe loop are growing continuously. During the fifth emission peak we observe a jump in theloop height which re-lates to the formation of a new loop at higher altitude. The microwave
loops characteristics are compared with corresponding properties of the hard X-ray emission
for the period of RHESSI observations (after the first microwave peak). Diagnostics ofparameters of accelerated electrons and other flare parameters are fulfilled. Possible theoreticalmodels explaining the behavior of the observed flaring loop system are considered.
Rhee, M.-H., Y.-I. Byun, H. R. Kim, J. W. Choi, J. W. Yoon, J. E. An, H. J. Kim, K. H. Lee,and Y. Kan-Ya [2010], "Project SETI KOREA, Astrobiology Science Conference 2010:
Evolution and Life: Surving Catastrophes and Extremes on Earth and Beyond, LPI
Contribution No. 1538, p.5191.
We have recently launched a new SETI project in Korea. It would be one of the first SETI
project using VLBI raw data to investigate short time scale radio events. We will report current
status of the Project SETI KOREA.

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Rioja, M. J., R. Dodson, F. Colomer, V. Bujarrabal, R. Kamohara, and H. Kobayashi [2008],"VERA Astrometric Observations of 43-GHz SiO Maser towards R Leonis Minoris," Proc. of
the 9th European VLBI Network Symposium on The role of VLBI in the Golden Age forRadio Astronomy and EVN Users Meeting, September 23-16, 2008, Bologna, Italy, pp.88-90.
Oxygen-rich Asymptotic Giant Branch (AGB)stars are intense emitters of SiO maser lines at
43 GHz( J=1→0, v=1and2). The masers appear at a distance of a few stellar radii occupying amore or less circular structure. The relative position of the spots of both the v=1 and v=2 SiO
transitions is an important result in order to elucidate the nature of the pumping mechanism,and hence a unique interpretation of the observations in terms of physical underlying
conditions. VLBI observations of the SiO maser emission has been a unique tool to sample theinnermost layers of the circumstellar envelopes in AGB stars, despite the difficulties to achieve
astrometrically aligned v=1 and v=2 SiO maser maps. We present such maps, at multiple
epochs, towards R LMi, and discuss the analysis.
Romney, J. D., R. T. Schilizzi, S. T. Garrington, L. I. Gurvits, X. Hong, X., D. L. Jauncey, H.
Kobayashi, R. Porcas, R. A. Preston, C. J. Salter, A. Szomoru, M. Tsuboi, J. S. Ulvestad, and A.
R. Whitney [2008], "Division / Commission 40 / Working Global Very Long Baseline
Interferometry," Transactions IAU, vol. 4, Issue 27A, pp.342-343.
This triennium began with an action to re-create the Terms of Reference for the Working
Group Global VLBI (WG-GV). These had been lost over the years since the Group wasestablished in 1990. Fortunately, the personal archive of one long-term member yielded a copyof the original memorandum by R. D. Ekers, which was found to coincide quite well withcurrent practice and areas of interest. New Terms of Reference, based on modern conditions,were drafted and accepted by both IAU and URSI.
Saito, H., M. Saito, Y. Yonekura, and F. Nakamura [2008], "High-Resolution Studies of theMultiple-Core Systems toward Cluster-Forming Regions Including Massive Stars," Astrophys.
J. Suppl., vol.178, pp.302-329.
We present the results of C18O observations by the Nobeyama Millimeter Array toward dense
clumps with radii of 0.3 pc in six cluster-forming regions including massive (proto) stars. We
identified 171 cores, whose radius, line width, and molecular mass range from 0.01 to 0.09 pc,
0.43 to 3.33 km s-1, and 0.5 to 54.1 Msolar, respectively. Many cores with various line widths
exist in one clump, and the index of the line width-radius relationship of the cores and theparental clump differs from core to core in the clump. This indicates that the degree of
dissipation of the turbulent motion varies for each core in one clump. Although the mass of thecores increases with the line width, most cores are gravitationally bound by the externalpressure. In addition, the line width and the external pressure of the cores tend to decrease withthe distance from the center of the clump, and these dependencies may be caused by the inner
H2 density structure of the clump that affects the physical properties of the cores. Moreover,the number density of the cores and the number density of young (proto) stars have a similar
relationship to the average H2 density of the clumps. Thus, our findings suggest that the cluster
is formed in the clump through the formation of such multiple cores, whose physical properties
would have been strongly related to the H 2 density structure and the turbulent motion of theclump.
Sakai, N., T. Sakai, and S. Yamamoto [2008a], "Tentative Detection of C4H- toward the
Low-Mass Protostar IRAS 04368+2557 in L1527," Astrophys. J. (Letters), vol.673,
pp.L71-L74.
The millimeter-wave rotational emission line (J=9-8) of the negative ion, C4H-, has tentatively
been detected toward the low-mass Class 0 protostar IRAS 04368+2557 in L1527 with the
IRAM 30 m telescope. The column density of C4H- is determined to be 1.1x1010 cm-2. The[C4H-]/[C4H] ratio is found to be 6.8x10-5, which is much lower than the [C6H-]/[C6H] ratio

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(0.093). From this result, the rate coefficient for the radiative attachment reaction between C4H
and electron is estimated to be as small as 3x10-11 cm3 s-1 on the basis of the simplified
chemical model. The present observation has demonstrated the uniqueness and importance ofL1527 in searching for a new carbon-chain molecule in a star-forming region.
Sakai, N., T. Sakai, T. Hirota, and S. Yamamoto [2008b], "Abundant Carbon-Chain Molecules
toward the Low-Mass Protostar IRAS 04368+2557 in L1527," Astrophys. J., vol.672,
pp.371-381.
We have detected the high-excitation lines of carbon-chain molecules such as C4H2
(J=100,10-90,9), C4H (N=9-8, F1, F2), l-C3H2 (41,3-31,2), and CH3CCH (J=5-4, K=2) toward alow-mass star-forming region, L1527. In particular, the F1 line of C4H is as strong as 1.7 K(TMB). The rotational temperature of C4H2 is determined to be 12.3±0.8 K, which is higher
than that in TMC-1 (3.8 K). Furthermore, the column density of C4H2 is derived to be about
1/4 of that in TMC-1, indicating that carbon-chain molecules are abundant in L1527 for astar-forming region. Small mapping observations show that the C4H, C4H2, and c-C3H2
emissions are distributed from the infalling envelope to the inner part. Furthermore, we havedetected the lines of C5H, HC7N, and HC9N in the 20 GHz region. Since the carbon-chain
molecules are generally deficient in star-forming cores, the above results cannot simply be
explained by the existing chemical models. The following hypothesis is proposed. If thetimescale of the prestellar collapse in L1527 were shorter than those of the other star-forming
cores, the carbon-chain molecules could survive in the central part of the core. In addition,
regeneration processes of the carbon-chain molecules due to star formation activities would
play an important role. Evaporation of CH4 from the grain mantles would drive theregeneration processes. The present observations show new chemistry in a warm and dense
region near the protostars, which is named "warm carbon-chain chemistry (WCCC)."
Sakai, N., T. Sakai, and S. Yamamoto [2008c], "Complex Organic Molecules in an Early Stageof Protostellar Evolution," Astrophys. and Sp. Sci., vol.313, pp.153-157.
We have detected the rotational lines of HCOOCH3 toward a Class 0 low-mass protostar,
NGC1333 IRAS4B, which is reported to be extremely young according to the dynamical ageof the molecular outflow (a few 100 yr). This suggests that the complex organic molecules
appear from the very early stage of protostellar evolution. On the other hand, the complex
organic molecules are not detected in a more evolved protostar, L1527. We have also found asimilar trend in a massive star forming region, NGC2264. The HCOOCH3 emission is almost
absent toward IRS1, whereas it is concentrated near MMS3, which is younger than IRS1. In
addition, the HCOOCH3 intensity peak is slightly shifted from the dust emission peak, as isseen in the Orion KL Compact Ridge, giving an important clue to solve its origin.
Sakai, N., T. Sakai, Y. Aikawa, and S. Yamamoto [2008d], "Detection of HCO+2 toward the
Low-Mass Protostar IRAS 04368+2557 in L1527," Astrophys. J. (Letters), vol.675,
pp.L89-L92.
The millimeter-wave rotational emission lines (404-303 and 505-404) of protonated carbon
dioxide, HCO+2(HOCO+), have been detected toward the low-mass Class 0 protostar IRAS
04368+2557 in L1527 with the IRAM 30 m telescope. This is the first detection of HCO+2
except for the Galactic center clouds. The column density of HCO+2 averaged over the beam
size (29") is determined to be 7.6x1010 cm, assuming a rotational temperature of 12.3 K. The
fractional abundance of gaseous CO2 relative to H2 is estimated from the column density of
HCO+2 with the aid of a simplified chemical model. If the HCO+2 emission only comes fromthe evaporation region of CO2 near the protostar (T >/~ 50 K), the fractional abundance of CO2
is estimated to be higher than 6.6x10-4. This is comparable to the elemental abundance ofcarbon in interstellar clouds, and hence, the direct evaporation of CO2 from dust grain isunrealistic as a source of gaseous CO2 in L1527. A narrow line width of HCO+2 also supports

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this. On the other hand, the fractional abundance of CO2 is estimated to be 2.9x10-7, if thesource size is comparable to the beam size. These results indicate that gaseous CO2 is abundanteven in the low-mass star-forming region. Possible production mechanisms of gaseous CO2 are
discussed.
Sakai, N., T. Sakai, T. Hirota, M. Burton, and S. Yamamoto [2009], "Discovery of the Second
Warm Carbon-Chain-Chemistry Source, IRAS15398-3359 in Lupus," Astrophys. J., vol.697,
pp.769-786.
We have conducted a search for carbon-chain molecules toward 16 protostars with the Mopra
22 m and Nobeyama 45 m telescopes, and have detected high excitation lines from several
species, such as C4H (N = 9-8), C4H2(J = 100,10-90,9), CH3CCH(J = 5-4, K = 2), and HC5N(J =32-31), toward the low-mass protostar, IRAS15398 - 3359 in Lupus. The C4H line is as brightas 2.4 K measured with the Nobeyama 45 m telescope. The kinetic temperature is derived tobe 12.6 ± 1.5 K from the K = 1 and K = 2 lines of CH3CCH. These results indicate that the
carbon-chain molecules exist in a region of warm and dense gas near the protostar. The
observed features are similar to those found toward IRAS04368+2557 in L1527, which shows
warm carbon-chain chemistry (WCCC). In WCCC, carbon-chain molecules are produced
efficiently by the evaporation of CH4 from the grain mantles in a lukewarm region near the
protostar. Our data clearly indicate that WCCC is no longer specific to L1527, but occurs in
IRAS15398 - 3359. In addition, we draw attention to a remarkable contrast between WCCC
and hot corino chemistry in low-mass star-forming regions. Carbon-chain molecules are
deficient in hot corino sources like NGC1333 IRAS4B, whereas complex organic molecules
seem to be less abundant in the WCCC sources. A possible origin for such source-to-source
chemical variations is suggested to arise from the timescale of the starless-core phase in eachsource. If this is the case, the chemical composition provides an important clue to explore thevariation of star formation processes between sources and/or molecular clouds.
Sakai, N., O. Saruwatari, T. Sakai, S. Takano, and S. Yamamoto [2010a], "Abundance
Anomaly of the 13C Species of CCH," Astron. Astrophys., vol.512, pp.A31(1-10).
Aims. We have observed the N = 1-0 lines of CCH and its 13C isotopic species toward a cold
dark cloud, TMC-1 and a star-forming region, L1527, to investigate the 13C abundances andformation pathways of CCH.
Methods. The observations have been carried out with the IRAM 30 m telescope.
Results. We have successfully detected the lines of 13CCH and C13CH toward the both sources
and found a significant intensity difference between the two 13C isotopic species. The [C13CH]/[13CCH] abundance ratios are 1.6 ± 0.4 (3σ) and 1.6 ± 0.1 (3σ) for TMC-1 and L1527,
respectively. The abundance difference between C13CH and 13CCH means that the two carbon
atoms of CCH are not equivalent in the formation pathway. On the other hand, the[CCH]/[C13CH] and [CCH]/[13CCH] ratios are evaluated to be larger than 170 and 250 toward
TMC-1, and to be larger than 80 and 135 toward L1527, respectively. Therefore, both of the13
C species are significantly diluted in comparison with the interstellar 12C/13C ratio of 60. The
dilution is discussed in terms of a behavior of 13C in molecular clouds.
Sakai, N., T. Shiino, T. Hirota, T. Sakai, and S. Yamamoto [2010b], "Long Carbon-Chain
Molecules and Their Anions in the Starless Core, Lupus-1A," Astrophys. J. (Letters), vol.718,
pp.L49-L52.
We have recently discovered a new starless core with bright radio emissions of longcarbon-chain molecules in the Lupus molecular cloud, which we have named as Lupus-1A.
Toward this source, the peak intensities of the C6H and C8H lines are found to be higher than
toward TMC-1 by a factor of 2-3. Even the lines of their anions, C6H- and C8H-, are alsobrighter than in TMC-1. Moreover, the line of C4H- has been detected for the first time in astarless core. The column densities of these long carbon-chain molecules are almost

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comparable to those in TMC-1, and hence, this source can be regarded as the second "TMC-1
like cloud." TMC-1 has long been an outstanding molecular cloud with rich carbon-chain
molecules since its discovery in 1976. In spite of extensive efforts, no comparable sources
have been found so far. Lupus-1A will be used for hunting of new interstellar molecules aswell as understanding of carbon-chain chemistry through critical comparison of physical andchemical properties with TMC-1. This source is important not only for astronomy but also formolecular science as an ideal spectroscopic laboratory because of narrow line shapes andbright intensities.
Sakai, T., N. Sakai, K. Kamegai, T. Hirota, N. Yamaguchi, S. Shiba, and S. Yamamoto [2008],"A Molecular Line Observation toward Massive Clumps Associated with Infrared Dark
Clouds," Astrophys. J., vol.678, pp.1049-1069.
We have surveyed the N2H+ J=1-0, HC3N J=5-4, CCS JN=43-32, NH3 (J, K) = (1, 1), (2, 2), (3,3), and CH3OH J=7-6 lines toward the 55 massive clumps associated with infrared dark clouds
by using the Nobeyama Radio Observatory 45 m telescope and the Atacama Submillimeter
Telescope Experiment 10 m telescope. The N2H+, HC3N, and NH3 lines are detected toward
most of the objects. On the other hand, the CCS emission is detected toward none of theobjects. The [CCS]/[N2H+] ratios are found to be mostly lower than unity even in the Spitzer
24μm dark objects. This suggests that most of the massive clumps are chemically more
evolved than the low-mass starless cores. The CH3OH emission is detected toward 18 out of
55 objects. All the CH3OH-detected objects are associated with the Spitzer 24μm sources,
suggesting that star formation has already started in all the CH3OH-detected objects. The
velocity widths of the CH3OH JK=70-60 A+ and 7-1-6-1 E lines are broader than those of N2H+
J=1-0. The CH3OH JK=70-60 A+ and 7-1-6-1 E lines tend to have broader line width in the MSX
dark objects than in the others, the former being younger or less luminous than the latter. The
origin of the broad emission is discussed in terms of the interaction between an outflow and an
ambient cloud.
Sakai, T., N. Sakai, T. Hirota, and S. Yamamoto [2010], "A Survey of Molecular Lines Toward
Massive Clumps in Early Evolutionary Stages of High-Mass Star Formation," Astrophys, J.,
vol.714, pp.1658-1671.
We have observed the CH3OH J = 2-1, SiO J = 2-1, C34S J = 2-1, H13CO+ J = 1-0, HN13C J =1-0, CCH N = 1-0, OCS J = 8-7, and SO JN = 22-11 lines toward 20 massive clumps, including
Midcourse Space Experiment (MSX) 8μm dark sources (infrared dark clouds) and MSX 8μm
sources, by using the Nobeyama Radio Observatory 45 m telescope. We have found that thevelocity widths of the CH3OH and C34S lines are broader than those of the H13CO+ line in the
MSX dark sources. On the other hand, they are comparable to the velocity width of the
H13CO+ line in the MSX sources. In addition, the [SiO]/[H13CO+] abundance ratio is found to
be enhanced in the MSX dark sources in comparison with the MSX sources. These results
suggest that shocks caused by interaction between an outflow and an ambient dense gas would
have substantial impact on the chemical composition of the MSX dark sources. The velocity
widths of the CH3OH and C34S lines relative to that of the H13CO+ line as well as the[SiO]/[H13CO+] abundance ratio could be used as good tools for investigating evolutionary
stages of massive clumps. On the basis of the results, we discuss the chemical and physicalevolution of massive clumps.
Sakao, T., S. Tsuneta, M. Shimojo, N. Narukage, R. Kano, T. Obara, S. Watari, and Hinode
Team [2009], "A New View of the Sun with Hinode Mission," Trans. JSASS Space Tech.
Japan, vol.7, pp.Tr.2-15-Tr.2-19.
We present highlights of observations of the Sun with Japanese Hinode mission launched by
JAXA in September 2006. The scientific objective of Hinode mission is to observe, in an
unprecedented detail, a wide variety of plasma activities in the Sun's corona together with

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magnetic activities on the photosphere and in the chromosphere, utilizing a suite of threestate-of-the-art telescopes; Solar Optical Telescope (SOT), X-Ray Telescope (XRT), and EUV
Imaging Spectrometer (EIS). Since the beginning of the observations late in October 2006,
Hinode has been providing ample information on activities of magnetized plasmas in the solar
atmosphere some of which are totally new to us. In this article, we present an overview of the
Hinode mission as well as some highlights of the observations.
Sako, N., M. Shimojo, and T. Kitabayashi [2010[, "Statistical Study of the Polar X-Ray Jets,”
38th COSPAR Scientific Assembly, 18-25 July 2010, p.4.
The X-Ray Telescope(XRT) abroad Hinode had revealed that X-ray jets in the polar region
occur at the high frequency. Savcheva et al. (2007) studied 104 X-ray jets occurred around thesouth pole and reported the parameters of the jets. However, their study included only the
X-ray jets that occurred in the coronal hole. In order to reveal the properties of the polar X-ray
jets in not only the coronal hole but also the quiet region, we detected 870 polar X-ray jets
occurred around the north pole, and investigated the jets statistically. The 470 jets in the 848
events occurred in the coronal hole. The occurrence rate of the jets in the coronal hole and thequiet sun is 5.04x10-12 jets/hr/km2 and 7.66x10-12 jets/hr/km2, respectively. It shows that thequiet region is more productive of X-ray jets than the coronal hole. We derived five parametersof the polar X-ray jets, and the average of the parameters are 2.91x104 km for the maximum
length, 4.42x103 km for the width, and 180 km/sec for the apparent velocity. The lifetime andlength scale of the jets in this result is smaller than that in Savcheva et al. (2007). The reason
for these differences is that we could detect smaller jets than the previous work because weused not only X-ray intensity images but also the running difference images for detecting thejets. We derived also the frequency distributions of the parameters and found thatthe frequency
distributions of the lifetime and the X-ray intensity of the footpoint flare show the power-raw
distribution. The power-law index of the lifetime is -4.22±0.36, and it is smaller than theindex(-1.2) derived from the jets that occurred near the active regions(Shimojo et al. 1996).
The difference indicates that the occurrence rate of the polar X-ray jets with short lifetime islarger than that of the X-ray jets that occurred near active regions.On the other hand, thepower-raw index of the X-ray intensity of the footpoint flare is -2.04±0.27. The index issmaller than that of the X-ray jets near the active regions(Shimojo et al. 1996).
Sanhueza, P., G. Garay, L. Bronfman, D. Mardones, J. May, and M. Saito [2010], "Molecular
Outflows Within the Filamentary Infrared Dark Cloud G34.43+0.24," Astrophys. J., vol.715,
pp.18-32.
We present molecular line observations, made with angular resolutions of ~20'', toward thefilamentary infrared dark cloud G34.43+0.24 using the APEX [CO(3→2), 13CO(3→2),
C18O(3→2), and CS(7→6) transitions], Nobeyama 45 m [CS(2→1), SiO(2→1), C34S(2→1),
HCO+(1→0), H13CO+(1→0), and CH3OH(2→1) transitions], and SEST [CS(2→1) andC18O(2→1) transitions] telescopes. We find that the spatial distribution of the molecularemission is similar to that of the dust continuum emission observed with 11'' resolution
showing a filamentary structure and four cores. The cores have local thermodynamic
equilibrium masses ranging from 3.3×102 to 1.5×103 Msun and virial masses from 1.1×103 to
1.5×103 Msun, molecular hydrogen densities between 1.8×104 and 3.9×105 cm-3, and column
densities >2.0×1022 cm-2, values characteristic of massive star-forming cores. The 13CO(3→2)
profile observed toward the most massive core reveals a blue profile indicating that the core isundergoing large-scale inward motion with an average infall velocity of 1.3 km s-1 and a mass
infall rate of 1.8×10-3 Msun yr-1. We report the discovery of a molecular outflow toward thenorthernmost core thought to be in a very early stage of evolution. We also detect the presenceof high-velocity gas toward each of the other three cores, giving support to the hypothesis thatthe excess 4.5μm emission ("green fuzzies") detected toward these cores is due to shocked gas.

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The molecular outflows are massive and energetic, with masses ranging from 25 to 80 Msun,
momentum 2.3-6.9×102 Msun km s-1, and kinetic energies 1.1-3.6×103 Msun km2 s-2,
indicating that they are driven by luminous, high-mass young stellar objects.
Sasaki, S., and T. Hiroi [2008a], "How Does Space Weathering Depend on the Surface
Condition of Airless Bodies (Asteroids, the Moon, and Mercury)?," 39th Lunar and Planetary
Science Conference, (Lunar and Planetary Science XXXIX), held March 10-14, 2008 in
League City, Texas. LPI Contribution No. 1391., p.1625.
Itokawa suggested that the rocky small asteroids should be weathered although they lackregolith. On Mercury, surface mixing probably caused by impacts would have weakened theweathering although it is covered with regolith.
Sasaki, S., T. Iwai, K.-I. Nogami, R. Srama, E. Gruen, H. Ohashi, T. Hirai, T. Yamamoto, M.
Fujii, and H. Shibata [2008b], "Development of Plane Parallel Impact-Ionization Dust/Debris
Detector," 37th COSPAR Scientific Assembly, held 13-20 July 2008, in Montreal, Canada,p.2740.
In-situ measurement of dust and small debris particles in space is important to study the origin
or those particles. Especially to examine the time variation of dust/debris flux, relatively large
sensor aperture (> 500cm2 ) is necessary for dust/debris measurement at LEO. We have beendeveloping light-weight large-area dust detectors for space. Impact-ionization dust detectors on
board HITEN and NOZOMI had a box-shape where volume/mass of a detector should belarger as increasing the target area. We have developed plane-parallel type detectors with atarget plate and entrance grids. So far we tested three models with different target diameters:
5cm, 15cm, 30cm. In these types, volume/mass of a detector is basically proportional to its
sensor area. A detector consists of a target plate and two grids. Electrons from
impact-generated plasma are collected by the target and positive ions from the plasma are
attracted by the inner grids. Detected charge signals at the target and grids are amplified andstored. Using the total charge and rise time of plasma signals, we can obtain information on
mass and velocity of impacted particles. Using van de Graff dust accelerators at Univ. Tokyo
and Max-Planck Institute Kernphysik, we have done experiments of irradiation of micron size
dust particles. Typical speed of impact velocity is 4-20km/s. A few of faster particles were alsomeasured. Particles of Ag, Fe, C, and latex polymer have been irradiated. We have confirmed
relationships between the total charge and dust mass, and between the charge rise time andimpact velocity. The detector can measure mass and velocity of micron-size dust particles inspace. Currently we are planning to measure dust and debris particles at LEO using the surface
unit on board the Space Station.
Sasaki, S., Y. Ishihara, H. Noda, H. Araki, Laser Altimeter (Lalt) in Emiko Migita, Kaguya,
and S. Tazawa [2008c], "KAGUYA Laser Altimeter (LALT) Initial Results on Lunar Impact
Structures," 37th COSPAR Scientific Assembly, held 13-20 July 2008, in Montreal, Canada,p.2739.
The main orbiter of Japanese lunar explorer KAGUYA(SELENE) has laser altimeter (LALT)
which measures the distance between the orbiter and the lunar surface. Detecting the delay
time of reflecting laser pulse from the surface, LALT can determine the lunar topography withthe accuracy better than 5m. After the initial checkout of the instrument, LALT started thenominal continuous observation on 30 December 2007 and it scanned the whole lunar surface
once by mid January 2008. KAGUYA LALT can detect reflected signals day and night.
Therefore LALT can scan the lunar globe in a half month. By late June, we will have 12 times
scans of the lunar surface. At that time, the spatial resolution will be 2.4km at the equator in
the longitudinal direction. Since pulse frequency is 1 second, the resolution in the latitudinal
direction is 1.5km. The spatial resolution will be one order of magnitude better than that of
Clementine altimeter. Also LALT covers high-latitude and polar regions where Clementine

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LIDAR did not obtain data. LALT can clarify the presence and shape of craters as well as large
impact structure. Previously unresolved heights of central peaks of large craters are obtained.
Within the farside highland, several large impact structures show multi-ring morphologies
some of which are obscure. The farside impact structures would be corresponding to gravity
patterns, which will be also obtained by KAGUYA gravity instruments. In the nearside, LALT
preliminary data would suggest hidden impact structures within the mare region.
Sasaki, S., and T. Hiroi [2008d], "Difference of Space Weathering Degree on Asteroids of
Various Sizes," Meteoritics and Planetary Sci. Suppl., 43, paper id. 5245.
Not Available
Sasaki, S., H. Araki, H. Hanada, N. Namiki, T. Iwata, K. Asari, S. Goossens, Y. Ishihara, T.
Ishikawa, N. Kawano, F. Kikuchi, Q. Liu, K. Matsumoto, H. Noda, S. Tazawa, S. Tsuruta, Y.
Harada, N. Petrova, K. Kurosawa, and S. Sugita [2008e], "Global Topography and Gravity of
the Moon Revealed by KAGUYA Mission," American Astronomical Society, DPS meeting#40, #9.01.
The Japanese lunar explorer KAGUYA (SELENE) was launched successfully on September
14th, 2007. KAGUYA has two small spin-stabilized subsatellites, Rstar (OKINA) and Vstar(OUNA) for gravity measurement. We can track the three satellites by new methods: 4-way
Doppler tracking between the main satellite and Rstar for the far-side gravity andmulti-frequency differential VLBI tracking between Rstar and Vstar. The global lunar gravity
field with unprecedented accuracy can be obtained. Through more than 6 months, precise
gravity field including most of farside was obtained. The farside gravity field shows significant
improvement from the previous model. Many circular features corresponding to impact
structures are clearly identified. Some of the circular gravity anomalies in the free-air gravity
apparently disappear in Bouguer anomaly map; the surface topography is a dominant source of
free-air gravity anomalies and large impact structures are supported by lithosphere, which
would lead to the difference of thermal history between nearside and farside. A possible
cryptomare candidate (a circular gravity anomaly without topographic signature) was also
found.
KAGUYA has a laser altimeter (LALT). The first precise global topography data with range
accuracy 5m have been produced by LALT. In the polar regions where CLEMENTINE did notcover, topographic features in the shadowed area are newly discovered. Solar illumination
condition was calculated: the region whose solar illumination rate is higher than 90% is very
limited. Lunar mean radius is 1737.15±0.01 km and the COM-COF offset is 1.94 km. The
amplitude of the power spectrum of topography spherical harmonics is larger than that of theprevious model at L>30.
From the gravity and topography data, we obtain the distribution of the crustal thickness on theMoon. We also estimate the correlation between gravity and topography and localized
admittance values. Gravity and topography observation of KAGUYA will continue until early2009.
Sasaki, S., Y. Ishihara, H. Araki, H. Noda, S. Goossens, N. Namiki, T. Iwata, H. Hanada, K.
Matsumoto, N. Kawano, F. Kikuchi, Q. Liu, Y. Harada, SELENE Gravity/Topography Group[2009a], "Lunar Topography and Crustal Thickness by KAGUYA (SELENE) Selenodesy
Observation," American Astronomical Society, DPS meeting #41, #26.02.
The Japanese lunar explorer KAGUYA (SELENE) was launched on September 14th, 2007 andcontinued its operation by June 11th, 2009. Laser altimeter(LALT) on board KAGUYA
obtained the first precise global topography data with range accuracy of 5m [1]. In the polar
regions where CLEMENTINE LIDAR could not obtain data, KAGUYA clarified topographic
features including permanently shadowed areas. Distribution of solar illumination rates was
also estimated at elevated areas [2]. The amplitude of the power spectrum of topography

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spherical harmonics is larger than that of the previous model at L>30. Using 4-way Doppler
tracking with relay satellite OKINA(Rstar), KAGUYA obtained the first precise gravity fieldof the lunar far-side [3]. Multi-frequency VLBI observation using subsatellites OKINA andOUNA(Vstar) improved the accuracy of gravity. Combined with topography data, we estimate
the crustal thickness variation of the Moon [4]. Gravity signatures of far-side impact basins aremostly explained by topography except for the central high. We have better correlation of
spherical harmonics coefficients between gravity and topography than the previous model [3].
On the far-side, obtained Bouguer anomaly distribution is relatively smooth both within South
Pole-Aitken basin (SPA) and within far-side highland terrain (FHT). This would imply
relatively smooth crust-mantle boundary there. The shape of the central SPA basin with thinnercrust is rather circular. SPA is also characterized by the admittance spectra. Although thecrustal thickness of SPA is much thinner than that FHT, the elastic thicknesses of both zones
are not so different on the basis of the admittance. SPA area would be elastically supported bya part of upper mantle.
[1] Araki, H. et al.(2009) Science 323, 892. [2] Noda et al.(2008) GRL,
doi:10.1029/2008GL035692 [3] Namiki, N. et al.(2009) Science 323, 900, [4] Ishihara, Y. etal.(2009) GRL, submitted.
Sasaki, S., N. Namiki, H. Hanada, H. Araki, T. Iwata, Y. Ishihara, K. Matsumoto, H. Noda, S.
Goossens, and Kaguya Topography/Gravity Team [2009b], "Global Topography and Gravityof the Moon Observed by KAGUYA," EPSC(European Planetary Science Congress) abstracts,
vol.4, pp.EPSC2009-547(1-2).
Not Available
Sasaki, S., Y. Ishihara, H. Araki, H. Noda, H. Hanada, K. Matsumoto, S. Goossens, N. Namiki,
T. Iwata, and M. Ohtake [2010], "Structure of the Lunar South Pole-Aitken Basin from
Kaguya (SELENE) Gravity/Topography," LPI Contribution No. 1533, p.1691.
KAGUYA gravity and topography data are used to characterize the structure of South
Pole-Aitken basin. Previously proposed elliptic basin shape was confirmed by crustal thickness.
The thinner region with 30km crust is offset from the basin center.
Sato, M., T. Hirota, M. Honma, and H. Kobayashi [2008a], "Absolute Proper Motions of Water
Masers in NGC 281 Measured with VERA," Proc. of the IAU Symp. 242, "Astrophysical
Masers and their Environments", eds. Jessica Chapman and Willem Baan, pp.170-171.
We report on absolute proper-motion measurements of H2O maser features in the NGC 281
West molecular cloud, located ~320 pc above the Galactic plane and associated with an HI
loop extending from the Galactic plane. We conducted six-epoch phase-referencing
observations of the maser source with VERA (VLBI Exploration of Radio Astrometry) over
six months since May 2006. The H2O maser features are found to be systematically moving
toward the southwest and further away from the Galactic plane with a vertical velocity of~20-30 km s-1 at its estimated distance of 2.2-3.5 kpc. Our new results provide the most direct
evidence that the gas in the NGC 281 region was blown out from the Galactic plane, most
likely in a superbubble driven by multiple or sequential supernova explosions in the Galactic
plane.
Sato, M., T. Hirota, M. Honma, H. Kobayashi, T. Sasao, T. Bushimata, Y. K. Choi, H. Imai, K.
Iwadate, T. Jike, S. Kameno, O. Kameya, R. Kamohara, Y. Kan-ya, N. Kawaguchi, M. K. Kim,
S. Kuji, T. Kurayama, S. Manabe, M. Matsui, N. Matsumoto, T. Miyaji, T. Nagayama, A.
Nakagawa, K. Nakamura, C. S. Oh, T. Omodaka, T. Oyama, S. Sakai, K. Sato, K. M. Shibata,Y. Tamura, and K. Yamashita [2008b], "Distance to NGC 281 in a Galactic Fragmenting
Superbubble: Parallax Measurements with VERA," Publ. Astron. Soc. Japan, vol.60,
pp.975-989.
We have used the Japanese VLBI array VERA to perform high-precision astrometry of an H2O

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maser source in the Galactic star-forming region NGC 281 West, which has been considered tobe part of a 300-pc superbubble. We successfully detected a trigonometric parallax of
0.355±0.030 mas, corresponding to a source distance of 2.82±0.24 kpc. Our direct distancedetermination of NGC 281 has resolved a large distance discrepancy between previous
photometric and kinematic studies; likely NGC 281 is in the far side of the Perseus spiral arm.
The source distance as well as the absolute proper motions were used to demonstrate the 3D
structure and expansion of the NGC 281 superbubble, ~650 pc in size parallel to the Galactic
disk and with a shape slightly elongated along the disk or spherical, but not verticallyelongated, indicating that the superbubble expansion may be confined to the disk. We estimate
the expansion velocity of the superbubble as being ~20 km/s-1, both perpendicular to andparallel to the Galactic disk with a consistent timescale of ~20 Myr.
Sato, M. T., and M. Tsuboi, [2009a], "SiO and H13CO+ Emission Lines Observations Toward
the Infalling Gas onto the CND at the Galactic Center," Proc. of the "Approaching
Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies", eds. Hagiwara,
Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402, pp.388-391.
The central region of our Galaxy (Sgr A*) is the nearest galactic center harboring a massive
black hole. The environment around Sgr A* is a topic of interest in diverse fields. We havestudied the gas feeding from giant molecular clouds (GMC) within 10 pc of the Galactic center
to the Circumnuclear Ring (CND), which is presumable is infalling gas toward Sgr A*. In
order to study the mechanism, we observed SiO (J=2-1 v=0) and H13CO+ (J=1-0) lines using
the Nobeyama Millimeter Array (NMA). We detected the CND clearly in SiO line. The
molecular gas in the CND rotates interactively. We observed two molecular streamers within
CND in SiO line. One is a new detection. The line intensity ratios at overlapping points of thestreamers in the CND are significantly higher (I(SiO)/I(H13CO+) > 8) than the average of otherlines in the CND (about 2-4). This is a strong evidence indicating these streamers areassociated with the CND.
Sato, M., T. Hirota, M. Honma, H. Kobayashi, and VERA Project Team [2009b], "Superbubble
Motion Away from the Galactic Plane: Astrometry of Water Masers in NGC 281 with VERA,"
Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser.
vol.402, pp.476-479.
We report on results of our parallax measurements of an H2O maser
source in the NGC 281 West molecular cloud, associated with a 300-pc fragmenting
superbubble above the Galactic plane. We have conducted multi-epoch phase-referencing
observations of the maser source with VERA (VLBI Exploration of Radio Astrometry) over 18
months year since May 2006. The parallax measurement yields a direct distance estimate of
2.82 ｱ 0.24 kpc, which agrees well with the photometric distance of 2.94 ｱ 0.15 kpc derived by
Guetter and Turner (1997) and resolves the large distance discrepancy of NGC 281 in previous
studies. We find that the H2O maser features in NGC 281 West are systematically moving
toward the southwest and further away from the Galactic plane with a vertical velocity of 20
km s 1. Our new results provide the most direct evidence for the NGC 281 superbubble
expansion is most likely driven by multiple or sequential supernova explosions in the Galactic
plane.
Sato, M., T. Hirota, M. J. Reid, M. Honma, H. Kobayashi, K. Iwadate, T. Miyaji, and SK. M.
hibata [2010], "Distance to G14.33-0.64 in the Sagittarius Spiral Arm: H2O Maser
Trigonometric Parallax with VERA," Publ. Astron. Soc. Japan, vol.62, pp.287-299.
We report on trigonometric parallax measurements for the Galactic star-forming region
G14.33-0.64 toward the Sagittarius spiral arm. We conducted multi-epoch phase-referencing
observations of an H2O maser source in G14.33-0.64 with the Japanese VLBI array VERA. We
successfully detected a parallax of π=0.893±0.101 mas, corresponding to a source distance of d

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= 1.12±0.13 kpc, which is less than half of the kinematic distance for G14.33-0.64. Our new
distance measurement demonstrates that the Sagittarius arm lies at a closer distance of ~1 kpc,
instead of the previously assumed ~2-3 kpc from the kinematic distances. The previously
suggested deviation of the Sagittarius arm toward the Galactic center from the symmetricallyfitted model (Taylor & Cordes 1993, ApJ, 411, 674) is likely due to large errors of thekinematic distances at low galactic longitudes. G14.33-0.64 most likely traces the near side of
the Sagittarius arm. We attempted to fit the pitch angle of the arm with other parallax
measurements along the arm, which yielded two possible pitch angles of i = 34°.7±2°.7 and i =11°.2±10｡.5. Our
proper-motion measurements suggest that G14.33-0.64 has no significant peculiar motion
relative to the differential rotation of the Galaxy (assumed to be in a circular orbit), indicatingthat the source motion is in good agreement with the Galactic rotation.
Sato, M. T., and M. Tsuboi [2008a], "Infallng Gas onto the Galactic Center Circumnuclear
Ring," Proc. of the "Observational Evidence for Black Holes in the Universe", AIP Conf. Proc.,vol.1053, pp.95-98.
The central region of our Galaxy (Sgr A*) is the nearest galactic center harboring a massive
black hole. The environment around Sgr A* is a topic of interest to diverse fields. We areinterested in gas feeding from giant molecular clouds (GMC) within 10 pc of the Galactic
center to the Circumnuclear Ring (CND), which is presumable Ą glay-down bay Ąh ofinfalling gas toward Sgr A*. In order to reveal the mechanism, we observed SiO J = 2-1 ν= 0
and H13CO+ J = 1-0 lines using the Nobeyama Millimeter Array (NMA). We depicted the CND
clearly in SiO line. Molecular gas in CND rotates interacting each other. We observed twomolecular streamers to CND in SiO line. One is a new detection. The line intensity ratios atoverlapping points of streamers with CND are significantly higher (I(SiO)/I(H13CO+)>8) than
the average of CND (about 2-4). This is a strong evidence indicating these streamers areconnecting to the CND.
Sato, M. T., and M. Tsuboi [2008b], "Infallng Gas onto the Galactic Center Circumnuclear
Ring," J. of Phys., Conf. Ser., vol.131, pp.012033(1-7).
The central region of our Galaxy (Sgr A*) is the nearest galactic center harboring a massive
black hole. The environment around Sgr A* is a topic of interest to diverse fields. We areinterested in gas feeding from giant molecular clouds (GMC) within 10 pc of the Galactic
center to the Circumnuclear Ring/Disk (CND), which is presumable 'lay-down bay' of infalling
gas toward Sgr A*. In order to reveal the mechanism, we observed the CND and its
surroundings in SiO and H13CO+ lines using Nobeyama Millimeter Array (NMA). We depict
the CND clearly in both lines and some molecular streamers to the CND in only SiO line
including one new detection. The line intensity ratios at overlapping points of streamers with
the CND are higher (I(SiO)/I(H13CO+) > 6) than the average of CND (2-4). This is a strong
evidence indicating these streamers are connecting to the CND. Some components at the outerregion of the CND are also detected in both lines. We also estimate the rotation velocity of the
CND as 110±10 km s-1 and of just a bit outside from the CND as 93±14 km s-1. The estimationof the rotation velocity in the distance range of 5-10 pc from the Sgr A* has a great meaning
since there have been few report about the kinematic parameters at just outside of the CND.
Satou, N., Y. Sekimoto, Y. Iizuka, T. Ito, W.-I. Shan, T. Kambe, K. Kumagai, M. Kamikura, Y.
Tomimura, Y. Serizawa, S. Asayama, and M. Sugimoto [2008], "A Submillimeter
Cartridge-Type Receiver: ALMA Band 8 (385-500GHz) Qualification Model," Publ. Astron.
Soc. Japan, vol.60, pp.1199-1207.
We have developed a cartridge-type receiver covering the frequency band of 385-500 GHz as aqualification model of Atacama Large Millimeter/submillimeter Array (ALMA) band 8. It
receives two orthogonal polarizations and down-converts the sideband-separated signals to

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intermediate frequencies (IF) of between 4 and 8 GHz. The cartridge-type receiver consists ofcold optics, two feed horns, a wire grid, mirrors, two sideband-separating SIS mixers,
cryogenic multipliers of a local oscillator (LO), cryogenic and warm IF ampliflers, a cartridge
body, and sensors/wirings. These components were individually tested, and then the cartridge
was integrated and tested as a complete assembly. We have also developed equipment for
efficiency tests of both the components and the integrated receiver. The single sideband (SSB) noise temperature of this receiver is 100 K at theband center and 300 K at the band edges. The beam pattern and cross-polarization pattern are
consistent with a physical optical calculation.
The amplitude stability is around 3x10-4 in 1 s. The phase stability is less than 2.°0 on a timescale of 0.1 s to 10 min. These results are promising for a receiver in the ALMA.
Sawada, T., J. Koda, T. Handa, M. Sugimoto, and T. Hasegawa [2008a], "NRO/CSO/ASTE
Galactic Plane CO Survey," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds.
Wada, K., and Combes, F., p.374.
Without abstract
Sawada, T., N. Ikeda, K. Sunada, N. Kuno, T. Kamazaki, K.-I. Morita, Y. Kurono, N. Koura, K.
Abe, S. Kawase, J. Maekawa, O. Horigome, and K. Yanagisawa [2008b], "On-The-Fly
Observing System of the Nobeyama 45-m and ASTE 10-m Telescopes," Publ. Astron. Soc.
Japan, vol.60, pp.445-455.
We have developed a spectral line On-The-Fly (OTF) observing mode for the Nobeyama
Radio Observatory 45-m and the Atacama Submillimeter Telescope Experiment 10-m
telescopes. Sets of digital autocorrelation spectrometers are available for OTF with heterodyne
receivers mounted on the telescopes, including the focal-plane 5x5 array receiver, BEARS, on
the 45-m. During OTF observations, the antenna is continuously driven to cover the mapped
region rapidly, resulting in high observing efficiency and accuracy. Pointing of the antenna andreadouts from the spectrometer are recorded as fast as 0.1 s. In this paper we report
improvements made to the software and instruments, requirements and optimization ofobserving parameters, data-reduction process, and verification of the system. It is confirmed
that, using optimal parameters, the OTF is about twice as the conventional position-switchobserving method.
Scott, K. S., M. S. Yun, G. W. Wilson, J. E. Austermann, I. Aretxaga, H. Ezawa, D. Ferrusca, B.
Hatsukade, D. H. Hughes, D. Iono, M. Giavalisco, R. Kawabe, K. Kohno, P. D. Mauskopf, T.
Oshima, T. A. Perera, J. Rand, Y. Tamura, T. Tosaki, M. Velazquez, and C. C. Williams [2010],"Deep 1.1 mm-Wavelength Imaging of the GOODS-S Field by AzTEC/ASTE - I. Source
Catalogue and Number Counts," Mon. Not. Roy. Astron. Soc., vol.405, pp.2260-2278.
We present the first results from a 1.1mm confusion-limited map of the Great Observatories
Origins Deep Survey-South (GOODS-S) taken with the AzTEC camera on the Atacama
Submillimeter Telescope Experiment. We imaged a 270 arcmin2 field to a 1σdepth of 0.48-0.73
mJy beam-1, making this one of the deepest blank-field surveys at mm-wavelengths everachieved. Although by traditional standards our GOODS-S map is extremely confused due to asea of faint underlying sources, we demonstrate through simulations that our source
identification and number counts analyses are robust, and the techniques discussed in thispaper are relevant for other deeply confused surveys. We find a total of 41 dusty starburst
galaxies with signal-to-noise ratios S/N ≥ 3.5 within this uniformly covered region, where only
two are expected to be false detections, and an additional seven robust source candidates
located in the noisier (1σ ≈ 1mJy beam 1) outer region of the map. We derive the 1.1mm
number counts from this field using two different methods: a fluctuation or “P(d)” analysis anda semi-Bayesian technique and find that both methods give consistent results. Our data are
well fit by a Schechter function model with (S',N3mJy, α) = (1.30+0.19-0.25 mJy, 160+27-28 mJy-1

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deg-2, -2.0). Given the depth of this survey, we put the first tight constraints on the 1.1mm
number counts at S1.1mm = 0.5 mJy, and we find evidence that the faint end of the number
counts at S850μm ∼2.0 mJy from various SCUBA surveys towards lensing clusters are biased
high. In contrast to the 870μm survey of this field with the LABOCA camera, we find noapparent underdensity of sources compared to previous surveys at 1.1 mm; the estimates of thenumber counts of SMGs at flux densities > 1 mJy determined here are consistent with thosemeasured from the AzTEC/SHADES survey. Additionally, we find a significant number of
SMGs not identified in the LABOCA catalogue. We find that in contrast to observations at
λ≤500μm, MIPS 24μm sources do not resolve the total energy density in the cosmic infrared
background at 1.1mm, demonstrating that a population of z ∼3 dust-obscured galaxies that are
unaccounted for at these shorter wavelengths potentially contribute to a large fraction (~2/3) of
the infrared background at 1.1mm.
Sekido, M., N. Kawaguchi, Y. Koyama, M. Kimura, T. Kondo, H. Takiguchi, T. Hobiger, K.
Takefuji, H. Harai, T. Ikeda, S. Shimojo, T. Oyama, T. Hara, Y. Kono, S. Kurihara, K. Kokado,
D. Tanimoto, K. Nozawa, H. Takechi, H. Uose, K. Fujisawa, and H. Takaba [2009], "e-VLBI
Activities in Japan," Proc. of the 8th International e-VLBI Workshop "Science and Technology
of Long Baseline Real-Time Interfrometry", pp.24-29.
Recent Japanese e-VLBI activities are reported in this paper. Of ﾟ ine data transfer though the
network has been regularly performed for geodetic VLBI experiments. Besides these offlinetransfers, real-time eVLBI experiments for ultra-rapid UT1 measurements have been
performed among Onsala, Mets 撹 ovi, Tsukuba, and Kashima stations in a pilot project. In thefield of astronomy, a real-time e-VLBI demonstration session organized by the ATNF in 2008
was the first occasion for Kashima to transmit VLBI data obtained by the K5 system to aforeign correlator
in real-time. The global e-VLBI observation session organized by JIVE for the opening event
of International Year of Astronomy in January 2009 was the first participation for a Japanesestation in a global real-time e-VLBI session. Overview of the K5 DAS systems (K5/VSSP, andK5/VSI) used for the e-VLBI is described.
Optically linked e-VLBI observations with domestic VLBI stations have been conducted by
the NAOJ. Also the NAOJ has developed a high speed VLBI data sender/reciver equipment
named VOA-200 and a high speed hardware correlator (2Gbps x 6 baselines). A test
observation of 8 Gbps real-time VLBI was successfully achieved by using the VOA-200 andthe hardware corre-lator in 2008.
Seta, H., M. Tashiro, N. Isobe, Y. Yaji, M. Hayashida, K. Nakanishi, T. Tosaki, K. Kohno, Y.
Shimajiri, M. Fukuhara, M. Sasada, A. Arai, and M. Umemura [2008], "Suzaku Observation of
the OJ 287, Quiescence and Predicted Flare in 2007," Proc. of the Workshop on Blazar
variability across the electromagnetic spectrum, published online, PoS063-1-6.
Suzaku observations are reported of the BL Lacertae object OJ 287, performed on 2007 April
10-13 during the optical quiescent phase and on 2007 November 7 9 during the optical flaring
phase. We organized the simultaneous the radio and optical observations with the Nobeyama
Millimeter Array and optical KANATA telescope at Hiroshima University, respectively. The
X-ray spectrum obtained in the quiescent phase was described by a single power-low modelwith a photon index of Γ= 1.65 ± 0.02 and the flux density was measured to be 216 ± 6 nJy at
1 keV. In the flare phase, the X-ray spectrum became harder (Γ= 1.50 ± 0.01), and the flux
density has doubled to be 398 ± 7 nJy at 1 keV. Our multi-wavelength spectrum exhibited theSR and IC components, and the X-ray spectra cannot be explained as an extension from the SR
components, but suggest that the X-rays are dominated by the IC component. We suggested
electron spectrum indices are variable for each phase. Thus, for the 2nd-flare, SR and IC
components increased without extending energy band.

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Seta, H., N. Isobe, M. S. Tashiro, Y. Yaji, A. Arai, M. Fukuhara, K. Kohno, K. Nakanishi, M.
Sasada, Y. Shimajiri, T. Tosaki, M. Uemura, H. Anderhub, L. A. Antonelli, P. Antoranz, M.
Backes, C. Baixeras, S. Balestra, J. A. Barrio, D. Bastieri, J. Becerra Gonzalez, J. K. Becker, W.
Bednarek, K. Berger, E. Bernardini, A. Biland, R. K. Bock, G. Bonnoli, P. Bordas, D. Borla
Tridon, V. Bosch-Ramon, D. Bose, I. Braun, T. Bretz, I. Britvitch, M. Camara, E. Carmona, S.
Commichau, J. L. Contreras, J. Cortina, M. T. Costado, S. Covino, V. Curtef, F. Dazzi, A. De
Angelis, E. De CeadelPozo, R. de los Reyes, B. DeLotto, M. De Maria, F. De Sabata, C.
Delgado Mendez, A. Dominguez, D. Dorner, M. Doro, D. Elsaesser, M. Errando, D. Ferenc, E.
Fernandez, R. Firpo, M. V. Fonseca, L. Font, N. Galante, R. J. Garc∼ Lopez, M. Garczarczyk,
M. Gaug, F. Goebel, D. Hadasch, M. Hayashida, A. Herrero, D. Hildebrand, D. Hohne-Monch,
J. Hose, C. C. Hsu, T. Jogler, D. Kranich, A. La Barbera, A. Laille, E. Leonardo, E. Lindfors, S.
Lombardi, F. Longo, M. Lopez, E. Lorenz, P. Majumdar, G. Maneva, N. Mankuzhiyil, K.
Mannheim, L. Maraschi, M. Mariotti, M. Martınez, D. Mazin, M. Meucci, M. Meyer, J. M.
Miranda, R. Mirzoyan, H. Miyamoto, J. Moldon, M. Moles, A. Moralejo, D. Nieto, K. Nilsson,
J. Ninkovic, N. Otte, I. Oya, R. Paoletti, J. M. Paredes, M. Pasanen, D. Pascoli, F. Pauss, R. G.
Pegna, M. A. Perez-Torres, M. Persic, L. Peruzzo, F. Prada, E. Prandini, N. Puchades, I.
Reichardt, W. Rhode, M. Ribo, J. Rico, M. Rissi, A. Robert, S. Rugamer, A. Saggion, T. Y.
Saito, M. Salvati, M. Sanchez-Conde, K.Satalecka, V. Scalzotto, V. Scapin, T. Schweizer, M.
Shayduk, S. N. Shore, N. Sidro, A. Sierpowska-Bartosik, A. Sillanpaa, J. Sitarek, D.
Sobczynska, F. Spanier, A. Stamerra, L. S. Stark, L. Takalo, F. Tavecchio, P. Temnikov, D.
Tescaro, M. Teshima, M. Tluczykont, D. F. Torres, N. Turini, H. Vankov, R. M. Wagner, W.
Wittek, V. Zabalza, F.
Zandanel, R. Zanin, J. Zapatero [2009]. "Suzaku andMulti-Wavelength Observations of OJ287 During the Periodic Optical Outburst in 2007," Publ.
Astron. Soc. Japan, vol.61, pp.1011-1022.
Suzaku observations of the blazar OJ 287 were performed in 2007 April 10-13 and November
7-9. They correspond to a quiescent and a flaring state, respectively. The X-ray spectra of thesource can be well-described with single power-law models in both exposures. The derived
X-ray photon index and the flux density at 1 keV were found to be Γ=1.65±0.02 andS1keV=215±5 nJy in the quiescent state. In the flaring state, the source exhibited a harder X-ray
spectrum (Γ=1.50±0.01) with a nearly doubled X-ray flux density of S1keV=404+6-5 nJy.
Moreover, significant hard X-ray signals were detected up to ~27 keV. In cooperation with
Suzaku, simultaneous radio, optical, and very-high-energy γ-ray observations of OJ 287 were
performed with the Nobeyama Millimeter Array, the KANATA telescope, and the MAGIC
telescope, respectively. The radio and optical fluxes in the flaring state (3.04±0.46 Jy and8.93±0.05 mJy at 86.75 Hz and in the V-band, respectively) were found to be higher by afactor of 2-3 than those in the quiescent state (1.73±0.26 Jy and 3.03±0.01 mJy at 86.75 Hz
and in the V-band, respectively). No notable γ-ray events were detected in either observation.
The spectral energy distribution of OJ 287 indicated that the X-ray spectrum was dominated byinverse Compton radiation in both observations, while synchrotron radiation exhibited aspectral cutoff at around the optical frequency. Furthermore, no significant difference in thesynchrotron cutoff frequency was found between the quiescent and flaring states. According toa simple synchrotron self-Compton model, the change of the spectral energy distribution is due
to an increase in the energy density of electrons with small changes of both the magnetic fieldstrength and the maximum Lorentz factor of electrons.
Shibasaki, K. [2008a], "Multi-Wavelength Imaging of Solar Plasma: High-Beta Disruption
Model of Solar Flares," Plasma and Fusion Res., vol.2, pp.S1012-1-S1012-4.
Solar atmosphere is filled with plasma and magnetic field. Activities in the atmosphere are due
to plasma instabilities in the magnetic field. To understand the physical mechanisms ofactivities / instabilities, it is necessary to know the physical conditions of magnetized plasma,

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such as temperature, density, magnetic field, and their spatial structures and temporaldevelopments. Multi-wavelength imaging is essential for this purpose. Imaging observations of
the Sun at microwave, X-ray, ENV and optical ranges are routinely going on. Due to freeexchange of original data among solar physics and related field communities, we can easily
combine images covering wide range of spectrum. Even under such circumstances, we still do
not understand the cause of activities in the solar atmosphere well. The current standard modelof solar activities is based on magnetic reconnection: release of stored magnetic energy byreconnection is the cause of solar activities on the Sun such as solar flares. However, recent
X-ray, ENV and microwave observations with high spatial and temporal resolution show that
dense plasma is involved in activities from the beginning. Based on these observations, I
propose a high-beta model of solar activities, which is very similar to high-beta disruptions inmagnetically confined fusion experiments.
Shibasaki, K. [2008b], "Leakage of Sub-Photospheric Hot Plasma through Magnetic Flux
Tube," American Geophysical Union, Fall Meeting 2008, abstract #SH41A-1614.
The solar corona has million degree temperature even though it is located above the cooler
chromosphere and the photosphere. Also, coronal plasma is constantly flowing out as the solar
wind. So the mechanism of coronal heating needs to include a mechanism of constant plasma
supply. Most of the proposed coronal heating mechanisms are by waves or nano-flares. Bothmechanisms are to carry energy of photospheric convection motion into the corona anddissipate there. Plasma supply is assumed to be through evaporation (or ablation) from thelower atmosphere due to steep temperature gradient. In these mechanisms, tenuous coronalplasma receives large amount of energy to heat and evaporate low temperature plasma into thecorona. Hence the temperature of the initially heated plasma should be much higher than the
million degree corona. Charged particles with such high temperature in the tenuous corona
cannot reach the lower atmosphere due to their strong diamagnetic moment. They will bepushed upwards where magnetic field is weak rather than downwards where magnetic field isstrong. Hence, the evaporation mechanism will not work. I will propose a quite different
mechanism of million-degree plasma supply in more direct manner. The solar corona is filledwith magnetic fields. They are generated at the base of the convection zone and lifted by theconvection motion. The standard model of the Sun shows that the temperature at the base of
the convection zone is about 2 million degree. So the plasmas trapped in the magnetic flux
tube must have temperature there. Plasma particles have diamagnetic moments and they will
be pushed along the flux tube toward weaker magnetic field region. As the result, the solar
atmosphere which is filled with magnetic field, generated at the base of the convection zone,
must have million degree temperature.
Shibasaki, K. [2009], "Nonlinear and Diamagnetic Nature of Plasma and Activities in the Solar
Atmosphere," American Astronomical Society, SPD meeting #40, #30.01; Bulletin of theAmerican Astronomical Society, vol.41, p.864.
Plasma is a nonlinear and diamagnetic media. Magnetic moment of each charged particle inthermal plasma is μ=-kT/B, where k is the Boltzmann constant, T is the plasma temperatureand B is the magnetic flux density. It does not depend on mass or charge. Negative valuemeans that the magnetic moment is anti-parallel to B, or diamagnetic.
This nonlinear and diamagnetic nature of plasma is often not explicitly treated due to low
plasma beta assumption. The plasma beta is the ratio between magnetic moment per unit
volume and the magnetic flux density. However, if the plasma beta exceeds several percent,nonlinear nature becomes important. This is one of the reasons why nuclear fusion experimentin magnetically confined plasmas is difficult. This condition should be the same in the solar
atmosphere.
Particles with magnetic moment anti-parallel to B are pushed toward weak field region along

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the field. This force (mirror force, f =μdB/dr = -kT/L) is proportional to the plasma
temperature and is inversely proportional to the magnetic scale length L (=1/ (1/B dB/dr)).
Generally, magnetic field strength decreases upwards, hence the force is directed upwards. At
higher temperature, this force exceeds the gravity force and generates temperature dependent
up-flows. If the magnetic field is closed, plasma will be accumulated around the top where
magnetic field is the weakest and they suppress B further due to their diamagnetism, hence ahigh beta region spontaneously appears around the loop top. High-beta plasma around the loop
top is unstable against the interchange mode or the ballooning mode due to convex outward
curvature (or bad curvature) of B. High-beta disruption will be expected from the outer surfaceof the loop top.
Shimajiri, Y., S. Takahashi, S. Takakuwa, M. Saito, and R. Kawabe [2008], "Millimeter- andSubmillimeter-Wave Observations of the OMC-2/3 Region. II. Observational Evidence for
Outflow-Triggered Star Formation in the OMC-2 FIR 3/4 Region," Atrophys. J., vol.683,
pp.255-266.
We have observed the Orion Molecular Cloud-2 FIR 3/4 region in the H13CO+ (J-1-0), 12CO
(J=1-0), SiO (ν=0, J=2-1), and CS (J=2-1) lines and the 3.3 mm continuum emission with theNobeyama Millimeter Array (NMA) and in the CO (J=3-2) and CH3OH (JK=7K-6K) lines with
Atacama Submillimeter Telescope Experiment (ASTE). Our NMA observations in the H13CO+
emission have revealed 0.07 pc scale dense gas associated with FIR 4 (FIR 4 clump). The
12
CO (J=3-2,1-0) emission shows high-velocity blue- and redshifted components to both thenortheast and southwest of FIR 3, suggesting an outflow from FIR 3 along the plane of the sky.
The SiO and CH3OH emission, known as shock tracers, are detected around the interface
between the outflow and FIR 4 clump. Furthermore, the 12CO (J=1-0) emission shows an
L-shaped structure in the PV diagram. These results suggest the presence of an interaction
between the outflow and FIR 4 clump. Moreover, our interferometric 3.3 mm continuum
observations have first found that FIR 4 consists of 11 dusty cores at a scale of ~2000 AU. The
separation among these cores (~5x103 AU) is on the same order of the Jeans length (~13x103
AU), and the estimated time scale of the fragmentation (~3.8x104 yr) is similar to the timescale of the outflow interaction (~1.4x104 yr). We suggest that the interaction triggered thefragmentation into these dusty cores, and hence the next generation of the cluster formation in
FIR 4.
Shimajiri, Y., S. Takahashi, S. Takakuwa, M. Saito, and R. Kawabe [2009], "Millimeter- andSubmillimeter-Wave Observations of the OMC-2/3 Region. IV Interaction between the
Outflow and the Dense Gas in the Cluster Forming Region of OMC-2 FIR 6," Publ. Astron.
Soc. Japan, vol.61, pp.1055-1063.
We have conducted millimeter interferometric observations of the Orion Molecular Cloud-2(OMC-2) FIR 6 region at an angular resolution of ~4"-7" with the Nobeyama Millimeter Array(NMA). In the 3.3-mm continuum emission we detected dusty core counterparts of previously
identified FIR sources (FIR 6a, 6b, 6c, and 6d), and moreover resolved FIR 6a into three dusty
cores. The size and mass of these cores are estimated to be 1100-5900 AU and 0.19-5.5M⦿,respectively. We found that in the 12CO (J=1-0) emission FIR 6b, 6c, and 6d eject molecular
outflow, and that the FIR 6c outflow also exhibits at least two collimated jet-like components
in SiO (J=2-1) emission. At the tip of one of the SiO components there appears an abrupt
increase in the SiO line width (~15 km s-1), where the three resolved cores in FIR 6a seem todelineate the tip. These results imply the presence of the interaction and a bowshock front
between the FIR 6c molecular outflow and FIR 6a. If the interaction occurred after theformation of the FIR 6a cores, the influence of the FIR 6c outflow on the FIR 6a cores would
be minimal, since the total gravitational force in the FIR 6a cores (1.0-7.7x10-4 M ⦿km s-1yr-1)
is much larger than the outflow momentum flux (2.4x10-5 M⦿km s-1yr-1). On the other hand, it

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is also possible that the interaction caused the gravitational instability in FIR 6a, and triggered
the fragmentation into three cores, since the separation among these cores (~2.0x103 AU) is on
the same order of the Jeans length (~5.0-8.4x103 AU). In either case, FIR 6a cores, with a massof 0.18-1.6 M⦿and a density of 0.2-5.8x107 cm-3, might be potential formation sites of the next
generation of cluster members.
Shimojo, M., and S. Tsuneta [2009], "The Relation Between Magnetic Fields and Coronal
Activities in the Polar Coronal Hole," Astrophys. J. (Letters), vol.706, pp.L145-L149.
We investigated the relation between polar magnetic fields and polar coronal activities basedon Stokes maps of photospheric and chromospheric lines, simultaneous X-ray and EUV
images. These images are taken with Hinode and Solar and Heliospheric Observatory. With
careful co-alignment between these images, we found that the X-ray jets, the X-ray brightpoints, and the coronal loops in the polar coronal hole appear around the relatively large
magnetic concentrations near the kG-patches with minority polarity. The magnetic
concentrations have magnetic polarity opposite to that of kG-patches, and they are clearly
identified in the Stokes-V maps of the Na I line. We also found that such minority magnetic
concentrations emerge from below the photosphere in the polar region. Our results suggest thatthe coronal activities and structures in the polar coronal hole can be used as a tracer of theappearance of the minority polarities in the polar region.
Shimojo, M. [2010[, "The Variations of Prominence Activities During Solar Cycle," 38th
COSPAR Scientific Assembly, 18-25 July 2010, p.2.
The prominence activities (prominence eruption/disappearance) in the solar atmosphereclosely relate with the CMEs that cause great influences on heliosphere and magnetosphere.
Gopal-swarmy et al. (2003) reported that 72 The Nobeyama Radioheliograph (NoRH) isobserving Sun in microwave (17 GHz) since 1992. At a flare, the main component of the
microwave from Sun is emitted from non-thermal electrons that are accelerated by flare. On
the other hand, the main component of the microwave is thermal emission when Sun is quiet,
and a prominence is clearly observed in microwave because there is the prominence on thelimb. We developed the automatic prominence activity detection program based on 17 GHz
images observed by NoRH, and investigated the variation of the properties of the prominence
activities that oc-curred from 1992 to the end of 2009. We found the following results. 1. The
variation in the number of prominence activities is similar to that of sunspots during one solar
cycle but there are differences between the peak times of prominence activities and sunspots. 2.
The frequency distribution as a function of the magnitude of the prominence activities the sizeof activated prominences at each phase shows a power-law distribution. The power-law index
of the distribution does not change except around the solar minimum. 3. The number ofpromi-nence activities has a dependence on the latitude On the other hand the averagemagnitude is independent of the latitude. In the paper, we will also discuss the relationship theother properties of prominence eruptions, solar cycle and the photospheric magnetic field.
Shintani, M., H. Imai, K. Ando, K. Nakashima, T. Hirota, N. Inomata, T. Kai, S. Kameno, M.
Kijima, H. Kobayashi, M. Kuroki, T. Maeda, K. Maruyama, N. Matsumoto, T. Miyaji, T.
Nagayama, R. Nagayoshi, K. Nakamura, A. Nakagawa, D. Namikawa, T. Omodaka, T. Oyama,
S. Sakakibara, R. Shimizu, K. Sora, M. Tsushima, K. Ueda, Y. Ueda, and K. Yamashita [2008],"Statistical Properties of Stellar H2O Masers - Results of Three-Year Single-Dish Observations
with the VERA Iriki Telescope," Publ. Astron. Soc. Japan, vol.60, pp.1077-1131.
We report on the results of monitoring observations of 242 stellar H2O masers, which havebeen made with the Iriki 20 m telescope of the VLBI Exploration of Radio Astrometry(VERA) from 2003 July to 2006 November. The present paper mainly focuses on 85 stellar
H2O masers that have been tightly observed with a time spacing of typically 1-2 months. In
particular, 46 masers out of them have been recognized concerning their periodic flux variation

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and have light-curve data of stellar visual light. Thus, the present paper shows some statisticalviews of the observed time variability properties of stellar H2O masers. We found a goodcorrelation between a time delay of the variation in the H2O maser flux with respect to that in
the stellar visual light and the stellar pulsation period. The corresponding phase lags are mildly
scattered, but are mainly concentrated in the range, 0.7 ≤∆ϕ≤ 1.5. We also measured
line-of-sight velocity drifts of the individual spectral peaks of H2O maser emission, whichindicate radial acceleration of mass-loss outflows from the evolved stars. We discuss possible
pulsation-driven shock waves that are enhanced near the stellar surface, and are propagating
outwards in the circumstellar envelope.
Shitov, S. V., J. Inatani, W.-L. Shan, M. Takeda, Z. Wang, A. V. Uvarov, A. B. Ermakov, and Y.
Uzawa [2008], "Mesurement of Emissivity of the ALMA Antenna Panel at 840 GHz Using
NbN-Based Heterodyne SIS Receiver," Proc. of the 19th International Symposium on SpaceTHz Technology, ed. Wolfgang Wild, pp.263-266.
We measured emissivity of sample presenting panel of ALMA antenna using Band-10
heterodyne SIS receiver as antenna switching balanced radiometer with 8 GHz instantaneous
bandwidth. Receiver noise temperature measured with 80 K/300 K antenna loads was ≈560 K(DSB). Emissivity of the surface is detected at LO frequency about 840 GHz via the imbalanceof the antenna switch due to extra reflection from sample of panel; absorption 0.25±0.10 % iscalculated from measured emissivity. To confirm measured value, samples made of phosphor
bronze and stainless steel are tested using the same technique. The values of 0.30±0.10 % and1.10±0.10 % are obtained for these samples correspondingly that is consistent with previous
data obtained using direct detector radiometers.
Sofue, Y. [2008a], "CO-Line Rotation Curves, Deep Potential of Massive Cores, andHigh-Density Molecular Nuclei," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds.
Wada, K., and Combes, F., pp.178-185.
We review observational studies of central rotation curves of spiral galaxies using theNobeyama mm-wave interferometer in the CO 2.6-mm line emission. The observedhigh-accuracy rotation curves show universal characteristics: RCs rise steeply in the nuclei, orthey start at finite speed, and are flat toward the galaxy edges. Calculated mass distributions
are similar to each other: spiral galaxies generally have a massive core of ~ 109M⦿ in thecentral 100 pc, bulge, disk and a dark halo. We found extremely high-density, single-peaked
molecular gas nuclei in many galaxies, which are embedded in deep gravitational potential ofthe massive core. Although the molecular nuclei is as that of a giant molecular cloud, the gas is
kept gravitationally stable because of the high-velocity rotation.
Sofue, Y. [2008b], "Central Rotation Curves by CO Lines," Proc. of the "Formation andevolution of galaxy disks", eds. J. G. Funes, and E. M. Corsini, ASP conf. Ser., vol.396,
pp.27-36.
Central rotation curves are fundamental to understand the mass distribution inside galactic
bulges and central disks, which may be physically linked to central massive objects. We review
observational studies of central rotation curves using mm-wave interferometers in the CO
2.6mm line emission. Observed high-accuracy rotation curves show steep rise in the nuclei, ormore likely, they start at finite speed from the center. Mass distributions show that spiralgalaxies generally nest a massive core of ~109 M⦿in the central 100 pc, which is supposed tolink the black hole and bulge. Massive cores are often associated with high-density molecular
gas nuclei, and the core mass and gas density are proportional. The molecular nuclei are
gravitationally stabilized by high velocity differential rotation in the deep gravitational
potential.
Sofue, Y., M. Honma, and T. Omodaka, [2009], "Unified Rotation Curve of the Galaxy Decomposition into de Vaucouleurs Bulge, Disk, Dark Halo, and the 9-kpc Rotation Dip -,"

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Publ. Astron. Soc. Japan, vol.61, pp.227-236.
We present a uni ﾞ ed rotation curve of the Galaxy re-constructed from existing data by
re-calculating the distances and velocities for a set of Galactic constants, R0 = 8 kpc and V0 =200 km s-1. We decomposed it into a bulge with de Vaucouleurs-law profile of half-mass scaleradius 0.5 kpc and mass 1.8 x 1010 M⦿, an exponential disk of scale radius 3.5 kpc and 6.5 x1010 M⦿, and an isothermal dark halo of terminal velocity 200 km s-1. A r 1=4 -law fit was
obtained for the first time for the Milky Way’s rotation curve. After fitting by thesefundamental structures, two local minima, or dips, of the rotation velocity are prominent at
radii 3 and 9 kpc. The 3-kpc dip is consistent with the observed bar. It is alternatively
explained by a massive ring with the density maximum at a radius of 4 kpc. The 9-kpc dip isclearly exhibited as the most peculiar feature in the Galactic rotation curve. We explain it by amassive ring of amplitude as large as 0.3 to 0.4-times the disk density with the density peak at
a radius of 11 kpc. This great ring may be related to the Perseus arm, while no peculiar featureof HI-gas is associated.
Sorai, K., N. Kuno, N. Nakai, H. Matsui, and A. Habe [2008a], "Kinematics of Molecular Gas
in the Bar of Maffei 2," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds. Wada,K., and Combes, F., p.380.
Without abstract
Sorai, K., A. Habe, H. Nishitani, K. Hosaka, Y. Watanabe, S. Miwa, Y. Ohishi, K. Motogi, T.
Minamidani, J. Awano, S. Sumida, Y. Fukuya, R. Uchida, N. Kaneko, M. Y. Fujimoto, Y.
Koyama, M. Kimura, and N. Nakai [2008b], "Large-Scale NH3 Observations toward theGalactic Star-Forming Regions I. W51 Molecular Cloud Complex," Publ. Astron. Soc. Japan,
vol.60, pp.1285-1296.
Large-area observations of dense molecular gas were made in NH3 (J, K ) = (1, 1), (2, 2), and(3, 3) inversion lines with 4.'5 resolution toward the molecular cloud complex of the W 51
region. The observations were a part of a NH3 survey of the Galactic star-forming regions
using the Tomakomai 11-m radio telescope. NH3 (J, K ) = (1, 1) and (2, 2) emission was
detected in the W 51 A and B complexes, while the detection of (J, K ) = (2, 2) emission was
marginal in W 51 B. The rotation temperature was ~40 K in the central part of the W 51 A
complex, while being ~20 K in the other positions. A weak correlation is found that theortho-to-para ratio decreases with increasing the rotation temperature, the far-infrared
luminosity and the index of the star-formation ef ﾞ ciency. This tendency is explained if starformation has continued for more than the time scale of the transformation between ortho- andpara-NH3 : active star formation on a large scale, such as the interaction of molecular clouds
with a spiral arm, has made the molecular gas warmer, even in a scale of ~10 pc, and theproceeding transformation has made the ortho-to-para ratio lower.
Sugimoto, M., G. Kosugi, S. Iguchi, H. Iwashita, M. Saito, J. Inatani, M. Tasaki, T. Takahashi,
K. Nakanishi, J. P. McMullin, J. P. Puga, B. Hoff, J. Notambuena, T. Kamazaki, B. Vila-Volaro,
B. Ikenoue, K.-I. Morita, S. Asayama, M. Yamada, and H. Kiuchi [2009a], "Beam Pattern
Measurements and Observational Evaluations of the ALMA/ACA 12-m Antenna," Publ.
Astron. Soc. Japan, vol.61, pp.451-459.
We have evaluated the beam pattern of the ALMA/ACA 12-m antenna with total power
observations of Jupiter and the Moon. Models of the expected beam pattern as it passes acrossJupiter and the Moon were derived in consideration of the radiation pattern of the actual
receiving system and the surface error of the main reflector. Since the profiles of the measured
beam patterns were consistent with those of the models within the range from the peak to -20
dB, we confirmed that the antenna achieved the beam pattern expected from its optical design.
After this confirmation, we performed astronomical observations. In addition to the detectionof the CS J = 3-2 (146.969026 GHz) spectrum toward Orion KL, the change in the Moon

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intensity was successfully detected during the total lunar eclipse during 2008 February 20-21.
A time lag longer than 10 min in the millimeter-wave eclipse relative to the corresponding
optical eclipse ephemeris was detected. Mapping observations of the Sun revealed the structureof the chromospheric networks at 147 GHz. These astronomical observations confirmed that
the ACA 12-m antenna could be successfully operated under various operating conditions.
Sugimoto, M., M. Carter, J. Inatani, Y. Sekimoto, and S. Iguchi [2009b], "Design of Corrective
Beam Waveguide System for the ALMA/ACA 7-m Antenna," Publ. Astron. Soc. Japan, vol.61,
pp.1065-1080.
A beam waveguide system for connecting the ALMA front-end, which has been designed for
the Cassegrain focus of the ALMA 12-m antenna, with the ALMA/ACA 7-m antenna wasdesigned. The beam waveguide system, covering 30-950 GHz, consists of flat mirrors or
prisms to modify the boresight tilt angle from the front-end, and recovers more than the half ofthe sensitivity loss caused by a misalignment between the front-end optics and the 7-m antenna.
No mechanical alignment procedure is needed for installation of the beam waveguide system,and thus it does not impact on the maintenance/operation scheme of the front-end system.
Beam-pattern measurements in the frequency ranges of ALMA bands 4 (144 GHz), 6 (252GHz), and 8 (385 GHz) have confirmed that directions of the radiation patterns transmitted tothe subreflector are successfully shifted by the beam waveguide system without any serious
deformation of the beam. The aperture efficiencies calculated from the measured radiation
patterns were determined to be 84.6% at 144 GHz, 86.1% at 252 GHz, and 84.8% at 385 GHz,
which are consistent with those of a simulated radiation pattern.
Sugimoto, M., S. Iguchi, J. Inatani, Y. Sekimoto, and S. Asayama [2010], "Sensitivity Analysis
of optical Systems in Radio Telescope," Publ. Astron. Soc. Japan, vol.62, pp.39-50.
We have demonstrated an approach to predict the overall efficiency and system noise
regarding optical systems in radio telescopes, based on a systematic evaluation of both theoptical propagation efficiency through all optical components, from the receiver horn to themain reflector, and of their noise contributions. The analysis employs several conventional
techniques, including the principle of multimode Gaussian optics and calculations of losses
associated with optical components. A detailed analysis was performed for cases of ALMA
band 4 (125-163 GHz) and 8 (385-500 GHz). The analysis predicts a reasonable efficiency of
0.75-0.76 (0.57-0.62) and a system noise of ~70 K (300-400 K) for band 4 (band 8). The
calculated efficiency of the band 4 optics was found to be consistent with the efficiency
measured by astronomical observations with the ALMA/ACA 12-m antenna. In addition to aconfirmation that the bands 4 and 8 optics were designed to maximize the overall efficiency,
the analysis for the bands 4 and 8 frequency ranges also confirmed that there is no differencein the optimum edge levels at the subreflector between the two different ways of maximization,i.e., toward the overall efficiency or the sensitivity, which is defined by the ratio of the overall
efficiency over the sum of noises generated from all possible sources. We also applied asensitivity analysis to the band 1 frequency case, and revealed a slight, but clear, difference inthe optimum edge levels between the sensitivity and the efficiency (difference is 1 ﾐ 2 dB).
This corresponds to a sensitivity loss of 1% if we optimize the optics to maximize theefficiency.
Sugiyama, K., K. Fujisawa, A. Doi, M. Honma, H. Kobayashi, T. Bushimata, N. Mochizuki,
and Y. Murata [2008a], "Mapping Observations of 6.7 GHz Methanol Masers with Japanese
VLBI Network," Publ. Astron. Soc. Japan, vol.60, pp.23-35.
We have observed 13 methanol maser sources associated with massive star-forming regions: W
3(OH), Mon R2, S 255, W 33A, IRAS 18151-1208, G 24.78+0.08, G 29.95-0.02, IRAS
18556+0136, W 48, OH 43.8-0.1, ON 1, Cep A, and NGC 7538 at 6.7GHz using the Japanese
VLBI Network (JVN). Twelve of the thirteen sources were detected at our longest baseline of

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~50Mλ, and their images are presented. Seven of them are the first VLBI images at 6.7GHz.
The high detection rate and the small fringe spacing of ~4 mas suggest that most of themethanol maser sources have compact structures. Given this compactness as well as the known
properties of long life and small internal motion, the methanol maser line is suitable forastrometry with VLBI.
Sugiyama, K., K. Fujisawa, M. Honma, A. Doi, N. Mochizuki, Y. Murata, and Y. Isono[2008b], "Japanese VLBI Network Observations of 6.7-GHz Methanol Masers II. Results,"
Proc. of the IAU Symp. 242, "Astrophysical Masers and their Environments", eds. Jessica
Chapman and Willem Baan, pp.176-177.
We are using a Japanese VLBI network (JVN) for VLBI observations of 6.7-GHz methanol
masers associated with massive star-forming regions. Here we present results for Cepheus A(Cep A) from observations taken on September 9, 2006. The distribution of the maser spots
indicates either a spherical bubble or a disk having an inclination of several tens degree. We
construct a disk model with an inclination of ~70° and a radius of ~700 AU. From a luminosityof 1.7 x 104 Lsolar for a source observed in this region, the excitation of the maser is probablyradiative.
Sugiyama, K., K. Fujisawa, A. Doi, M. Honma, Y. Isono, H. Kobayashi, N. Mochizuki, and Y.
Murata [2008c], "A Synchronized Variation to the 6.7 GHz Methanol Maser in Cepheus A,"
Publ. Astron. Soc. Japan, vol.60, pp.1001-1006.
We present the results of monitoring observations of a 6.7 GHz methanol maser in Cepheus A(Cep A) using the Yamaguchi 32m radio telescope and of imaging observations conducted with
the JVN (Japanese VLBI Network). We indentified five spectral features, which are grouped
into two groupes: redshifted (-1.9 and -2.7 km s-1) and blueshifted (-3.8, -4.2, and -4.9 km s-1).
We detected rapid variabilities in these maser features within a monitoring period of 81 d. The
redshifted features decreased in flux density to 50% of the initial value, while the blueshifted
ones rapidly increased within 30 d. The time variation in these maser features had two
remarkable properties: synchronization and negative correlation between the redshifted and theblueshifted. Based on the JVN observations,we found that the maser spots were associatedwith the Cep A HW2 object and had an arched structure with a scale of ~1400AU; also,
separations of the five maser features were found to be larger than 100AU. These properties ofthe masers, namely, the synchronization of the flux variation and the spectral and spatial
isolations of the features, suggest that the collisional excitation by a shock wave from acommon exciting source is unlikely to happen. Instead, the synchronized time variation of themasers can be explained if all the maser features are excited by infrared radiation from the dustthat is heated by a common exciting source with a rapid variability.
Sugiyama, K., K. Fujisawa, A. Doi, M. Honma, Y. Isono, N. Mochizuki, Y. Murata, S.
Sawada-Satoh, and K. Wajima [2008d], "Associating Sites of Methanol Maser Emissions at
6.7 GHz," Proc. of the 9th European VLBI Network Symposium on The role of VLBI in theGolden Age for Radio Astronomy and EVN Users Meeting, September 23-16, 2008, Bologna,
Italy, p.99.
We have carried out VLBI observations of some methanol maser sources at 6.7 GHz with theJapanese VLBI Network (JVN) using phase-referencingt echniques. We superposed themethanol masers on water, hydroxyl masers, radio continuum,and various molecular line
emissions with an accuracy of a milliarcsecond (mas) scale, which is enough for investigating
a positional relation with a central or exciting star. In this paper, were port results of thesuperposition in massive star-forming regions( SFRs) Cepheus A (CepA) and Onsala 1 (ON1).
The methanol maser spots of Cep A showed an arched structure with a scale of 1400 AU. This
structure was roughly per-pendicular to a radio continuum jet, having an exciting star near thecenter of the arch, and was coincident with the CH3CN, NH3 disks. It is easy to explain that the

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Cep A methanol masers are associated with a circumstellar disk around a massive young stellar
object (YSO). The methanol maser spots of ON 1 formed two main clusters isolated 1800 AU
from each other, which corre-sponded to a red- and ablue-shifted spectral feature, respectively.
The direction of the elongation of the isolated clusters coincided with the H13CO+, SiO
molecular outflows, although each spatial size is quite different. Also, the position-velocity
diagram along the direction of the molecular outflows roughly coincided. The ON 1
methanol masers may trace an outflow ejected from a massive YSO, while it is also thought tobe possible that the masers of this source may trace an expansion of an Ultra-compact (UC)HII region by superposing on the hydroxyl masers.
Sugiyama, K., K. Fujisawa, K. Wajima, S. Sawada-Satoh, Y. Isono, M. Honma, Y. Murata, N.
Mochizuki, and A. Doi [2009], "The Kinematics of the Methanol Maser at 6.7 GHz in Cepheus
A," Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics andTechnologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser.
vol.402, pp.392-395.
We have conducted VLBI observations of methanol masers at 6.7 GHz with JVN and watermaser at 22.2 GHz with VERA in the massive star-forming region Cepheus A (Cep A). The
distribution of methanol maser spots showed an arc-like structure. Comparing the distributionsof CH3CN line emission and continuum emission at 8, 22, and 43 GHz obtained from otherobservations, we inferred that the 6.7-GHz methanol masers in Cep A originates from arotating disk with a radius of 690 AU, a PA of 110°, and an inclination of 73°. Also, some of
the water masers in this region may be associated with the rotating disk.
Sunada, K., T. Nakazato, N. Ikeda, S. Hongo, Y. Kitamura, and J. Yang [2007], "Water Maser
and Ammonia Survey toward IRAS Sources in the Galaxy I. H2O Maser Data," Publ. Astron.
Soc. Japan, vol.59, pp.1185-1219.
We present H2O maser data from a survey toward IRAS sources in the Galaxy with theNobeyama 45m telescope. This survey had a 1σ noise as small as 0.24Jy, resulting in one of
the most sensitive water-maser surveys. The maximum distance of the masers to be detectedby our survey is estimated to be 3 kpc for sources with Fν, 1 kpc < 10Jy and 10 kpc for thosewith 10 Jy ≤Fν, 1 kpc <100Jy, where Fν, 1 kpc is the maser flux density converted at a distance of 1
kpc/ For strong masers with Fν, 1 kpc ≥100Jy,our survey cloud detect all sources in the Galaxy.
We carried out a total of 2229 observations toward 1536 sources and detected water-maser
emission toward 222 sources. Our survey newly found masers from 75 of the 222 sources. The
maser spectra of the new sources are shown in addition to the line parameters of all thedetected sources. Furthermore, we discovered an extremely high-velocity component with
VLSR = -146 km s-1 toward a well-known source, NGC 7538 IRS 11. For the three sources of
NGC 1333 IRAS 4A/B, IRAS 05329-0512, and 06053-0622, we succeeded to spatiallyseparate multiple-velocity components.
Sunada, K., N. Ikeda, Y. Kitamura, T. Nakazato, and J. Yang [2010], "Class 0 Protostellar
Candidates in the AKARI-FIS Bright Source Catalogue," Proc. of the "AKARI, a light toilluminate the misty universe", eds. T. Onaka, G. J. White, T. Nakagawa, and I. Yamamura,
ASP Conf. Ser. vol.418, pp.73-78.
It is expected that the FIS Bright Source Catalogue contains many Class 0 protostellar
candidates. In particular, the identification of high-mass protostellar candidates is expected. To
search new protostellar candidates systematically in the FIS Bright Source Catalogue, wecharacterized the far-infrared properties of various known objects. We carried out theidentification of the FIS point sources for our 1563 survey sources. As a result, we could findthe region occupied by the sources associated with the water maser emission on the FIS
log(F140μm) - log(F90μm/F65μm) diagram. Comparing the core properties with the far-infrared
properties, we also found the spread of the region occupied by the H2O maser sources meant

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the mass difference and the evolution sequence. Finally, we examined the far-infrared
properties of all the point sources in the catalogue. Considering the above results, we were able
to confirm the new protostellar candidates from low- to high-mass in the FIS Bright Source
Catalogue.
Tachihara, K., R. Neuhauser, and Y. Fukui, [2009], "Search for Remnant Clouds Associatedwith the TW Hya Association," Publ. Astron. Soc. Japan, vol.61, pp.585-591.
We report on a search for the parental molecular clouds of the TW Hya association (TWA),
using CO emission and Na I absorption lines. TWA is the nearest young (~50 pc; ~10 Myr)stellar association; yet in spite of its youth there has been no detection of any associated natal
molecular gas, as is the case with other typical young clusters. Using infrared maps as a guide,
we conducted a CO cloud survey toward a region with a dust extinction of E (B - V ) > 0.2
mag, or AV > 0.6 mag. CO emission was detected in the direction of three IR dust clouds, andwe rejected one cloud out of the TWA, because no interstellar Na absorption was detected in
the nearby Hipparcos stars, implying that it is too distant to relate to the TWA. The two otherclouds exhibit only faint and small-scale CO emission. Interstellar Na I absorptions of
Hipparcos targets (HIP 57809, HIP 64837, and HIP 64925, at distances of 133, 81, and 101 pc,
respectively) by these clouds were also detected. We conclude that only a small fraction of theinterstellar matter (ISM) toward the infrared (IR) dust cloud is located at a distance less than
100 pc, which may be all that is left out of the remnant clouds of TWA; the remaining remnant
cloud dissipated within the last ~1 Myr. Such a short-dissipation timescale may be due to an
external perturbation or kinematic segregation that has a large stellar proper motion relative tothe natal cloud.
Takahashi, H., H. Matsuo, and K. Nakanishi [2010], "Spectroscopic Imaging Study of Nearby
Spiral Galaxies: Introduction of Observations with AKARI, NRO and ASTE," Proc. of the"AKARI, a light to illuminate the misty universe", eds. T. Onaka, G. J. White, T. Nakagawa,and I. Yamamura, ASP Conf. Ser. vol.418, pp.491-494.
The aim of this research is to reveal the spatial distribution of the star formation activity
toward nearby galaxies by comparing CO molecular emission lines with the large area
observation in FIR lines. We report the imaging observations of far-Infrared (FIR) forbiddenlines via FIS-FTS and CO molecular lines from low to high excitation levels with ASTE,
which are good tracer of star forming regions or photo-dissociation regions, especially spiralgalaxies, in order to derive the information of the physical conditions of the ambientinterstellar radiation fields. The information tells us not only the difference of current star
forming activity between the arm and the interarm of these galaxies but also star forming
history and evolution of spiral galaxies with systematic and statistical study. Furthermore thedust properties can be referred by combining far-infrared photometric data and submillimeter
observation. This observation program is a proposal which presents a tool for investigation ofphysical properties of nearby galaxies.
Takahashi, S., M. Saito, S. Takakuwa, and R. Kawabe [2008a], "A New Evolutionary Scenario
of Intermediate-Mass Star-Formation Revealed by Multi-Wavelength Observations of
OMC-2/3," Astrophys. and Sp. Sci., vol.313, pp.165-168.
We have performed millimeter- and submilli- meter-wave survey observations using theNobeyama millimeter array (NMA) and the Atacama Submillimeter Telescope Experiment(ASTE) in one of the nearest intermediate-mass (IM) star forming regions: Orion Molecular
Cloud-2/3 (OMC-2/3). Using the high-resolution capabilities offered by the NMA ("several
arcsec), we observed dust continuum and H13CO+(1-0) emission in 12 pre- and proto-stellar
candidates identified previously in single-dish millimeter observations. We unveiled theevolutionary change with variations of the morphology and velocity structure of the denseenvelopes traced by the H13CO+(1-0) emission. Furthermore, using the high-sensitivity

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capabilities offered by the ASTE, we searched for large-scale molecular outflows associatedwith these pre- and proto-stellar candidates observed with the NMA. As a result of the CO(3-2)
observations, we detected six molecular outflows associated with the dense gas envelopes
traced by H13CO+(1-0) and 3.3 mm continuum emission. The estimated CO outflow
momentum increases with the evolutionary sequence from early to late type of the protostellar
cores. We also found that the 24 mum flux increases as the dense gas evolutionary sequence.
We propose that the enhancement of the 24 mum flux is caused by the growth of the cavity (i.e.
the CO outflow destroys the envelope) as the evolutionary sequence. Our results show that thedissipation of the dense gas envelope plays an essential role in the evolution of the IM
protostars. The extremely high-sensitivity and high-angular resolution offered by ALMA will
reveal unprecedented details of the inner "50 AU of these protostars, which will provide us abreak through in the classic scenario of IM star/disk formation.
Takahashi, S., M. Saito, N. Ohashi, N. Kusakabe, S. Takakuwa, Y. Shimajiri, M. Tamura, and
R. Kawabe [2008b], "Millimeter- and Submillimeter-Wave Observations of the OMC-2/3
Region. III. An Extensive Survey for Molecular Outflows," Astrophys. J., vol.688, pp.344-361.
Using the ASTE 10 m submillimeter telescope and the 1.4 m Infrared Survey Facility (IRSF),
we performed an extensive outflow survey in the Orion Molecular Cloud 2 and 3 region. Our
survey, which includes 41 potential star-forming sites, has been newly compiled using
multiwavelength data based on millimeter- and submillimeter-continuum observations, as wellas radio continuum observations. From the CO(3-2) observations performed with the Atacama
Submillimeter Telescope Experiment (ASTE) 10 m telescope, we detected 14 CO molecular
outflows, seven of which were newly identified. This higher detection rate, as compared toprevious CO(1-0) results in the same region, suggests that CO(3-2) may be a better outflow
tracer. Physical properties of these outflows and their possible driving sources were derived.
Derived parameters were compared with those of CO outflows in low- and high-massstar-forming regions. We show that the CO outflow momentum correlates with the bolometricluminosity of the driving source and with the envelope mass, regardless of the mass of thedriving sources. In addition to these CO outflows, seven sources having near-IR features
suggestive of outflows were also identified.
Takahashi, S., P. T. P. Ho, T.-W. Tang, R. Kawabe, and M. Saito [2009], "Evolutionary Statusof Brightest and Youngest Sources in the Orion Molecular Cloud -3 Region," Astrophys. J.,
vol.704, pp.1459-1470.
The brightest continuum source in the Orion molecular cloud-3 region (OMC-3), MMS 6, wasobserved with the Very Large Array (VLA), the Nobeyama Millimeter Array (NMA), and theSubmillimeter Array (SMA). Our data were supplemented by near- to mid-infrared archival
data taken by Spitzer Space Telescope. The compact continuum source, MMS 6-main, wasdetected with an H2 mass of 3.0 Msun with a size of 510 AU. Despite its compact andwell-condensed appearance, neither clear CO outflow, radio jet, nor infrared sources (at awavelength shorter than 8μm) were detected at MMS 6-main even with the present highangular resolution and high-sensitivity observations. The derived H2 column density, 2.61025 cm-2, corresponds to a visual extinction of Av ~ 15, 000 mag, and the derived number
density is at least two orders of magnitude higher than for the other OMC-2/3 continuum
sources. The volume density profile of the source was estimated to have a power-law index of
2 or steeper down to a radius of ~450 AU. The timescale to form a protostar at the center or thetimescale elapsed after its formation is estimated to be 830 to 7600 yr. This is much shorter
than the typical lifetime of the Class 0/I protostars, which is ~104-105 yr, suggesting that MMS
6-main is probably in either the earliest stage of the protostellar core or in the latest stage ofthe prestellar phase.
Takahashi, S., S. Deguchi, N. Kuno, T. Shimoikura, and F. Yoshida [2010], "A Search for

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Water Masers in the Saturnian System," Publ. Astron. Soc. Japan, vol.62, pp.L17-L21.
We searched for H2O 6(1,6)-5(2,3) maser emission at 22.235 GHz from several Saturnian
satellites with the Nobeyama 45m radio telescope in May 2009. Observations were made for
Titan, Hyperion, Enceladus and Atlas, for which Pogrebenko et al. (2009) had reported
detections of water masers at 22.235 GHz, and in addition for Iapetus and other inner satellites.
We detected no emission of the water maser line for all the satellites observed, althoughsensitivities of our observations were comparable or even better than those of Pogrebenko etal.. We infer that the water maser emission from the Saturnian system is extremely weak, orsporadic in nature. Monitoring over a long period and obtaining statistical results must be
made for the further understanding of the water maser emission in the Saturnian system.
Takakuwa, S., D. Iono, B. Vila-Vilaro, T. Sekiguchi, and R. Kawabe [2008], "Scientific Role of
ACA for Low-Mass Star-Formation Study," Astrophys. and Sp. Sci., vol.313, pp.169-173.
We discuss the scientific role of the Atacama Compact Array (ACA), the Japanese contribution
to the ALMA project, for low-mass star-formation study. Our recent observations of several
low-mass protostellar envelopes in the submillimeter CS (J=7-6) and HCN (J=4-3) lines with
the SMA and ASTE have revealed that these submillimeter emissions are more extended than~2000 AU and show different velocity structures from those traced by millimeter lines. These
results suggest the importance of taking short-spacing informations the ACA can offer. Our
comprehensive imaging simulations of these protostellar envelopes, as well as prestellar coresand debris disks, unprecedentedly demonstrate the scientific importance of ACA.
Takeuchi, T., H. Yamamoto, K. Torii, N. Kudo, T. Hayakawa, A. Kawamura, N. Mizuno, T.
Onishi, A. Mizuno, H. Ogawa, and Y. Fukui [2010], "NANTEN Survey of Molecular Clouds
toward the Galactic Centre; Association of Compact Astronomical Objects," Publ. Astron. Soc.
Japan, vol.62, pp.557-612.
In order to better understand molecular clouds and their properties toward the Galactic centerregion, we have analyzed the NANTEN database of 12CO (J = 1-0) and 13CO (J = 1-0) to
search for associations with candidates for young high-mass star-forming regions, such as
IRAS point sources, radio continuum sources recombination line sources, maser line sources,and other molecular line sources. We have also compared the data with TeV γ-ray sources. The
analyzed region covers -12°≤ l ≤12° and -1°.5 ≤ b ≤ 1°.5 for 12CO, and -6°≤ l ≤ 8° and -1°≤ b≤1° for 13CO. As a result, we identified 167 IRAS point sources, 73 recombination line sources,
58 maser sources, 107 radio continuum sources, and 77 molecular line sources associated with
169 positions with the CO emission. The associations among the objects with known velocity
are fairly certain (68%), while those with only positional coincidence are less reliable (32%).
We present a catalog of these CO clouds in a form useful for future follow-up studies. As
specific examples of usage of the catalog, we highlight three outstanding regions of active starformation: W 28, W 30, and W 31. In particular, we have discovered that the W 30 region
shows a striking correlation between the extended TeV γ-ray source and the molecular gas.
This is a second case of such a good correlation identified from the NANTEN dataset
subsequent to W 28 (Aharonian et al. 2008, A&A, 481, 401). We suggest that the pulsar PSR
J1803 2137 near the molecular features may play a role in γ-ray production. The W 31 region
exhibits another active star formation, while noγ-ray source is yet known.
Takita, S., Y. Kitamura, H. Kataza, D. Ishihara, M. Ueno, H. Fujiwara, N. Ikeda, A. Kawamura,
H. Murakami, Y. K. Okamoto, T. Onaka, S. Oyabu, I. Sakon, and H. Takahashi [2009],"Diffuse 18 m Emission around TYC 3159-691 Discovered by the AKARI MIR All-Sky
Survey," Publ. Astron. Soc. Japan, vol.61, pp.291-299.
We report on observations of the mysterious object TYC 3159-6-1 located toward the Cygnus
X region. It shows interesting characteristics in the AKARI mid-infrared All-Sky Survey. The
central star is clearly detected as a point source at 9μm, while no point-like source, but a large

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shell-like structure is seen around the source at 18μm. The optical spectrum indicates thepresence of the weak Hαemission on the red smooth continuum, where as the mid-infraredN-band spectrum shows neither excess emission nor significant silicate absorption
Interferometric continuum observations at 104 GHz do not show any appreciable peak at theposition of the star. On the basis of these observations, we investigate three possibilities ofconcerning the nature of TYC 3159-6-1: a nearby young stellar object, a heavily extinctedhigh-mass star, and an asymptotic giant branch(AGB) star with a detached shell. We conclude
that none of these cases can account for the observations consistently, and the nature of TYC
3159-6-1 remains a mystery.
Tamura, Y., K. Nakanishi, K. Kohno, R. Kawabe, and S. K. Okumura [2008], "HCN and HCO+
Imaging of the Antenna Galaxies: Distribution and Evolution of Dense Molecular Gas in a
Colliding Galaxy System," Proc. of the "Mapping the Galaxy and Nearby Galaxies", eds.
Wada, K., and Combes, F., p.379.
Without abstract
Tamura, Y., K. Kohno, K. Nakanishi, B. Hatsukade, D. Iono, G. W. Wilson, M. S. Yun, T.
Takada, Y. Matsuda, T. Tosaki, H. Ezawa, T. A. Perera, K. S. Acott, J. E. Austermann, D. H.
Hughes, I. Aretxaga, A. Chung, T. Oshima, N. Yamaguchi, K. Tanaka, and R. Kawabe [2009],"Spatial Correlation between Submillimeter and Lyman-Alpha Galaxies in the SSA 22
Protocluster," Nature, vol.459, pp.61-63.
Lyman-α emitters are thought to be young, low-mass galaxies with ages of ~108yr (refs 1, 2).
An overdensity of them in one region of the sky (the SSA22 field) traces out a filamentary
structure in the early Universe at a redshift of z~3.1 (equivalent to 15 per cent of the age of the
Universe) and is believed to mark a forming protocluster. Galaxies that are bright at(sub)millimetre wavelengths are undergoing violent episodes of star formation, and there isevidence that they are preferentially associated with high-redshift radio galaxies, so thequestion of whether they are also associated with the most significant large-scale structure
growing at high redshift (as outlined by Lyman-α emitters) naturally arises. Here we report an
imaging survey of 1,100-μm emission in the SSA22 region. We find an enhancement ofsubmillimetre galaxies near the core of the protocluster, and a large-scale correlation between
the submillimetre galaxies and the low-mass Lyman-α emitters, suggesting synchronous
formation of the two very different types of star-forming galaxy within the same structure athigh redshift. These results are in general agreement with our understanding of the formationof cosmic structure.
Tanaka, K., T. Oka, M. Nagai, and K. Kamegai [2009], "A Large Expanding Molecular Arc in
the Sagittarius B1 Complex," Publ. Astron. Soc. Japan, vol.61, pp.461-469.
Results of molecular line observations toward the Sagittarius B1 complex are reported. Mapsof the HCN, HCO+ and SiO J = 1-0 emissions were taken with the NRO 45-m telescope. With
these data, combined with the ASTE CO J = 3-2 survey data, we have investigated the spatial
structure, kinematics and physical conditions of two peculiar molecular features: CO0.55+0.07
and SiO0.56-0.01. The CO arc, CO0.55+0.07, shows clear expanding motion with sizes of
8.5x6.8 pc2 and an expansion velocity of 40 km s-1. The SiO shell, SiO0.56-0.01, has a size of
3.0 x 3.4 pc2, and surrounds an X-ray Fe line source, G0.570-0.018. The mass and the kinetic
energy of CO0.55+0.07 are estimated to be 105.5 M⦿ and 1051.5 erg, respectively. The kinetic
energy of SiO0.56-0.01 is ~1050.4 erg. An LVG analysis shows that the typical density andkinetic temperature are 103.8 cm-3 and 28 K, respectively. High-density clumps with a densityof 104.0-4.5 cm-3 associated with CO0.55+0.07 and SiO0.56-0.01 have been found, supporting
the idea that they consist of swept-up material. The huge kinetic energy of CO0.55+0.07 is
considered to be injected by a series of supernova explosions that took place within ~2 x 105 yr,
which would suggest that it is a ‘bubble’ created by a massive stellar cluster, whose mass is

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estimated to be 103.5-4.5 M⦿. The origin of SiO0.5-0.01 is rather unclear, but we suggest that it
could be related to the X-ray source G0.570-0.018.
Tatematsu, K., R. Kandori, T. Umemoto, and Y. Sekimoto [2007], "Orion A Giant Molecular
Cloud in N2H+, HC3N, and CCS, American Astronomical Society, AAS Meeting #211,#139.13.
The "integral-shaped filament" of the Orion A giant molecular cloud was mapped in N2H+ J =1-0 (93 GHz), and its northern end, OMC-2/3 region was observed also in HC3N J =5-4 (45GHz) and CCS (45 and 82 GHz). The observations were carried out with Nobeyama 45-m
Radio Telescope. Their distribution was compared with our previous H13CO+ map (Aso et al.
2000) and with the dust map in the literature. N2H+ distribution is similar to the dust
distribution, except for the central part of the Orion Nebula, where gas temperature is high. We
identified 34 cloud cores from N2H+ data, and carried out hyperfine fitting to spectra. Theiraverage physical parameters are N2H+ excitation temperature Tex = 9.3±4.3 K, linewidth
Deltav = 0.92±0.52 km/s, core radius R = 0.086±0.018 pc, column density N (H2) = 4.2±1.61022 cm -2, average density n (H2)=7±3; 104 cm-3, and core mass M = 30.3±20.5 Mo. The
excitation temperature is twice as high as that in Taurus cores (Tatematsu et al. 2004). The
masses of cores identified both in N2H+ and in H13CO+ in OMC-2/3 are very consistent. We
found one peculiar H13CO+ core which is not prominent in either N2H+, HC3N or dust. This
core overlaps with the lobe of the intense outflow, which might cause H13CO+ intensity
enhancement. In OMC-2/3, we detected no CCS emission. In general N2H+ and HC3N
distribution is quite similar in OMC-2/3, but we observed displacement between N2H+ andHC3N over 2 arcmin scale along the OMC-3 ridge, which has a chain of Class 0-I protostars(and candidates) including X-ray protostars.
Tatematsu, K., R. Kandori, T. Umemoto, and Y. Sekimoto [2008], "N2H+ and HC3N
Observations of the Orion A Cloud," Publ. Astron. Soc. Japan, vol.60, pp.407-419.
The “∫-shaped filament'' of the Orion A giant molecular cloud was mapped in N2H+, and its
northern end, the OMC-2/3 region, was also observed in HC3N and CCS. The results werecompared with map s of other molecular lines and the dust continuum emission. The N2H+
distribution is similar to the dust continuum distribution, except for the central part of theOrion Nebula. The distribution of H13CO+ hold a resemblance to that of the dust continuum,
but the N2H+ distribution looks more similar to the dust continuum distribution. The N-bearing
molecules, N2H+ and NH3, seem to be more intense in OMC-2, compared with the H13CO+ andCS distribution. This suggests that OMC-2 has a higher abundance of N-bearing molecules, ora higher filling factor of the quiescent gas. We identified 34 cloud cores from N2H+ data. Over
the Orion Nebula region, the N2H+ linewidth is large (1.1-2.1 km s-1). In the OMC-2/3 region,
it becomes moderate (0.5-1.3 km s-1), and it is smaller (0.3-1.1 km s-1) in the south of the Orion
Nebula. On the other hand, the gas kinetic temperature of the quiescent cores observed in N2H+
is rather constant (~ 20 K) over the∫-shaped filament. We detected no CCS emission in the
OMC-2/3 region. In general, N2H+ and HC3N distribution is quite similar in the OMC-2/3
region, but we observed displacement between N2H+ and HC3N over a 2' scale in OMC-3,
which has a chain of Class 0-I protostars (candidates).
Torii, K., N. Kudo, M. Fujishita, T. Kawase, T. Okuda, H. Yamamoto, A. Kawamura, N.
Mizuno, T. Onishi, M. Machida, K. Takahashi, S. Nozawa, R. Matsumoto, J. Ott, K. Tanaka, N.
Yamaguchi, H. Ezawa, J. Stutzki, U. Klein, F. Bertoldi, K. Bon-Chul, L. Bronfman, M. Burton,
A. Benz, H. Ogawa, and Y. Fukui [2010], "Temperature and Density in the Foot Points of the
Molecular Loops in the Galactic Center; Analysis of Multi-J Transitions of 12CO(J=1-0, 3-2,
4-3, 7-6), 13CO(J=1-0) and C18O(J=1-0)," Publ. Astron. Soc. Japan, vol.62, pp.675-695.
Fukui et al. (2006) discovered two molecular loops in the Galactic center and argued that thefoot points of the molecular loops, two bright spots at both loops ends, represent the gas

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accumulated by the falling motion along the loops, subsequent to magnetic flotation by the
Parker instability. We have carried out sensitive CO observations of the foot points toward
l=356° at a few pc resolution in the six rotational transitions of CO; 12CO(J=1-0, 3-2, 4-3, 7-6),
13
CO(J=1-0) and C18O(J=1-0). The high resolution image of 12CO (J=3-2) has revealed thedetailed distribution of the high excitation gas including U shapes, the outer boundary of whichshows sharp intensity jumps accompanying strong velocity gradients. An analysis of themulti-J CO transitions shows that the temperature is in a range from 30-100 K and density isaround 103-104 cm-3, confirming that the foot points have high temperature and density
although there is no prominent radiative heating source such as high mass stars in or aroundthe loops. We argue that the high temperature is likely due to the shock heating under C-shockcondition caused by the magnetic flotation. We made a comparison of the gas distribution withtheoretical numerical simulations and note that the U shape is consistent with numericalsimulations. We also find that the region of highest temperature of ~100 K or higher inside theU shape corresponds to the spur having an upward flow, additionally heated up either bymagnetic reconnection or bouncing in the interaction with the narrow neck at the bottom of the
U shape. We note these new findings further reinforce the magnetic floatation interpretation.
Tosaki, T., Y. Shioya, N. Kuno, T. Hasegawa, K. Nakanishi, S. Matsushita, and K. Kohno[2008a], "Giant Molecular Association in Spiral Arms of M31 : Evidence for Dense Gas
Formation via Spiral Shock Associated with Density Waves?," Proc. of the "Mapping the
Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F., p.382.
Without abstract
Tosaki, T., R. Miura, T. Sawada, N. Kuno, K. Nakanishi, K. Kohno, S. K. Okumura, S.
Komugi, Y. Tamura, and R. Kawabe [2008b], "NRO 45 M and ASTE 10 M Observations ofDense Gas in Giant HII Regions of M 33," EAS Publication Series, vol.31, pp.211-212.
We present 12CO(J=3-2) and 12CO(J=1-0) observations of the supergiant HII region NGC 604
in the nearest face-on piral galaxy M 33 using the Atacama Submillimeter Telescope
Experiment (ASTE) 10-m and the Nobeyama Radio Observatory (NRO) 45-m telescopes. We
found high 12CO(J=3-2)/12CO(J=1-0) ratio gas with an arc-like distribution ("high-ratio gasarc") surrounding the central star cluster of NGC 604. Our results suggest that dense gas
formation and second-generation star formation occur in the surrounding gas compressed by
the stellar wind and/or supernova of the first-generation stars of NGC 604, i.e., the central starcluster of NGC 604. Thus, NGC 604 is an example of large-scale sequential star formation.
Trushkin, S. A., N. N. Bursov, T. Kotani, N. A. Nizhelskij, M. Namiki, M. Tsuboi, and P. A.
Voitsik, [2007], "Recent Radio Monitoring of Microquasars with RATAN-600 Radio
Telescope," Proceedings of the 6th INTEGRAL workshop "The Obscured Universe", 2-8 July
2006, Moscow, ESA SP-622.
We report about the multi-frequency (1-30 GHz) daily monitoring of the radio flux variabilityof the three microquasars: SS433, GRS1915+105 and Cyg X-3 during the period from
September 2005 to May 2006. 1. We detected clear correlation of the flaring radio fluxes and
X-rays 'spikes' at 2-12 keV emission detected in RXTE ASM from GRS1915+105 during eight
relatively bright (200-600 mJy) radio flares in October 2005. The 1-22 GHz spectra of theseflares in maximum were optically thick at frequencies lower 2.3 GHz and optically thin at thehigher frequencies. During the radio flares the spectra of the X-ray spikes become softer thanthose of the quiescent phase. Thus these data indicated the transitions from very high/hardstates to high/soft ones during which massive ejections are probably happened. These ejections
are visible as the detected radio flares. 2. After of the quiescent radio emission we havedetected a drop down of the fluxes (~20 mJy) from Cyg X-3. That is a sign of the following
bright flare. Indeed such a 1Jy-flare was detected on 3 February 2006 after 18 days of thequenched radio emission. The daily spectra of the flare in the maximum was flat from 1 to 100

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GHz, using the quasi-simultaneous observations at 109 GHz with RT45m telescope andmillimeter array (NMA) of Nobeyama Radio Observatory in Japan. The several bright radio
flaring events (1-10 Jy) followed during this state of very variable and intensive 1-12 keV
X-ray emission (~0.5 Crab), which being monitored in RXTE ASM program.
Trushkin, S., N. Nizhelskij, T. Kotani, N. Kawai, M. Tsuboi, and M. Namiki [2009], "Active
Flaring States of GRS 1915+105 and Cyg X-3 in Radio/X-Ray Monitoring," Proc. of"Astrophysics with All-Sky X-Ray Observations", pp.88-93.
In multi-wavelength collaboration we studied the variability of the microquasars
GRS1915+105 and Cyg X-3 during 2005 to May 2008 with the RATAN-600 radio telescope of
SAO RAS. We detected clear correlation of the flaring radio fluxes and X-rays 'spikes' at 2-12
keV emission redundant in RXTE ASM from GRS1915+105 during eight relatively bright(200-600 mJy) radio flares in October 2005. Spectra of these flares at maximum are opticallythick at frequencies lower than 2.3 GHz and optically thin at the higher frequencies. During theradio flares the spectra of the X-ray spiked become softer than the those of the quiescent phase.
Thus these data indicate the transitions from the very high/hard state to high/soft state during
which massive ejections probably occur. These ejections are detected as radio flares. such
X-ray/radio events correlation detected later in 2006-2008. In December 2005 after of the
4-year quiescent radio state (100-200 mJy) Cyg X-3 entered the softer X-ray with low level of
hard (15-50 keV) X-ray and high (~0.5 crab) in the soft band (1-10 keV). In the following 500
days we have detected more 10 bright (> 1Jy) flaring events correlated with rising phases of
ASM-Swift-BAT intensity of Cyg X-3. A first 1 Jy-flare was detected on 3 February 2006 after
18 days of the quenched radio emission (< 20mJy). The spectrum of the flare at the maximum
id flat from 1 to 100 GHz, obtained the quasi-simultaneous observations with RT45m
telescope and millimeter array (NMA) of Nobeyama Radio Observatory.
Tsai, A. L., S. Matsushita, K. Nakanishi, K. Kohno, R. Kawabe, T. Inui, H. Matsumoto, T. G.
Tsuru, A. B. Peck, and A. Tarchi [2009], "Molecular Superbubbles and Outflows from the
Starburst Galaxy NGC 2146," Publ. Astron. Soc. Japan, vol.61, pp.237-250.
We present results from a deep (1σ = 5.7 mJy beam-1 per 20.8 km s-1 velocity channel)
12CO(1-0) interferometric observation of the central 60" region of the nearby edge-on starburst
galaxy NGC 2146, observed with the Nobeyama Millimeter Array. Two diffuse expanding
molecular superbubbles and one molecular outflow were successfully detected. One molecularsuperbubble, with a size of ~1 kpc and an expansion velocity of ~50 km s-1, is located below
the galactic disk; a second molecular superbubble, with a size of ~700 pc and an expansion
velocity of ~35 km s-1, is also seen in the position ﾐ velocity diagram; the molecular outflow islocated above the galactic disk with an extent of ~2 kpc expanding with a velocity of up to~200 km s-1. The molecular outflow has an arc-like structure, and is located at the front edge ofthe soft X-ray outflow. In addition, the kinetic energy (~3 x 1055 erg) and the pressure ( ~1 x
10-12±1 dyn cm-2) of the molecular outflow are comparable to, or smaller than, that of the hotthermal plasma, suggesting that the hot plasma pushes the molecular gas out from the galactic
disk. Inside the ~1 kpc size molecular superbubble, diffuse soft X-ray emission seems to exist.
However, since the superbubble lies behind the inclined galactic disk, it is largely absorbed by
the molecular gas.
Tsap, Y. T., Y. G. Kopylova, A. V. Stepanov, V. E. Melnikov, and K. Shibasaki [2008],"Ballooning Instability in Coronal Flare Loops," Solar Phys., vol.253, pp.161-172.
Within the framework of ideal magnetohydrodynamics the excitation of the ballooning
instability in a toroidal coronal loop with a radius of cross section a and a radius of curvature R
is analyzed by using the energy method. Kink oscillations are able to excite the ballooning
instability when the plasma beta parameter β>2a/R. It has been suggested that this can resultin the formation of cusp-shaped coronal loops. Modulation of gyrosynchrotron emission

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caused by kink oscillations is considered. The intensity of gyrosynchrotron emission for
optically thin sources is the most sensitive to Alfvén disturbances. The obtained theoreticalresults are discussed in the light of Yohkoh, SOHO, TRACE, RHESSI, and Nobeyama
observations.
Tsuboi, M., A. Miyazaki, and T. Handa [2008a], "The Synchrotron Cut-Off Frequency ofRelativistic Electrons in the Radio Arc and Their Acceleration Area," Proc. of the "Mapping
the Galaxy and Nearby Galaxies", eds. Wada, K., and Combes, F., pp.133-138.
The Galactic Center region is a nearest central region of spiral galaxy. Unique structures which
may relate intrinsic activities in the central region have been found. "gRadio Arc" is a mostoutstanding one of such features. This consists of two parts with different properties. These are
non-thermal "Vertical filament" and thermal "Arched filament" [1]. Although the intensity is
abruptly decreased at the both ends of Vertical filament, the positive galactic latitude extension
corresponds to the base of a famous off-plane feature, "Galactic Center ｽ-shaped lobe", which
was identified by Sofue and Handa (1986) [2]. The lobe also consists of two parts withdifferent properties. The positive longitude part is highly linear polarized up to 50% at 10 GHz,
which is non-thermal, and the negative longitude part is non-polarized, which is presumably
thermal [3]. It is controversial that the lobe is a real combined structure or an apparent featureby chance superposition in the line of sight. On the other hand, the negative galactic latitude
extension is distinctive only in linear polarization map. Two polarized extensions is called"Polarized Lobe" [3]. Radio Arc and Polarized Lobe are presumably a part of large scalepoloidal magnetic field through the Galactic center region. It is, however, an open question
how much is the strength of the magnetic field. In addition, several vertical continuum features
identified in lower frequency map are also a part of such magnetic field [4]. It is also an open
question that such magnetic field exists anywhere in the region or is restricted in smaller
region. The synchrotron cut-off frequency in the Radio Arc and its distribution presumably
provide the informations of the acceleration area of relativistic electrons and the acceleration
mechanism.
Tsuboi, M., T. Tosaki, N. Kuno, K. Nakanishi, T. Sawada, T. Umemoto, S. A. Trushkin, T.
Kotani, N. Kawai, Y. Kurono, T. Handa, K. Kohno, T. Tsukagoshi, O. Kameya, H. Kobayashi,
K. Fujisawa, A. Doi, T. Omodaka, H. Takaba. H. Sudou, K. Wakamatsu, Y. Koyama, E. Kawai,
N. Mochizuki, and Y. Murata [2008b], "The 2006 Radio Outburst of a Microquasar Cyg X-3:
Observation and Data," Publ. Astron. Soc. Japan, vol.60, pp.465-473.
We present the results of the multi-frequency observations of radio outburst of the microquasar
Cyg X-3 in 2006 February and March with the Nobeyama 45-m telescope, the Nobeyama
Millimeter Array, and the Yamaguchi 32-m telescope. Since the prediction of a flare by
RATAN-600, the source was monitored from January 27 (UT) with these radio telescopes. At
the eighteenth day after the quench of the activity, successive flares exceeding 1 Jy weresuccessfully observed. The time scale of the variability in the active phase is presumably
shorter in higher frequency bands. We also present the result of a follow-up VLBI observation
at 8.4 GHz with the Japanese VLBI Network 2.6 days after the first rise. A VLBI image
exhibits a single core with a size of <8 mas (80 AU). The observed image is almost stable,
although the core showed a rapid variation in the flux density. No jet structure can be seen at asensitivity of Tb (brughtness temperature)= 7.5x105 K.
Tsuboi, M., A. Miyazaki, and S. K. Okumura [2009a], "The Galactic Center 50-km s-1
Molecular Cloud with an Expanding Shell," Publ. Astron. Soc. Japan, vol.61, pp.29-37.
We performed high-resolution observations of a Galactic Center 50-km s-1 molecular cloud in
the CS J = 1-0 line using the Nobeyama Millimeter Array (NMA). The molecular cloud mainly
has three different spatial components with large velocity widths of up to 60 km s-1. The
northwest component is located at an apparent contact point to the Sgr A east shell, and

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elongated along the boundary of the shell. The large velocity width of the component is
responsible for interaction with the Sgr A east shell. The molecular gas distribution in CS line
emission is dissimilar to that observed previously in NH3 line emissions. The appearanceshows presumably the area of CS line emission enhanced by shock. The central and southwest
components are located just out of the Sgr A east shell and far from it, respectively. However,these components have large velocity widths. We found a well-shaped circular molecular shellwith expanding motion in the 50-km s-1 molecular cloud. This is responsible for the large
velocity width. The continuum source in the expanding molecular shell has a steep spectrum in
mm-wavelengths, although this was not identified in a previous 5-GHz map. This source may
be an SNR with an ionized sheath. From the aspect ratio of an expanding molecular shell of
1.1, the magnetic field in/around the shell is estimated to be smaller than 100μ Gauss. This
weak magnetic field is consistent with on-going active star formation in the 50-km s-1
molecular cloud. A comparison among CS line emission, low-frequency continuum, andmillimeter
continuum toward the 50-km s-1 molecular cloud suggests a face-on view of the Sgr A region.
The molecular cloud is located in the Sgr A halo region.
Tsuboi, M., A. Miyazaki, K. Nakanishi, K. Kamegai, and T. Kotani [2009b], "A MM-Wave
Flare from Cyg X-3," The Astronomer's Telegram, #2053.
We report that the microquasar Cyg X-3 (20:32:25.77, 40:57:27.97, J2000) is currently
undergoing a mm-wave flare. A peak activity exceeding 0.4 Jy at 43 GHz has been detectedwith the 45-m telescope of the Nobeyama Radio Observatory at 2009/05/20 20:40 (UT),
followed by a decay with an e-folding time of 150 min. At 86 GHz, the peak is higher than 0.3
Jy, and the rise and decay profile shows a more complicated structure.
Tsuboi, M., and T. Handa [2010], "Highly Polarized Counterpart of the Double Helix Nebula,"
Astrophys. J. (Letters), vol.719, pp.L177-L180.
We identified the double helix nebula (DHN) found by the Spitzer Space Telescopein the
Galactic center region as a highly polarized feature at 10 GHz with the Nobeyama 45 m
telescope. The DHN is located near the north end of the polarized plumes. The position anglesof Faraday rotation corrected B vectors in the DHN are presumably along the twisting IR
filaments. The linear polarization degree of the DHN is as large as p = 10%, and reaches p =15% ± 2% at the radio polarization peak of the DHN. This means that the DHN has highlyordered magnetic field with synchrotron-emitting relativistic electrons.
Ueda, K., H. Imai, S. Deguchi, R. Kamohara, T. Maeda, N. Matsumoto, and T. Omodaka[2008], "Japanese VLBI Network Observations of SiO Masers in the M-Type Giant IRC
10414," Publ. Astron. Soc. Japan, vol.60, pp.1051-1056.
We present two-epoch maps of SiO masers (ν=1 and ν=2, J=1-0) associated with the M-typestar IRC-10414, which were obtained with the Japanese VLBI Network (JVN). The spatial an
Doppler velocity distributions, and the intensity ratio of the ν=1 to ν=2 (J=1-0) lines havesignificantly changed for eight years since our previous Very Long Baseline Array (VLBA)
observation, The maser proper motions revealed by these two-epoch observations with aninterval of one month are quite random and too fast to be explained by ballistic motions of themaser clumps. The maser distributions seen in the present observations cannot be explained bya rotating-infalling ring model implied in the previous work. We discuss the kinematical
relation between the SiO and H2O masers in IRC-10414. In the present observations, the scale
sizes of SiO ν=1 and ν=2 masers in IRC-10414 were roughly equal, as observed in typical
Mira variables.
Ujihara, H., and T. Bushimata [2009a], "Measurement of the Antenna Mesh: Characteristics
for VSOP-2/ASTRO-G," Proc. of the "Approaching Micro-Arcsecond Resolution with
VSOP-2: Astrophysics and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and

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Murata, Y., ASP Conf. Ser. vol.402, pp.66-69.
The surface of the main reflector antenna of the VSOP-2 satellite is made of metal wire that is
woven into a tense mesh. Numerical simulations are required to determine the reflectivity
characteristics of the mesh which are functions of the reflecting angle, polarization andfrequency of the incident radio wave and the tension of the mesh. These characteristics were
measured with the tension of 200g/m, 350g/m, 500g/m.
Ujihara, H. [2009b], "Designs and Development of Multimode Horns for ASTRO-G/VSOP-2
Satellite," Proc. of the "Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics
and Technologies", eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf.
Ser. vol.402, pp.70-73.
The antenna optics of VSOP-2 satellite require low cross polarization, and the volume of thereceiver box is limited. Thus, instead of conventional corrugated horns, multimode horns were
proposed and designed in order to reduce the axial length and weight of the horns but stillcompatible with a low cross polarization. These multimode horns were designed for threeobservational bands of VSOP-2 at 8GHz, 22GHz, 43GHz, all with about the same antenna
illumination size. However, the ratio of waveguide and wavelength are slightly different. The
22GHz-horn was designed at first, and the other horns were arranged around it. The propertiesof the horns were improved by controlling the complex amplitude of higher modes and byfitting the beam width to the antenna optics. The BBM models of horns were tested, and theirmeasured beam patterns agree well with numerical simulations.
Ukita, N., H. Ezawa, B. Ikenoue, and M. Saito [2007], "Thermal and Wind Effects on the
Azimuth Axis Tilt of the ASTE 10-m Antenna," Publ. Natl. Obs. Japan, vol.10, pp.25-33.
The azimuth axis title of the ASTE 10-m antenna induced by thermal and wind loading wasinvestigated with a dual-axis inclinometer on the azimuth axis, along with thermometers on thepedestal and yoke structures and an ultrasonic anemometer on a nearby station. The
dependence of the inclinometer zero-point offsets against temperature of the device,temperature gradients in the pedestal and yoke structure were obtained for the measurements
over 11 months during the antenna being parked at its home position (azimuth angles = ±180
degrees, an elevation angle = 60 degrees) under wind velocities < 8 m s-1. The temperaturedependences of the zero-point offsets were found to be 1.24 and -0.46 arcseconds/degree, andwere close to those obtained with an independent method. The azimuth axis tilts due to thetemperature difference between the two opposite sides of pedestal walls were found to beabout 1.1 and 1.7 arcseconds/degree, and consistent with 1.5 arcseconds/degree estimated witha simple model. The residual axis tilt of the whole samples after removal of the temperaturedependences shows dependence against overturning moment estimated from the wind data.
The stiffness of the antenna structures between the yoke base section and the ground wasestimated to be 5.3 and 3.4 GNm/rad using the observed tilts in two directions; and were
smaller than 6/0 GNm/rad from a mechanical model prediction. Based on these field
experiments, we discuss the improvements and limitations of pointing performance with theinclinometer metrology system.
Ukita, N., B. Ikenoue, and M. Saito [2008a], "Optical Seeing Measurements with an Optical
Telescope on a Radio Antenna," Publ. Natl. Astron. Obs. Japan, vol.11, pp.1-11.
Individual images of a video CCD camera with a 10-cm objective lens recorded for pointing
performance tests of a prototype 12-m antenna for the ALMA project have been analyzed toevaluate both antenna tracking accuracy and optical seeing at the NRAO VLA site. Data of star
image centroid motion have been compared with readouts of angle encoders and inclinomterson the azimuth axis in the yoke structure of the antenna. Under good tracking conditions, a
power spectral density (PSD) of image motion during tracking over about 5 minutes had a
Kolmogorov power index of -2/3. At frequencies > 4 Hz, the PSD showed a steeper decline

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due to a finite exposure time of the video camera (1/30 seconds) than -2/3, which suggests awind speed of about 3 m s-1 at the level where the main turbulence occurs. At lower
frequencies, a flattening of the PSD was observed with a turnover frequency of about 0.05 Hz,
which in turn suggests an "outer scale" of about 60 m, a length of large-scale disturbances inKolmogorov's model. The image centroid fluctuations observed during all-sky pointing tests
showed a dependence on air mass A as A0.5 and were 0.5 to 0.9 arcseconds rms at the zenith.
These measurements suggest that observations for 2-3 seconds can determine a star position
with a typical error of 0.3 to 0.6 arcseconds.
Ukita, N. [2008b], "Wind Induced Surface Deformation of the Nobeyama 45-m Radio
Telescope," Proc. of the SPIE, vol.7012, pp.70120V-1-11.
Reflector surface deformation due to wind loading on the Nobeyama 45-m antenna has beenmeasured with four LED lamps on the surface at r = 20 m and two CCD cameras on the central
hub as it rotates in azimuth with elevation angles of 90 and 11 degrees. The side-wind loadingof 8.4 m s-1 caused a tilt of 12 arcseconds and an astigmatic deformation of 0.8 mm. The frontand back-wind loading of 9.9 m s-1 induced a vertical displacement variation of 2.3 mm. Theselargescale surface deformation profiles have been compared with those of finite element
calculations and coefficients of axial force and yaw moment predicted by a JPL wind tunnel
data excerpt.
Ukita, N., H. Ezawa, S. Onodera, and M. Saito [2010], "Wind-Induced Pointing Errors andSurface Deformation of a 10-m Submillimeter Antenna," J. Proc. of the SPIE, vol.7733,
pp.77331D-77331D-11.
Two types of field measurements on the Atacama Submillimeter Telescope Experiment 10-m
antenna have been made to diagnose antenna oscillations in strong wind gusts and to reduce
pointing errors due to static/quasi-static wind loadings. The measurements with seismic
accelerometers on the reflector have been compared with those from axis angle encoders. Our
results have confirmed that the dominant wind effects are at low frequencies, and have foundthat twist and pitching motion of yoke arms are the dominant source of pointing jitters anddecrease with frequency along the Kolmogorov slope of -5/3. In the range from about 1 to 10
Hz, the servo-loop excites and dominates pointing error oscillations. For azimuth oscillations,the frontal wind has the largest effects, compared with side- or tail-wind. To improve pointing
performance against static/quasi-static wind effects, we have implemented and tested an
auxiliary auto-pointingcorrection system with a lookup table compiled from all-sky pointing
measurements under strong winds, invoking the Taylor's "frozen turbulence" hypothesis. We
have successfully demonstrated that use of upwind data from a nearby anemometer helps toreduce the pointing errors of static wind effects from 2.4 " rms (correction OFF) to 1.2 " rms(correction ON) under a mean wind speed of 9.3 m s-1.
Umemoto, T., N. Mochizuki, K. M. Shibata, D.-G. Roh, and H.-S. Chung [2008], "Millimetre
Wavelength Methanol Masers Survey towards Massive Star Forming Regions," Proc. of theIAU Symp. 242, "Astrophysical Masers and their Environments", eds. Jessica Chapman andWillem Baan, pp.234-235.
We present the results of a mm wavelength methanol maser survey towards massive star
forming regions. We have carried out Class II methanol maser observations at 86.6 GHz, 86.9
GHz and 107.0 GHz, simultaneously, using the Nobeyama 45 m telescope. We selected 108
6.7 GHz methanol maser sources with declinations above -25 degrees and fluxes above 20 Jy.
The detection limit of maser observations was ~3 Jy. Of the 93 sources surveyed so far, wedetected methanol emission in 25 sources (27%) and "maser" emission in nine sources (10%),of which thre "maser" sources are new detections. The detection rate for maser emission isabout half that of a survey of the southern sky (Caswell et al. 2000). There is a correlation
between the maser flux of 107 GHz and 6.7 GHz/12 GHz emission, but no correlation with the

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"thermal" (non maser) emission. From results of other molecular line observations, we foundthat the sources with methanol emission show higher gas temperatures and twice the detection
rate of SiO emission. This may suggest that dust evaporation and destruction by shock areresponsible for the high abundance of methanol molecules, one of the required physicalconditions for maser emission.
Umemoto, T., M. Saito, K. Nakanishi, N. Kuno, and M. Tsuboi [2009], "Detection of a Radio
Flare at Millimeter-Wavelengths from the X-Ray T Tauri Star V773 Tau," Proc. of the"Approaching Micro-Arcsecond Resolution with VSOP-2: Astrophysics and Technologies",
eds. Hagiwara, Y., Fomalont, Ed., Tsuboi, M., and Murata, Y., ASP Conf. Ser. vol.402,
pp.400-403.
We present the results of multi-frequency observations of a radio flare in the young stellar
object (YSO) V773 Tau, which is probably a weak-line T Tauri star. We carried out radio
continuum observations at 22 GHz, 43 GHz and 86 GHz, using the Nobeyama 45 m telescope,and detected a radio flare at all frequencies. The radio flare occurred near periastron passage,
and the flux density became 4 to 10 times higher, then rapidly decreased at 43 and 86 GHz
within a few hours. The radio spectrum was rising (brighter at higher frequency) during theflare. On the other hand, the radio continuum at 22 GHz was detected even 28 hours later atmore than 2 mJy. Thus, the active phase is surprisingly long at 22 GHz. V773 Tau is the mostpromising target for detailed imaging of the magnetosphere with the next space VLBI project
VSOP-2.
Uralov, A. M., V. V. Grechnev, I. G. Rudenko, and H. Nakajima [2008], "Microwave Neutral
Line Associated Source and a Current Sheet," Solar Phys., vol.249, pp.315-335.
Neutral Line associated Sources (NLSs) are quasi-stationary microwave sources projected onto
vicinities of the neutral line of the photospheric magnetic field. NLSs are often precursors of
powerful flares, but their nature is unclear. We endeavor to reveal the structure of an NLS andto analyze a physical connection between such a source with a site of energy release in thecorona above NOAA 10488 (October/November 2003). Evolution of this AR includes
emergence and collision of two bipolar magnetic structures, rise of the main magnetic
separator, and the appearance of an NLS underneath. The NLS appears at a contact site ofcolliding sunspots, whose relative motion goes on, resulting in a large shear along a tangent.
Then the nascent NLS becomes the main source of microwave fluctuations in the AR. The
NLS emission at 17 GHz is dominated by either footpoints or the top of a loop-like structure,an NLS loop, which connects two colliding sunspots. During a considerable amount of time,the emission dominates over that footpoint of the NLS loop, where the magnetic field isstronger. At that time, the NLS resembles a usual sunspot-associated radio source, whosebrightness center is displaced towards the periphery of a sunspot. Microwave emission of an
X2.7 flare is mainly concentrated in an ascending flare loop, initially coinciding with the NLS
loop. The top of this loop is located at the base of a non-uniform bar-like structure visible insoft X-rays and at 34 GHz at the flare onset. We reveal i) upward lengthening of this bar
before the flare onset, ii) the motion of the top of an apparently ascending flare loop along theaxis of this bar, and iii) a non-thermal microwave source, whose descent along the bar was
associated with the launching of a coronal ejection. We connect the bar with a probableposition of a nearly vertical diffusion region, a site of maximal energy release inside anextended pre-flare current sheet. The top of the NLS loop is located at the bottom of thisregion. A combination of the NLS loop and diffusion region constitutes the skeleton of aquasi-stationary microwave NLS.
Vila-Vilaro, B. [2008], "Rare CO Isotope Observations of M51a (NGC5194)," Publ. Astron.
Soc. Japan, vol.60, pp.1231-1248.
We present observations of the central regions of M 51a (NGC 5194) in the J = 1-0 rotational

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transitions of 13CO, C18O, and C17O. The last two are the ﾞ rst detections reported for thisobject. We have combined these data with published HCN and CO(J = 1-0) observations withthe same telescope to carry out some LVG modeling (single-cloud and two-cloud mixtures) of
the line ratios. The results are compatible with the presence of a region emitting most of the
HCN and another component at lower temperatures and densities emitting most of the rest of
the molecular emission. The observed high C18O/C17O ratio, together with our models, suggestthat this is caused by an underabundance of [C17O] (compared with Galactic values). This canbe explained by different evolutionary histories. The C18O emission line has a clearly
asymmetric profile, implying the presence of significant excitation differences within theobserved region. Finally, there is an indication that the CO(1-0) is overestimating themolecular gas mass in the central kpc of this galaxy. This is similar to what is found in the
Milky Way at similar spatial scales, and possibly associated with a change in the conversion
factor due to the average cloud properties in the central regions of this object.
Wajima, K., N. Kawaguchi, Y. Murata, and H. Hirabayashi [2007], "Radiation Testing ofConsumer High-Speed LSI Chips for the Next Space VLBI Mission," Publ. Astron. Soc. Japan,
vol.59, pp.1221-1226.
We performed two types of radiation testing on high-speed LSI chips to test their suitability foruse in wideband observations by the Japanese next space VLBI mission, VSOP-2. In the total
ionization dose experiment we monitored autocorrelation spectra which were taken with
irradiated LSI chips and the source current at intervals up to 1,000 hours from the ionizationdose, but we could not see any change of these features for the chips irradiated with dose rates
expected in the VSOP-2 mission. In the single event effect experiment, we monitored the crosscorrelation phase and power spectra between the data from radiated and non-radiated devices,and the source current during the irradiation of heavy-ions. We observed a few tens of single
event upsets as discrete delay jumps for each LSI. We estimated the occurrence rate of single
events in space as between once a few days to once a month. No single event latch-up wasseen in any of the LSIs. These results show that the tested LSIs have sufficient tolerance to theenvironment for space VLBI observations.
Wilson, G. W., I. Aretxaga, D. Hughes, H. Ezawa, J. E. Austermann, S. Doyle, I.
Hernandez-Curiel, R. Kawabe, T. Kitayama, K. Kohno, A. Kuboi, H. Matsuo, P. D. Mauskopf,
Y. Murakoshi, A. Montana, P. Natarjan, T. Oshima, N. Ota, T. Perera, J. Rand, K. S. Scott, K.
Tanaka, M. Tsuboi, C. C. Williams, and M. S. Yun [2008], "A Bright, Dust-Obscure,Millimeter-Selected Galaxy Beyond the Bullet Cluster (1E0657-56)," Mon. Not. Roy. Astron.
Soc., vol.390, pp.1061-1070.
Deep 1.1 mm continuum observations of 1E0657-56 (the 'Bullet Cluster') taken with themillimeter-wavelength camera AzTEC on the 10-m Atacama Submillimeter Telescope
Experiment (ASTE), have revealed an extremely bright (S1.1 mm= 15.9 mJy) unresolved
source. This source, MMJ065837-5557.0, lies close to a maximum in the density of underlying
mass distribution, towards the larger of the two interacting clusters as traced by the
weak-lensing analysis of Clowe et al. Using optical-infrared (IR) colours, we argue that
MMJ065837-5557.0 lies at a redshift of z= 2.7 ± 0.2. A lensing-derived mass model for the
Bullet Cluster shows a critical line (caustic) of magnification within a few arcsec of the
AzTEC source, sufficient to amplify the intrinsic millimetre-wavelength flux of the AzTEC
galaxy by a factor of ∼20. After subtraction of the foreground cluster emission at 1.1mm dueto the Sunyaev-Zel'dovich effect, and correcting for the magnification, the rest-frame far-IR
luminosity of MMJ065837-5557.0 is ≤1012 Lsolar, characteristic of a luminous infrared galaxy(LIRG). We explore various scenarios to explain the colours, morphologies and positional
offsets between the potential optical and IR counterparts, and their relationship with
MMJ065837-5557.0. Until higher resolution and more sensitive (sub)millimetre observations

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are available, the detection of background galaxies close to the caustics of massive lensing
clusters offers the only opportunity to study this intrinsically faint millimetre-galaxy
population.
Winnberg, A., S. Deguchi, M. J. Reid, J. Nakashima, H. Olofsson, and H. H. J. Habing [2009],"CO in OH/IR Stars to the Galactic Centre," Astron. Astrophys., vol.497, pp.177-181.
Most stars form in Giant Molecular Clouds (GMCs) and regulate the evolution of galaxies invarious respects. The formed stars affect the surrounding materials strongly via their UVphotons, stellar winds, and supernova explosions, which lead to trigger the formation of
next-generations of stars in the GMCs. It is therefore crucial to reveal the distribution andproperties of GMCs in a galaxy. The Magellanic System is a unique target to make suchdetailed comprehensive study of GMCs. This is because it is nearby and the LMC is nearlyface-on, making it feasible to unambiguously identify associated young objects within GMCs.
Recent millimeter and sub-millimeter observations in the Magellanic System have started toreveal the distribution and properties of the individual GMCs in detail and their relation to starformation activities. From the NANTEN CO surveys, three types of GMCs can be classified interms of star formation activities; Type I is starless, Type II is with H ii regions only, and TypeIII is associated with active star formation indicated by huge H ii regions and young starclusters. The further observations to obtain detailed structure of the GMCs by Mopra and
SEST and to search for the dense cores by ASTE and NANTEN2 in higher tansition lines of
CO have been carried out with an angular resolution of about 5 to 10 pc. These observations
revealed that the differences of the physical properties represent an evolutionary sequence of
GMCs in terms of density increase leading to star formation. Type I and II GMCs are at theearly phase of star formation where density does not yet become high enough to show active
star formation, and Type III GMCs represent the later phase where the average density is
increased and the GMCs are forming massive stars.
Wong, T., A. Hughes, Y. Fukui, A. Kawamura, N. Mizuno, J. Ott, E. Muller, J. L. Pineda, D. E.
Welty, S. Kim, Y. Mizuno, M. Murai, and T. Onishi [2009], "Molecular and Atomic Gas in the
Large Magellanic Cloud. I. Conditions for CO Detection," Astrophys. J., vol.696, pp.370-384.
We analyze the conditions for detection of CO(1-0) emission in the Large Magellanic Cloud,using the recently completed second NANTEN CO survey. In particular, we investigate
correlations between CO integrated intensity and H I integrated intensity, peak brightness
temperature, and line width at a resolution of 2.'6 (~40 pc). We find that significant H I column
density (exceeding ~1021 cm-2) and peak brightness temperature (exceeding ~20 K) arenecessary but not sufficient conditions for CO detection, with many regions of strong H Iemission not associated with molecular clouds. The large scatter in CO intensities for a given
H I intensity persists even when averaging on scales of >200 pc, indicating that the scatter is
not solely due to local conversion of H I into H2 near GMCs. We focus on two possibilities toaccount for this scatter: either there exist spatial variations in the I(CO) to N(H2) conversion
factor, or a significant fraction of the atomic gas is not involved in molecular cloud formation.
A weak tendency for CO emission to be suppressed for large H I linewidths supports thesecond hypothesis, insofar as large linewidths may be indicative of warm H I, and calls into
question the likelihood of forming molecular clouds from colliding H I flows. We also find thatthe ratio of molecular to atomic gas shows no significant correlation (or anticorrelation) withthe stellar surface density, though a correlation with midplane hydrostatic pressure Ph is foundwhen the data are binned in Ph. The latter correlation largely reflects the increasing likelihoodof CO detection at high H I column density.
Yamada, M., K. Wada, and K. Tomisaka [2009], "Three dimensional Line Transfer Study ofEnergy Sources in Compact Molecular Gas in Active Galaxies - AGN/Starburst Connection-,"Proc. of the "The starburst-AGN connection", eds. Weimin Wang, Zhaoqing Yang, Zhijian Luo,

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and Zhu Chen, ASP Conf. Ser., vol.408, pp.254-258.
Recent observations suggest molecular line ratios in millimeter and submillimeter bands may
be a good tool to reveal the long-standing question on the origin of energy sources in obscured
active galaxies ﾐ AGN and/or starburst. Observations of actual molecular medium show in
general inhomogeneous structures as well as high-resolution hydrodynamic simulations do. Inorder for precise interpretation of emergent line emission from the inhomogeneous molecular
gas to probe the dominant energy source of active galaxies, we study characteristic features of
emergent intensities via three-dimensional non-LTE (non-local thermodynamic equilibrium)line transfer simulations. Our results succeeded in making clear 1) the necessary conditions for
HCN/HCO+-dichotomy, and 2) importance of clumpiness on intensity ratio and its
interpretation. These results are obtained for the first time by our realistic three-dimensional
simulations, and line transfer simulations will be a powerful tool to comprehensive studies ofextragalactic interstellar medium (ISM) in forthcoming ALMA (Atacama Large
Millimeter/submillimeter Array) era.
Yamamoto, S., R. Nakamura, T. Matsunaga, Y. Ogawa, Y. Ishihara, T. Morota, N. Hirata, M.
Ohtake, T. Hiroi, Y. Yokota, and J. Haruyama [2010a], "Global Distribution of Olivine
Exposures on the Moon Revealed by SELENE Spectral Profile," LPI Contribution No. 1533,
p.1646.
Here, we report the global distribution of olivine exposures, possibly originating from the lunar
mantle as discovered by Spectral Profiler onboard the Japanese lunar explorer SELENE(Kaguya).
Yamamoto, S., F. Nakamura, T. Matsunaga, Y. Ogawa, Y. Ishihara, T. Morota, N. Hirata, M.
Ohtake, T. Hiroi, Y. Yokota, and J. Haruyama [2010b], "Possible Mantle Origin of Olivine
Lunar Impact Basins Detected by SELENE," Nature Geosci., vol.3, pp.533-536.
The composition, structure and evolution of the Moon's mantle is poorly constrained. The
mineral olivine, one of the main constituents of Earth's mantle, has been identified by
Earth-based telescopic observations at two craters on the near side of the Moon, Aristarchus
and Copernicus. Global reflectance spectra in five discrete spectral bands produced by the
spacecraft Clementine suggested several possible olivine-bearing sites, but one of thecandidate occurrences of olivine was later re-classified, on the basis of continuous reflectancespectra over the entire 1 m band, as a mixture of plagioclase and pyroxene. Here we present a
global survey of the lunar surface using the Spectral Profiler onboard the lunar explorer
SELENE/Kaguya. We found many exposures of olivine on the Moon, located in concentric
regions around the South Pole-Aitken, Imbrium and Moscoviense impact basins where thecrust is relatively thin. We propose that these exposures of olivine can be attributed either to an
excavation of the lunar mantle at the time of the impacts that formed the basins, or tomagnesium-rich pluton in the Moon's lower crust. On the basis of radiative transfer modelling,
we suggest that at least some of the olivine detected near impact basins originates from upper
mantle of the Moon.
Yan, J., J. Ping, K. Matsumoto, and F. Li [2008], "The Simulation of Lunar Gravity Field
Recovery from D-VLBI of Chang'E-1 and SELENE Lunar Orbiters," Adv. Sp. Res., vol.42,
pp.337-340.
The lunar gravity field is a foundation to study the lunar interior structure, and to recover theevolution history of the Moon. It is still an open and key topic for lunar science. For above
mentioned reasons, it becomes one of the important scientific objectives of recent lunar
missions, such as KAGUYA (SELENE) the Japanese lunar mission and Chang'E-1, theChinese lunar mission. The Chang'E-1 and the SELENE were successfully launched in 2007. Itis estimated that these two missions can fly around the Moon longer than 6 months
simultaneously. In these two missions, the Chinese new VLBI (Very Long Baseline

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Interferometry) network will be applied for precise orbit determination (POD) by using a
differential VLBI (D-VLBI) method during the mission period. The same-beam D-VLBI
technique will contribute to recover the lunar gravity field together with other conventional
observables, i.e. R&RR (Range and Range Rate) and multi-way Doppler. Taking VLBI
tracking conditions into consideration and using the GEODYNII/SOVLE software of
GSFC/NASA/USA [[Rowlands et al., 1997] and [Ullman, 1994]], we simulated the lunar
gravity field recovering ability with and without D-VLBI between the Chang'E-1 and SELENE
main satellite. The cases of overlapped flying and tracking period of 30 days, 60 days and 90
days have been analyzed, respectively. The results show that D-VLBI tracking between two
lunar satellites can improve the gravity field recovery remarkably. The results and methods
introduced in this paper will benefit the actual missions.
Yasui, C., N. Kobayashi, A. T. Tokunaga, and M. Saito [2008], "Extreme Outer Galaxy: A
Laboratory of Star Formation in an Early Epoch of the Galaxy's Formation," Proc. of the"Panoramic views of galaxy formation and evolution", eds. T. Kodama, T. Yamada, and K.
Aoki, ASP Conf. Ser. vol.399, pp.481-482.
The extreme outer Galaxy (EOG) has a very different environment from that in the solar
neighborhood, and is an excellent laboratory for the study of the star formation processes that
happened during the formation period of the Galaxy. In particular, the study of the EOG may
shed light on the origin and role of the thick disk, whose metallicity range matches well withthat of the EOG. Through a detailed near-infrared (NIR) study of Cloud 2, one of the most
distant star-forming regions in the EOG, we show that key star-formation items, such as theinitial mass function (IMF) and star-formation efficiency, in such a potentially "primordial"
environment can be studied in detail. We are continuing a detailed study of a number ofstar-forming regions in the EOG, mostly with wide-field NIR imaging using Subaru Telescope.
It turns out that NIR imaging is the most efficient way to find star formation activity in such
distant regions.
Yasui, C., N. Kobayashi, A. T. Tokunaga, M. Saito, and C. Tokoku [2009], "Disk Fraction in a
Low-Metallicity Environment," Proc. of the "Exoplanets and disks: their formation anddiversity", eds. Usuda, T., Tamura, M., and Ishii, M., AIP Conf. Proc., vol.1158, pp.171-172.
The extreme outer galaxy (EOG), at a galactic radius of more than 18 kpc, is known to havevery low metallicity. We find that in two very young (~0.5 Myr) star-forming clusters in the
EOG the fraction of stars with near-infrared excess is significantly lower than for those in thesolar neighborhood. Our results suggest that most stars forming in the low-metallicity
environment experience disk dispersal at an earlier stage (<1 Myr) than those forming in thesolar metallicity environment (as much as ~5-6 Myr).
Yoda, T., T. Handa, K. Kohno, T. Nakajima, M. Kaiden, Y. Yonekura, H. Ogawa, and J.-I.
Morino, [2010], "The AMANOGAWA-2SB Galactic Plane Syrvey I. Data on Galactic
Equator," Publ. Astron. Soc. Japan, vol.62, pp.1277-1289.
Using a waveguide-type sideband-separating receiver (2SB receiver) on the Tokyo-NRO
60-cm telescope (renamed the AMANOGAWA telescope), we carried out simultaneous
observations in the 12CO (J=2-1) and 13CO (J=2-1) lines over the galactic plane l=0°-245｡
along b=0° with a 3'.75 grid. Using the 12CO (J=1-0) data of Dame et al. (2001, ApJ, 547, 792),
who used a beam size almost the same as ours, we show 12CO (J=2-1)12CO (J=1-0) and 13CO
(J=2-1)12CO (J=2-1) intensity ratios on the l-v map and the intensity correlations among the12
CO (J=2-1), 13CO (J=2-1), and 12CO (J=1-0) lines. As a result, a linear correlation between
12
CO (J=2-1) and 12CO (J=110) and a curved correlation between 12CO (J=2-1) and 13CO
(J=2-1), as produced by most of the data, have been found. We investigated these correlations
with simple radiative transfer equations to ascertain a number of restrictions on the physicalquantities of molecular gas on a galactic scale.

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Yokota, Y., T. Matsunaga, M. Ohtake, J. Haruyama, R. Nakamura, S. Yamamoto, Y. Ogawa, T.
Morota, T. Honda, K. Saiki, K. Nagasawa, K. Kitazato, S. Sasaki, A. Iwasaki, H. Demura, and
N. Hirata [2010], "Pefinement of Lunar Vis/NIR Phase Curve Acquired by SELENE Spectral
Profiler," LPI Contribution No. 1533, p.2532.
The SELENE Spectral Profiler (SP) acquired lunar visible to NIR spectral data at a spatial
resolution of 500 m. we report refined results of the phase curves derived from SP data.
Yoshida, A., Y. Kitamura, Y. Shimajiri, and R. Kawabe [2010], "Dependence of the Turbulent
Velocity Field on Gas Density in L1551," Astrophys. J., vol.718, pp.1019-1035.
We have carried out mapping observations of the entire L1551 molecular cloud with about 2
pc x 2 pc size in the 12CO(1-0) line with the Nobeyama 45 m radio telescope at the higheffective resolution of 22'' (corresponding to 0.017 pc at the distance of 160 pc), and analyzed
the 12CO data together with the 13CO(1-0) and C18O(1-0) data from the Nobeyama Radio
Observatory database. We derived the new non-thermal line width-size relations, σNT vprop Lν,for the three molecular lines, corrected for the effect of optical depth and the line-of-sightintegration. To investigate the characteristic of the intrinsic turbulence, the effects of theoutflows were removed. The derived relations are (σNT/km s-1) = (0.18 ± 0.010)(L/pc)0.45 ± 0.095,(0.20 ± 0.020)(L/pc)0.48 ± 0.091, and (0.22 ± 0.050) (L/pc)0.54 ± 0.21 for the 12CO, 13CO, and C18O
lines, respectively, suggesting that the line width-size relation of the turbulence very weakly
depends on our observed molecular lines, i.e., the relation does not change between the density
ranges of 102-103 and 103-104 cm-3. In addition, the relations indicate that incompressible
turbulence is dominant at the scales smaller than 0.6 pc in L1551. The power spectrum indicesconverted from the relations, however, seem to be larger than that of the Kolmogorov spectrum
for incompressible flow. The disagreement could be explained by the anisotropy in the
turbulent velocity field in L1551, as expected in MHD turbulence. Actually, the autocorrelation
functions of the centroid velocity fluctuations show larger correlation along the direction of themagnetic field measured for the whole Taurus cloud, which is consistent with the results ofnumerical simulations for incompressible MHD flow.
Yusef-Zadeh, F., H. Bushouse, M. Wardle, C. Heinke, D. A. Roberts, C. D. Dowell, A.
Brunthaler, M. J. Reid, C. L. Martin, D. P. Marrone, D. Porquet, N. Grosso, K. Dodds-Eden, G.
C. Bower, H. Wiesemeyer, A. Miyazaki, S. Pal, S. Gillessen, A. Goldwurm, G. Trap, and H.
Maness [2009], "Simultaneous Multi-Wavelength Observations of Sgr A* during 2007 April
1-11," Astrophys. J., vol.706, pp.348-375.
We report the detection of variable emission from Sgr A* in almost all wavelength bands (i.e.,
centimeter, millimeter, submillimeter, near-IR, and X-rays) during a multi-wavelength
observing campaign. Three new moderate flares are detected simultaneously in both near-IR
and X-ray bands. The ratio of X-ray to near-IR flux in the flares is consistent with inverse
Compton scattering of near-IR photons by submillimeter emitting relativistic particles which
follow scaling relations obtained from size measurements of Sgr A*. We also find that the flarestatistics in near-IR wavelengths is consistent with the probability of flare emission being
inversely proportional to the flux. At millimeter wavelengths, the presence of flare emission at
43 GHz (7 mm) using the Very Long Baseline Array with milliarcsecond spatial resolution
indicates the first direct evidence that hourly timescale flares are localized within the inner
30x70 Schwarzschild radii of Sgr A*. We also show several cross-correlation plots between
near-IR, millimeter, and submillimeter light curves that collectively demonstrate the presenceof time delays between the peaks of emission up to 5 hr. The evidence for time delays at
millimeter and submillimeter wavelengths are consistent with the source of emission initiallybeing optically thick followed by a transition to an optically thin regime. In particular, there isan intriguing correlation between the optically thin near-IR and X-ray flare and optically thickradio flare at 43 GHz that occurred on 2007 April 4. This would be the first evidence of a radio

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flare emission at 43 GHz delayed with respect to the near-IR and X-ray flare emission. The
time delay measurements support the expansion of hot self-absorbed synchrotron plasma bloband weaken the hot spot model of flare emission. In addition, a simultaneous fit to 43 and 84
GHz light curves, using an adiabatic expansion model of hot plasma, appears to support a
power law rather than a relativistic Maxwellian distribution of particles.
Zhu, M., P. P. Papadopoulos, M. Xilouris, N. Kuno, and U. Lisenfeld [2009], "Is the Gas andDust Mass Over-Estimated in the Starburst Galaxy NGC 3310?," Proc. of the "The
starburst-AGN connection", eds. Weimin Wang, Zhaoqing Yang, Zhijian Luo, and Zhu Chen,ASP Conf. Ser., vol.408, pp.76-79.
We present a new observational study of the gas and dust properties in the starburst galaxy
NGC 3310.
Zhu, M., P. P. Papadopoulos, E. M. Xilouris, N. Kuno, and U. Lisenfeld [2009], "Tracing
Molecular Gas Mass in Extreme Extragalactic Environments: An Observational Study,"
Astrophys. J., vol.706, pp.941-959.
We present a new observational study of the 12CO(1-0) line emission as an H2 gas mass tracer
under extreme conditions in extragalactic environments. Our approach is to study the fullneutral interstellar medium (H2, HI, and dust) of two galaxies whose bulk interstellar medium(ISM) resides in environments that mark (and bracket) the excitation extremes of the ISM
conditions found in infrared luminous galaxies, the starburst NGC 3310, and the quiescentspiral NGC 157. Our study maintains a robust statistical notion of the so-called X = N(H2)/ICO
factor (i.e., a large ensemble of clouds is involved) while exploring its dependence on the very
different average ISM conditions prevailing within these two systems. These are constrainedby fully sampled 12CO(3-2) and 12CO(1-0) observations, at a matched beam resolution ofhalf-power beam width ~15'', obtained with the James Clerk Maxwell Telescope (JCMT) on
Mauna Kea (Hawaii) and the 45 m telescope of the Nobeyama Radio Observatory in Japan,
combined with sensitive 850μm and 450μm dust emission and H I interferometric images
which allow a complete view of all the neutral ISM components. Complementary 12CO(2-1)
observations were obtained with the JCMT toward the center of the two galaxies. We found an
X factor varying by a factor of 5 within the spiral galaxy NGC 157 and about two times lower
than the Galactic value in NGC 3310. In addition, the dust emission spectrum in NGC 3310
shows a pronounced submillimeter "excess." We tried to fit this excess by a cold dust
component but very low temperatures were required (TC ~ 5-11 K) with a correspondingly low
gas-to-dust mass ratio of ~5-43. We furthermore show that it is not possible to maintain thelarge quantities of dust required at these low temperatures in this starburst galaxy. Instead, weconclude that the dust properties need to be different from Galactic dust in order to fit thesubmillimeter "excess." We show that the dust spectral energy distribution can be fitted by anenhanced abundance of very small grains and discuss different alternatives.