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Probing the precise location of the radio core in the TeV blazar Mrk 501 with VERA at 43 GHz
Koyama, Shoko,Kino, Motoki,Doi, Akihiro,Niinuma, Kotaro,Hada, Kazuhiro,Nagai, Hiroshi,Honma, Mareki,Akiyama, Kazunori,Giroletti, Marcello,Giovannini, Gabriele,Orienti, Monica,Isobe, Naoki,Kataoka, Jun Astronomical Society of Japan 2015 Publications of the Astronomical Society of Japan Vol.67 No.4
Chemical variation in molecular cloud cores in the Orion A cloud. II.
Tatematsu, Ken'ichi,Ohashi, Satoshi,Umemoto, Tomofumi,Lee, Jeong-Eun,Hirota, Tomoya,Yamamoto, Satoshi,Choi, Minho,Kandori, Ryo,Mizuno, Norikazu Astronomical Society of Japan 2014 Publications of the Astronomical Society of Japan Vol.66 No.1
Lightcurve survey of V-type asteroids in the inner asteroid belt
Hasegawa, S.,Miyasaka, S.,Mito, H.,Sarugaku, Y.,Ozawa, T.,Kuroda, D.,Nishihara, S.,Harada, A.,Yoshida, M.,Yanagisawa, K.,Shimizu, Y.,Nagayama, S.,Toda, H.,Okita, K.,Kawai, N.,Mori, M.,Sekiguchi, T.,Is Astronomical Society of Japan 2014 Publications of the Astronomical Society of Japan Vol.66 No.3
[CI] 809 GHz Imaging of the NGC 6334 Complex
KIM, Sungeun,NARAYANAN, Desika Astronomical Society of Japan 2006 Publications of the Astronomical Society of Japan Vol.58 No.4
<P>We present Antarctic Submillimeter Telescope and Remote Observatory (AST/RO) observations of submillimeter emissions from the NGC 6334 complex for both the fine-structure line of atomic carbon and the rotational transition of CO. We detected strong emission from the entire star-forming NGC 6334 complex, and present maps of emission and emission. Comparing these maps with archival ASCA data, we show that, to the south of NGC 6334, the [CI] emissions are likely to be associated with strong X-ray emissions from the FIR sources. However, the calculation using the X-ray dissociation region model shows that the majority of the [CI] emission can not arise from X-ray dissociation of the cloud. Alternatively, far-ultraviolet radiation produced in the photodissociation regions is expected to contribute to dissociate the carbon monoxide in the NGC 6334 complex.</P>
Kambe, Eiji,Ando, Hiroyasu,Sato, Bun’ei,Izumiura, Hideyuki,Sekii, Takashi,Paulson, Diane B.,Yanagisawa, Kenshi,Masuda, Seiji,Shibahashi, Hiromoto,Hatzes, Artie P.,MARTI´C, Milena,LEBRUN, Jean-Claude,M Astronomical Society of Japan 2008 Publications of the Astronomical Society of Japan Vol.60 No.1
An improvement of the radial-velocity measurement accuracy is crucial for the detection of tiny stellar oscillationsand exoplanets. Through the analysis of week-long extensive observations of solar-type stars (Procyon in 2000, 2002, and 2006/2007 and τ Cet in 2002 and 2006/2007), we have carefully examined, revised, and finelytuned the widely used multiple Gaussian IP fitting method for the spectrograph, HIDES. By determining a necessaryand sufficient number of free parameters in the model as well as introducing an iterative process in the radial-velocityanalysis, we can reach a precision of below 3ms<SUP>-1</SUP>, which is much smaller than the precision of 6ms<SUP>-1</SUP> officially announced so far for HIDES. We also make our technique refined for the 2002 McDonald Procyon data. Even with our revised method, slow radial velocity variations with an amplitude of about 10ms<SUP>-1</SUP> are left in the Procyon data. We emphasize that it is neither due to particular observing instruments nor radial-velocity analysis, and thus could be due to stellar origin. The analysis presented here makes the foundations of our next scientific analysis of the radial-velocity variations of Procyon, which will be presented in our forthcoming papers.
Visible-wavelength spectroscopy of subkilometer-sized near-Earth asteroids with a low delta-v
Kuroda, D.,Ishiguro, M.,Takato, N.,Hasegawa, S.,Abe, M.,Tsuda, Y.,Sugita, S.,Usui, F.,Hattori, T.,Iwata, I.,Imanishi, M.,Terada, H.,Choi, Y.-J.,Watanabe, S.-i.,Yoshikawa, M. Astronomical Society of Japan 2014 Publications of the Astronomical Society of Japan Vol.66 No.3