2013.4.29-5.5

5月 2日(木)15:30~16:30  VLBIコロキウム  中央棟(南)2F VLBIセミナー室
May 2 Thu  VLBI Colloquium   VLBI Seminar Room, Main Bldg. (South) 2F

5月 2日(木)16:00~17:00  野辺山談話会   野辺山観測所 本館 輪講室
May 2 Thu  Nobeyama NAOJ Seminar  Seminar Room, Nobeyama

詳細は以下をご覧下さい。

5月2日(木)

キャンパス
三鷹
セミナー名
VLBIコロキウム
臨時・定例の別
定例 (毎週木曜日の下記の時間)
日時
5月 2日(木曜日)15時30分 ~ 16時30分
場所
中央棟(南) 2階VLBIセミナー室
講演者
千田 華
所属
東海大M1
タイトル
The optical observation and multiwavelength variations of an Active Galactic Nucleus
Abstract
I have measured multi-band optical flux variation for a sample of 5 blazars on short, day-tomonth, timescales. My sample contains five BL Lacertae object. These photometric observations, made during September 2012 to December 2012, used Schmidt-Cassegrain telescope. My data indicate that two (Mrk421, PG1553+113) were no variations while three blazars (1ES1959+650,S50716+714 and BL Lac) were variations. Since correlation with visible light and X-rays is not seen with almost all the observed objects, argues about each radiation origin. And I want discusses the radiation mechanism from a blazar.
連絡先
名前:鈴木大輝
備考
テレビ参加:可能
キャンパス
野辺山
セミナー名
国立天文台野辺山 談話会
臨時・定例の別
定例
日時
5月 2日(木曜日)16時00分~17時00分
場所
野辺山観測所 本館 輪講室
講演者
西谷 洋之
所属
野辺山宇宙電波観測所
タイトル: NH3 Survey of Massive Star-Forming Region W43
Abstract
We performed a NH3 (1, 1), (2, 2), and (3, 3) inversion lines survey of W43 region with Hokkaido University 11-m telescope. The survey covers the giant molecular cloud complexes with the massive star-forming region W43 (G30.8) and W43 S (G29.9) with several pc scale resolution. We detected these three line emissions from ~41%, ~ 16%, and ~10%, respectively, of 51 positions, which are selected based on the integrated intensity maps of 13CO (J=1-0) line of GRS (Jackson et al. 2006). We divided the observed area into sub-regions and estimated the difference of their evolutionary stages of star formation from the rotation temperature, NH3/13CO, FIR luminosity from IRAS data, and the associations with IRDCs and HII regions. Rotation temperatures are deduced to be ~15–20 K. We also derived the temperatures of ~6 -12 K, which may be interpreted as the temperatures when NH3 molecules were formed, from the population distribution between ortho- and para-levels of NH3. The rotation temperature > the formation temperature suggests that the elapsed time from formation of the NH3 molecules is shorter than the relaxation time between the ortho- and para-levels, ~10^6 years. It is consistent with that we found only one SNR, if at all, within the observed area in our literature research. They suggest that the complexes contain the sub-regions in the different evolutionary stages of star formation within a timescales shorter than the lifetime of massive stars.
連絡先
名前:柴崎清登、廣田晶彦
備考
テレビ参加可

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