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2014.2.24-3.2

2月24日(月)13:30~15:00  太陽系小天体セミナー  南棟2階会議室
Feb 24 Mon   Solar System Minor Body Seminar   Conference Room, South Bldg.2F

2月26日(水)10:30~12:00  総研大コロキウム   中央棟(北)1F講義室
Feb 26 Wed   SOKENDAI colloquium         Lecture Room

2月27日(木)15:30~16:30 VLBIコロキウム     中央棟(南)2F VLBIセミナー室
Feb 27 Thu   VLBI Colloquium      VLBI Seminar Room, Main Bldg. (South)

詳細は以下をご覧下さい。

2月24日(月)

キャンパス
三鷹
セミナー名
太陽系小天体セミナー
臨時・定例の別
定例
日時
2月24日(月曜日)13時30分~15時
場所
南棟2階会議室
講演者
渡部潤一
所属
国立天文台
連絡先
 名前:渡部潤一
備考
テレビ会議またはスカイプによる参加も可

2月26日(水)

Campus
Mitaka
Seminar Name
SOKENDAI colloquium
Regular/Irregular
Regular
Date
10:30-12:00, Feb 26, 2014
Place
Lecture Room
Speaker 1
Nobuyuki Sakai
Affiliation
D3, SOKENDAI, Mitaka(supervisor : Mareki Honma)
Title
The first astrometry result of the Perseus arm beyond a Galactic longitude l of ~ 190 deg with VERA
Abstract
Contexts. Currently, VERA and VLBA have been conducting kpc-scales astrometry to make a 3D map of the Milky Way Galaxy.
AIms. We aim to expand previous astrometry coverage of the Perseus arm from a Galactic longitude l of ~ 190 deg to that of ~ 240 deg.
This is crucial to accurately understand large scale structure of the Perseus arm.
Methods. We carried out nine-epochs VERA astrometry observations toward massive star-forming region IRAS 07427-2400 (l = 240.3 deg, b = 0.1 deg, Vlsr = 68.0 km/s) between January 20, 2012 and September 16, 2013.
Results. The measured parallactic distance is 5.18 +0.79/-0.59 kpc, which places the source in the 3rd Galactic quadrant of the Perseus arm.
Discussions. A combination of our astrometry result and previous ones reveal that the pitch angle of the Perseus arm is constant (i = 17.7 +/- 1.8 deg) in 94.60 deg < l < 240.32 deg, although the pitch angle is changed significantly (i = 11.5 +/- 1.3 deg) in 43.17 deg < l < 94.60 deg. The difference indicates that bifurcation or spur as seen in external disk galaxies may occur in 43.17 deg < l < 94.60 deg for the Perseus arm.
Speaker 2
Shino Nagisa
Affiliation
D2, SOKENDAI, Mitaka(supervisor : Mareki Honma)
Title
Methanol maser observation of massive star formation region IRAS 18089-1732
Abstract
The formation scenario of massive star is not yet fully understand.
Methanol maser is regarded as the signpost of the formation process of the massive star. Particular, the 44GHz methanol maser is associated with an outflow, and it is said that the 6.7GHz methanol maser is associated with an accretion disk.
If this is true, 44GHz methanol maser is expected to be distributed perpendicularly with respect to rotating disk. Detecting (or rejecting) this will play a major role in understanding the scenario of massive star formation.
In order to test this, we observed 6.7GHz methanol maser using JVN and obtained space distribution map. We also analyzed the VLA archive data of the 44GHz methanol maser.
We were able to get the space distribution map of the 44GHz methanol maser and the 6.7GHz methanol maser of IRAS18089-1732.
We argue about each emission position from the result.
Organizer
Name : Ayumu Matsuzawa
Comment
TV conference system is available connecting from Nobeyama, Hawaii,Mizusawa, and Okayama

2月27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
日時
2月27日(木曜日)15:30 ~ 16:30
場所
中央棟(南)2階VLBIセミナー室
講演者
千田 華
所属
東海大学
タイトル
A previous studies of gamma-ray bright radio galaxies
Abstract
The radio galaxy 3C 84 (z=0.0176;1mas=0.35 pc) is well-known for many traces of recurrent activities in its relativistic jet on various spatial ranging from sub-pc to kpc.
Recently,the sub-pc scale jet in 3C 84 has increased its activity again at radio band such as an ejection of a new jet component, related with an active phase in GeV regime after the launch of Fermi space telescope.
Thus, 3C 84 is the best laboratory to study the radio properties of subparsec jet in connection with the gamma-ray activity.
In this talk, I will review previous studies about 3C 84, especially relate on gamma-ray emission.
Finally, I will report the results of 3C 84 observations performed in the GENJI program from 2011 to 2013.
As a result, jet component flux is increasing and the component is moving to the south with sub-relativistic velocity during three years.
Therefore our results suggest that jet component is a hot spot and it is still growing.
世話人の連絡先
名前:MIN CHEULHONG
備考
テレビ参加可

以上

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