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2012.1.30-2.5

1月30日(月)16:00~17:00 Galaxy Workshop Subaru すばる棟 1F 院生セミナー室
Jan 30 Mon  Student Seminar Room, Subaru Bldg

1月31日(火)10:00~10:40 総研大研究中間レポート発表会      講義室
Jan 31 Tue  SOKENDAI Progress Report (Master Thesis) Presentation Lecture Room

1月31日(火)14:00~15:00 総研大博士論文本審査・発表会      講義室
Jan 31 Tue  SOKENDAI Doctor Thesis Presentation        Lecture Room

2月1日(水)10:30~12:00 総研大コロキウム           講義室
Feb 1 Wed  Sokendai Colloquium     Lecture Room

2月1日(水)16:00~17:00 Galaxy Workshop Subaru すばる棟 1F 院生セミナー室
Feb 1 Wed  Student Seminar Room, Subaru Bldg

2月3日(金)13:00~14:00 総研大博士論文本審査・発表会      講義室
Feb 3 Fri  SOKENDAI Doctor Thesis Presentation        Lecture Room

2月3日(金)16:00~17:00 天文台談話会    すばる棟 1F 大セミナー室
Feb 3 Fri        NAOJ Seminar Large Seminar Room, Subaru Bldg

詳細は以下をご覧ください。

1月30日(月)

キャンパス
三鷹
セミナー名
Galaxy Workshop Subaru
臨時・定例の別
臨時
日時
1月30日(月)16時~17時
場所
すばる棟 1F 院生セミナー室
講演者
Myung Gyoon Lee
所属
Seoul National Univ.
タイトル
“Wandering Star Clusters in the Universe”
Abstract
Star clusters are often found in galaxies. However, some star clusters in the universe may want to be free, as we sometimes do. Recently we are witnessing the existence of some star clusters wandering in nearby galaxy groups to galaxy clusters. The nature and origin of these wandering star clusters are not yet known, but they may be related with the first objects in the universe. Current understanding of these objects will be discussed in relation with galaxy evolution.
(Refs)
1) Lee, M.G., Park, and Hwang 2010, Science, 328, 334, ‘Detection of a Large-Scale Structure of Intracluster Globular Clusters in the Virgo Cluster’
2) Lee, M.G. et al. 2010, ApJ, 709, 1083,’ The Globular Cluster System of the Virgo Giant Elliptical Galaxy NGC 4636. II. Kinematics of the Globular Cluster System’
3) Lee, M.G. et al. 2008, ApJ, 674, 886 ‘ Wide-Field Survey of Globular Clusters in M31. II. Kinematics of the Globular Cluster System’
連絡先
名前:小林正和
備考
テレビ参加不可

1月31日(火)

キャンパス
三鷹
セミナー名
総研大研究中間レポート発表会
臨時・定例の別
臨時
日時
1月31日(火)10:00~10:40
場所
中央棟北1F講義室
発表者
利川 潤
所属
総合研究大学院大学 天文科学専攻
タイトル
A Primitive Clustering Structure Proved by Wide-field Imaging
連絡先
名前:総務課研究支援係(大学院担当)
Campus
Mitaka
Seminar
SOKENDAI Progress Report (Master Thesis) Presentation
Regular/Irregular
Irregular
Date
January 31, 10:00~10:40
Place
Lecture Room
Speaker
Jun Toshikawa
Affiliation
SOKENDAI (The Graduate University for Advanced Studies)
Title
A Primitive Clustering Structure Proved by Wide-field Imaging
Contact
Research Support Section
キャンパス
三鷹
セミナー名
総研大博士論文本審査・発表会
臨時・定例の別
臨時
日時
1月31日(火)14:00~15:00
場所
中央棟北1F講義室
発表者
金子 紘之
所属
総合研究大学院大学 天文科学専攻
タイトル
Molecular Gas Properties and Star Formation in Interacting Galaxies
連絡先
名前:総務課研究支援係(大学院担当)
Campus
Mitaka
Seminar
SOKENDAI Doctor Thesis Presentation
Regular/Irregular
Irregular
Date
January 31, 14:00~15:00
Place
Lecture Room
Speaker
Hiroyuki Kaneko
Affiliation
SOKENDAI (The Graduate University for Advanced Studies)
Title
Molecular Gas Properties and Star Formation in Interacting Galaxies
Contact
Research Support Section

2月1日(水)

キャンパス
三鷹
セミナー名
総研大コロキウム
臨時・定例の別
定例
日時
2月1日(水曜日)10:30~12:00
場所
中央棟(北)1階 講義室
発表者
舘洞 すみれ
所属
総研大 M1・三鷹(指導教員 : 有本 信雄)
タイトル
Morphological Evolution of Passively Evolving Galaxies at 1.4<z<2.5
連絡先
名前:坂井伸行
備考
野辺山、ハワイ、水沢、岡山からTV会議で参加可能。
キャンパス
三鷹
セミナー名
Galaxy Workshop Subaru
臨時・定例の別
定例
日時
2月1日(水)16時~17時
場所
すばる棟 1F 院生セミナー室
講演者
岡本 桜子
所属
Peking Univ., the Kavli Institute for Astronomy and Astrophysics
タイトル
“Dwarf Galaxies around the Milky Way”
Abstract
Dwarf galaxies around the Milky Way provide us a unique opportunity to investigate galaxy formation and evolution through their re-solved stars.
Most of them are con-sidered to be both dynamically and chemically simple, with the high M/L ratio, and their number is doubled in recent years thanks to systematic surveys in the SDSS data archive (e.g. Willman et al.
2005; Belokurov et al. 2007). These newly discovered ultra faint dwarf (UFD) galaxies are roughly 10 to 100 times fainter than the well-known “classical” dSphs, having amorphous morphology and too low surface brightness to be found by the photographic plate. Because of their faint luminosities and apparently large sizes in the sky, the general natures of UFDs, such as star formation history (SFH) and detailed structural properties are still unclear. Here, I will present the recent results of our deep and wide photometric studies of 6 UFD galaxies and 3 classical dSphs, and then discuss the future projects related with these dwarf satellites.
連絡先
名前:小林正和
備考
テレビ参加不可

2月3日(金)

キャンパス
三鷹
セミナー名
総研大博士論文本審査・発表会
臨時・定例の別
臨時
日時
2月3日(金)13:00~14:00
場所
中央棟北1F講義室
講演者
大井 渚
所属
総合研究大学院大学 天文科学専攻
タイトル
Growth of Super Massive Black Holes Revealed from Near-Infrared Imaging of Host Galaxies
連絡先
名前:総務課研究支援係(大学院担当)
Campus
Mitaka
Seminar
SOKENDAI Doctor Thesis Presentation
Regular/Irregular
Irregular
Date
February 3, 13:00~14:00
Place
Lecture Room
Speaker
Nagisa Oi
Affiliation
SOKENDAI (The Graduate University for Advanced Studies)
Title
Growth of Super Massive Black Holes Revealed from Near-Infrared Imaging of Host Galaxies
Contact
Research Support Section
キャンパス
三鷹
セミナー名
国立天文台談話会
臨時・定例の別
定例
日時
2月 3日(金) 16:00-17:00
場所
大セミナー室
講演者
Gu Liyi
所属
東京大学大学院理学系研究科
タイトル
Interactions Between the Hot Plasmas and Galaxies in Clusters
Abstract
Compared to spatial distribution of dark matter in galaxy clusters, the optical-emitting galaxies appear to be more centrally-concentrated, while the X-ray-emitting intracluster medium (ICM) shows a flatter profile. Inabout half of nearby clusters, a giant cD galaxy is found at the center, where the ICM shows a two-phased nature: a cool phase, high metal abundance ICM coexists with a hot phase, low abundance ICM.
This nature is explained by a corona-like magnetic loop structure anchored on the cD galaxy, which confines the cool phase within loops.
The moving member galaxies interact with the magnetized ICM, exerting heats via magnetohydrodynamic turbulence that prevents the cool phase ICM from being radiatively cooled out.

By such galaxy-ICM interaction, the member galaxies gradually lose kinetic energy to the ICM and infall to the center. By examining the “optical-light vs. ICM-mass ratio” profiles for 34 relaxed clusters from z=0.9 to z=0.1, we detect a significant evolution that the galaxy light is more concentrated in nearby clusters. Various systematic errors, e.g., background uncertainties due to cosmic variance, and biases, e.g., different rest-frame bands, cosmic cluster growth, etc, have been taken into account. This result provides important support for our galaxy-ICM interaction view.
連絡先
名前:勝川行雄

以上

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