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2014.11.10-11.16

11月10日(月)13:30~15:00  太陽系小天体セミナー   南棟2階会議室
Nov 10 Mon   Solar System Minor Body Seminar   Conference Room, South Bldg.2F

11月12日(水)10:00~11:00  総研大コロキウム   中央棟(北)1F講義室
Nov 12 Wed   SOKENDAI colloquium         Lecture Room

11月12日(水)14:00~15:00  ALMAJセミナー     ALMA棟 1F 会議室
Nov 12 Wed   ALMAJ Seminar              Room 109 1F of ALMA Bldg.

11月13日(木)15:00~16:00  理論コロキウム   中央棟(北)1F講義室
Nov 13 Thu   DTA Colloquium            Lecture Room

11月14日(金)16:00~17:00  国立天文台談話会   大セミナー室
Nov 14 Fri   NAOJ Seminar               Large Seminar Room

詳細は以下をご覧下さい。

11月10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
11月10日(月曜日)13時30分~15時
場所
南棟2階会議室
講演者
匠あさみ
講演者
松村行博
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

11月12日(水)

Campus
Mitaka
Seminar Name
SOKENDAI colloquium
Regular/Irregular
Regular
Date
10:00-11:00,11/12, 2014
Place
Lecture Room
Speaker
GIONO Gabriel
Affiliation
D2, SOKENDAI, Mitaka(supervisor: SUEMATSU Yoshinori)
Title
CLASP, from science requierement to instrumentation
Abstract
Comments from my previous talk suggested to focus more on the science related to CLASP instead of the detailed instrumentation. Hence, I decided to recap the science requirement of the instrument and explain from which scientific interests these requirement are derived. Then, I will show the result of several experiments performed to confirm the instrument requirements. Finally, I’ll conclude by summarizing the current status of CLASP instrument, and introduce the remaining experiments planned to prepare the instrument before its flight in August 2015.
Organizer
Name : Taiki Suzuki
Comment
TV conference system is available connecting from Nobeyama, Hawaii,Mizusawa, and Okayama.

11月12日(水)

Campus
Mitaka
Seminar
ALMAJ Seminar
Regular/Irregular
Regular
Date
2pm-3pm Novemer 12
Place
Room109 (1F) at ALMA Building
Speaker
Hiroko Shinnaga
Affiliation
NAOJ Chile Observatory
Title
Magnetic Field in The Isolated Massive Dense Clump IRAS
20126+4104 II. A Study Across A High Spatial Dynamic Range; From 1
Parsec Scale Down To 20 AU Scale
Abstract
We report on a study of the magnetic field structures of IRAS 20126+4104, a massive dense clump in which the rotation axis and the magnetic field axis are misaligned. In order to study the role of magnetic field in high mass star forming regions in detail, we investigate magnetic field of the object in a high spatial dynamic range. The data sets that we use include interferometric data taken with the Submillimeter Array (SMA) and single-dish data with 9 arcsec beam taken with the SHARP/CSO (Shinnaga et al. 2012) and with 15 arcsec beam taken with SCUPOL at the JCMT telescope (Matthews et al. 2009).
Comparing the above results with the VLBI spectropolarimetric observations by Surcis et al. 2014, these four independent data sets allow us to investigate the magnetic field structures across a very high spatial dynamic range (5 × 103), between 1 pc scale and down to 20 AU scale of the massive dense clump − massive (− 10Msun) (proto)star system. The magnetic field lines measured in these four different spacial scales turned out to be consistent with each other. We carried out detailed theoretical simulations for this object based on the study reported in Shinnaga et al. 2012 and Kataoka et al. 2012. By comparing the observational results with the theoretical simulations, we find that the mag- netic field plays a critical role during the course of the gravitational collapse of the massive dense clump.
Facilitator
-Name:Kazuya Saigo

11月13日(木)

キャンパス
三鷹
セミナー名
理論コロキウム
臨時・定例の別
 定例
日時
 11月13日(木曜日) 15時00分~16時00分
場所
 講義室
講演者
 Kenneth C. Wong
所属
ASIAA
タイトル
Strong Gravitational Lensing as a Probe of Galaxy Evolution and Cosmology
Abstract
Strong gravitational lens galaxies present a unique opportunity to study galaxy evolution and cosmology. By constructing a mass model of the lens galaxy that can reproduce the observed lensing configuration, it is possible to constrain the structural properties of the galaxy.
Furthermore, lensed quasars with a measured time delay can be used to constrain cosmological parameters, independent of other probes such as supernovae, CMB observations, and BAOs. Most of the lens galaxies discovered to date have been at relatively low redshift (z˜0.3) with very few discovered at z > 1. I present the discovery of a lens galaxy at z = 1.62, making it the most distant lens galaxy known. Analysis of this system shows that it is a compact early-type galaxy with an IMF more consistent with Chabrier than Salpeter, in contrast to results for similar galaxies at low redshift. I also present results from the H0LiCOW project, which aims to accurately model five time-delay lenses to get an accurate determination of the Hubble constant. In particular, correcting for biases introduced by line-of-sight structures projected near the lens galaxy is a key systematic that needs to be overcome. I present a new method for accurately and efficiently characterizing these effects, which accounts for the most significant perturbers explicitly while treating the majority of the perturbers with an approximation that greatly reduces the necessary computations.
連絡先
 名前: 長谷川 靖紘

11月14日(金)

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
11月14日(金) 16:00-17:00
場所
大セミナー室
講演者
柴田 大(Masaru Shibata)
所属
京都大学基礎物理学研究所(Kyoto University)
タイトル
「連星中性子星の合体:重力波と電磁波対応天体」
“Merger of binary neutron stars: Gravitational waves and electromagnetic counterparts”
Abstract
The merger of binary neutron stars is one of most promising sources of gravitational waves. It is also a promising candidate for the central engine of short-hard gamma-ray bursts and a source of the strong transient electromagnetic signal that could be the counterpart of gravitational-wave signals. Numerical relativity is probably the unique tool for theoretically exploring the merger process, and now, it is powerful enough to provide us a wide variety of aspects of the binary-neutron-star merger. In this talk, I will summarize our current understanding of the entire merger event that has been explored by numerical-relativity simulations. In particular, I focus on the relation between the neutron-star equation of state and gravitational waves emitted during the late inspiral and merger phase, and observable electromagnetic signal that is likely to be emitted by the dynamical ejecta.
連絡先
名前:鈴木 竜二

以上

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