1月27日（月）13：30～15：00 太陽系小天体セミナー 南棟2階会議室
Jan 27 Mon Solar System Minor Body Seminar Conference Room, South Bldg. 2F
1月29日（水）10：30～12：00 総研大コロキウム 中央棟（北）1F講義室
Jan 29 Wed SOKENDAI colloquium Lecture Room
1月29日（水）14：00～15：00 ALMAJセミナー ALMA棟 1F 会議室
Jan 29 Wed ALMAJ Seminar Room 109 1F of ALMA Bldg.
1月30日（木）16：00～17：00 国立天文台野辺山談話会 野辺山観測所本館 講義室2
Jan 30 Thu Nobeyama NAOJ Seminar Lecture Room2,Main Bldg., Nobeyama
1月31日（金）16：00～17：00 国立天文台談話会 大セミナー室
Jan 31 Fri NAOJ Seminar Large Seminar Room
詳細は以下をご覧下さい。
1月27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
- 1月27日（月曜日）13時30分～15時
- 場所
- 南棟２階会議室
- 講演者
- 古荘玲子
- 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
1月29日(水)
- Campus
- Mitaka
- Seminar Name
- SOKENDAI colloquium
- Regular/Irregular
- Regular
- Date
- 10:30-12:00, Jan 29, 2014
- Place
- Lecture Room
- Speaker 1
- Giono Gabriel
- Affiliation
- D1, SOKENDAI, Mitaka（supervisor : Yoshinori Suematsu）
- Title
- TBA
- Abstract
- TBA
- Speaker 2
- Onoue Masfusa
- Affiliation
- M1, SOKENDAI, Mitaka（supervisor : Nobunari Kashikawa）
- Title
- High-z Quasar Selection with Hyper Suprime-Cam
- Abstract
- Quasars at high (>6) redshift are one of the best tracers of early Universe,
thanks to its high luminosity and characteristic spectrum.
However, quasars are very rare objects and it is important to establish a method to
select quasars effectively.
Based on the above, I will present the strategy for identifying high-z quasars by using SED fitting (#HSC project 47).
The goal of this study is to effectively isolate high-z quasars from contaminating sources such as brown dwarfs.
We are going to apply SED fitting method for quasar selection along with conservative two-color selection.
I will report the current status of SED fitting code development, and preliminary results of its application.
In addition, I would like to introduce the recently found three z~7 quasars (Venemans+13). - Organizer
- Name : Ayumu Matsuzawa
- Comment
- TV conference system is available connecting from Nobeyama, Hawaii,Mizusawa, and Okayama
1月29日(水)
- キャンパス
- 三鷹
- セミナー名
- ALMAJ セミナー
- 臨時・定例の別
- 定例
- 日時
- １月２９日（水曜日） １４時～１５時
- 場所
- 国立天文台 ALMA棟 1F 会議室
- 講演者
- 廣田 朋也
- 所属
- 水沢VLBI観測所
- タイトル
- LMA Cycle 0 Observation of Orion Radio Source I
- Abstract
-
I will report our recent results of new Atacama Large Millimeter/Submillimeter Array (ALMA) observations of a circumstellar disk around Source I in Orion KL. We detected two ortho-H2O lines at 321 GHz (10,2,9-9,3,6) and 336 GHz (v=1,5,2,3-6,1,6) for the first time in Source I. The latter one is in vibrationally excited state at the lower state energy of 2939 K, suggesting an evidence of hot molecular gas close to Source I. The integrated intensity map of the 321 GHz line is elongated along the bipolar outflow while the 336 GHz line map is unresolved with a beam size of 0.4″. Both of these maps show velocity gradient perpendicular to the bipolar outflow. The velocity centroid map of the 321 GHz line implies spatial and velocity structure similar to that of SiO masers tracing the root of the outflow emanating from the disk surface. In contrast, the 336 GHz line are emitted from the disk midplane with a diameter of 0.2″ (84 AU) as traced by a radio continuum emission and a dark lane of
the SiO maser distribution. The observed velocity gradient and the spectral profile of the 336 GHz H2O line can be reconciled with a model of an edge-on ring-like structure with an enclosed mass of 7 Solar masses and an excitation temperature of >3000 K. The present results provide a new evidence of hot and neutral circumstellar disk rotating around Source~I with a diameter of 100 AU scale. - 連絡先
- 名前：西合一矢, ジェームス
- 備考
- テレビ参加の可(前日までに要連絡）
1月30日(木)
- Campus
- Nobeyama
- Seminar
- NRO seminar
- Regular/Irregular
- Irregular
- Date
- 16:00~17:00, Jan. 30
- Place
- Lecture room #2, Main building, NRO
- Speaker
- Hsi-An Pan
- Affiliation
- SOKENDAI
- Title
- Environmental Dependence of Star Formation in Nearby Barred Spiral Galaxies
- Abstract
-
We study environmental dependence of the physical properties of GMCs and their ability of star formation in nearby galaxies. In the first place, the relation of molecular gas and stars are studied in large scale (few hundred pc) in terms of the Kennicutt-Schmidt (K-S) law in IC 342. We found that there is no universal K-S law in this galaxy.
The results of K-S law can be explained by the different star formation mechanisms in different regions of a galaxy. The results of IC 342 is reproduced by the similar analysis in other fifteen galaxies, suggesting that the non-universal star formation law is common in nearby galaxies. The non-universal K-S law can be explained with the variation of dense gas fraction as well. We further study this topic in the bar region of galaxy NGC 6946 by the observations with a fine resolution (100 pc). Star formation efficiency is enhanced in the northern bar of this galaxy in terms of its azimuthal K-S law.
Indeed, the resolved GMC properties suggest that the GMCs in the northern bar is denser than that in the southern bar and other area.
The denser GMCs may be a result of higher pressure of ambient ISM exerted on the GMCs. To confirm the result of NGC 6946, we enlarge the galactic environment by comparing the GMCs in NGC 6946 and those in starburst, normal disk, and dwarf galaxies. The results suggest again that galactic environments are regulating GMCs properties and their star forming activity. - Facilitator
- Name：Kana Morokuma-Matsui
- Comment
- teleconference available
1月31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
- 1月31日(金) 16:00-17:00
- 場所
- 大セミナー室
- 講演者
- Mercedes Richards
- 所属
- Pennsylvania State University
- タイトル
- “3D Tomographic Image Reconstruction of Gas Flows in Interacting Binary Star Systems”
- Abstract
- Interacting binary star systems are in the process of mass transfer during which gas will flow along a path called the gas stream, from the more evolved mass-losing star to its companion. Images of these gas flows have not yet been realized with direct-imaging techniques because such details cannot be resolved even with the largest telescopes.
However, the image reconstruction technique of Doppler tomography has revealed 2D images of gas flowing along the predicted gravitational path between the stars, accretion disks or accretion annuli around the mass-gaining star, hot spots where the gas flow collides with the surface of the star, and evidence of magnetic flows connected with the cool magnetically-active mass-losing star. The extension to 3D tomography has unveiled views of extensive gas flows beyond the central plane of the binary system. These new 3D images show that the magnetic field of the mass losing star can influence the gas motions dramatically in some cases. Hence, tomography has revealed the active environments that exist in a range of objects from direct-impact binaries to cataclysmic variables and gamma ray binaries. - 連絡先
- 名前：田中雅臣
以上