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2017.12.11-12.17

12月12日(火)13:30~15:00 太陽系小天体セミナー       南棟2階会議室
Dec 12 Tue         Solar System Minor Body Seminar Conference Room, South Bldg.2F

12月13日(水)10:00~12:00 総研大コロキウム          講義室
Dec 13 Wed         SOKENDAI colloquium      Lecture Room

12月15日(金)16:00~17:00 国立天文台談話会         コスモス会館会議室  
Dec 15 Fri          NAOJ Seminar          Conference Room, Cosmos Lodge 

詳細は以下をご覧下さい。

12月12日(火)

キャンパス
三鷹
セミナー名
太陽系小天体セミナー
定例・臨時の別
定例
日時
12月12日(火曜日)13時30分~15時
場所
南棟2階会議室
講演者
Jakub Vaverka
タイトル
Cosmic dust detection by Earth-orbiting spacecraft
Abstract
The cosmic dust particles are part of the solar system and can feasibly be observed in the near-Earth space or when they enter the Earth’s atmosphere. There are several different techniques that are used to measure cosmic dust entering the Earth’s atmosphere such as space-born dust detectors, meteor and HPLA radars, and optical methods.
One complementary method could be to use electric field instruments initially designed to measure the electric field and waves. A plasma cloud generated by a hypervelocity dust impact on a spacecraft body can be detected by the electric field instruments commonly operated on spacecraft. Since Earth-orbiting missions are generally not equipped with conventional dust detectors, the electric field instruments offer an alternative method to measure the Earth’s dust environment. On the other hand, this way of dust impact detection is a relatively new.
Signatures of dust impacts in the measured electric field are not still completely understood and explained. A frequently neglected problem is the identification of dust impacts in obtained waveforms. The recent understanding and description of the dust detection by the electric field instruments will be presented and signal interpretation will be discussed.

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

12月13日(水)

Campus
Mitaka
Seminar
SOKENDAI colloquium
Regularly Scheduled/Sporadic
Irregular
Date and time
December 13, 2017, 10:00 -12:00

Place
Lecture Room

Speaker
Shuichiro Tsuda
Affiliation
SOKENDAI 1st year (M1)(Supervisor: 本間希樹,秦和弘,柴田克典)
Title
Resolved magnetic-field structure and variability near the event horizon of Sgr A* Abstract (if you like):

Speaker
Jungha Kim
Affiliation
SOKENDAI 4th year (D2)(Supervisor: 本間希樹,廣田智也,柴田克典)
Title
Dynamics of jets/outflows from high-mass young stellar objects revealed by KaVA and ALMA observations Abstract (if you like):

Speaker
Satoshi Kikuta
Affiliation
SOKENDAI 3rd year (D1)(Supervisor: Masatoshi Imanishi,Yuichi Matsuda,Yutaka Komiyama)
Title
Lyman Alpha Imaging around a Hyperluminous QSO at z=2.84 Abstract (if you like):Ly-alpha imaging is a powerful technique to study galaxy formation at high-redshift by detecting redshifted Ly-alpha emission line with narrowband filters. I present the latest results of our Ly-alpha imaging around a hyperluminous QSO at z=2.84, namely HS1549+1919, with HSC/Subaru. We have detected >3400 LAEs within 36 arcmin from the QSO (i.e., ~1.1 deg^2 FoV). The QSO is found to reside in the center of massive overdensity of LAEs which is embedded within a large scale (~100 cMpc) structure of LAEs. We have also detected a gigantic Ly-alpha nebula around the QSO as well as many Ly-alpha blobs. The nebula is the largest and the most luminous to date and has a peculiar morphology: bubble-like structure extending several hundred kpc. After sharing the current status I present our future plans to further reveal galaxy formation in this rich environment. Your comments and suggestions are very welcome.

Please note that the presenter information posted here is not necessarily listed in order of presentation.

Facilitator
-Name:Nagaaki Kambara

Comment
TV conference system is available connecting from Nobeyama, Hawaii, Mizusawa, and Okayama.

12月15日(金)

キャンパス
三鷹
セミナー名
国立天文台談話会
定例・臨時の別
定例
日時
 12月15日(金曜日) 16時 ~ 17時
場所
コスモス会館会議室
講演者
Yi-kuan Chiang
所属
Johns Hopkins University
タイトル
Which Galactic dust map should I use? Insights from extragalactic tomography
Abstract
(optional)
Over the past few years, clustering-based redshift estimation has emerged as a new way to estimate redshifts and perform extragalactic tomography of arbitrary datasets. On a similar timescale, observations by Planck, WISE, Pan-STARRS and 21cm radio surveys have been used to create a multitude of SFD-type Galactic dust maps. I will explain how clustering-based redshift estimation can be used to test the quality of the seven different dust maps currently available and I will show that extragalactic signatures can be revealed in many of them. When such maps are used for correcting optical magnitudes, we therefore expect biases which are likely to affect galaxy evolution studies and the precision of cosmological experiments using supernovae, BAOs, or the growth of structures. I will present possible solutions to alleviate this issue and discuss which map should be used depending on which measurement one wishes to make.

連絡先
-名前:阿久津 智忠

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