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2019.7.15-7.21

7月16日(火)10:00~10:50   2019年度前期 研究中間レポート発表会 講義室
Jul 16 Tue     SOKENDAI Progress Report Defense in 1st semester, AY2019 Lecture Room

7月16日(火)13:30~15:00   太陽系小天体セミナー  南棟2階会議室  
Jul 16 Tue      Solar System Minor Body Seminar    Conference Room, South Bldg.2F 

7月17日(水)10:30~12:00   総研大コロキウム   講義室
Jul 17 Wed     SOKENDAI colloquium Lecture Room

7月17日(水)13:30~14:30  ATCセミナー すばる棟 大セミナー室
Jul 17 Wed         ATC Seminar  Large Seminar Room

7月17日(水)13:30~15:00  科学研究部コロキウム    開発棟3号館3階会議室
Jul 17 Wed  Colloquium of Division of Science  Conference room, Instrument Development Bldg. 3 3F 

詳細は以下をご覧下さい。

7月16日(火)

キャンパス
三鷹 
セミナー名
2019年度前期 研究中間レポート発表会
SOKENDAI Progress Report Defense in 1st semester, AY2019
定例・臨時の別
臨時
日時
 7月16日(火曜日) 10時~10時50分
場所
三鷹キャンパス 講義室 Lecture Room in Mitaka Campus
講演者
Liang, Yongming
所属
総研大 天文科学専攻
タイトル
Correlation between galaxy and IGM at z=2.2 mapped by Subaru/HSC
連絡先
-名前:井上 瑞穂

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7月16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
7月16日(火曜日)13時30分~15時
場所
南棟2階会議室
講演者
西田信幸

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

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7月17日(水)

Campus
Mitaka
Seminar
SOKENDAI colloquium
Regularly Scheduled/Sporadic
Regular
Date and time
July 17, 2019, 10:30 -12:00

Place
Lecture Room

Speaker
Takafumi Tsukui
Affiliation
SOKENDAI 3rd year (D1)(Supervisor: Satoru Iguchi, Hiroshi Nagai, Yuichi Matsuda)
Title
Galactic Dynamics and Dark Matter Profile of NGC1380 with ALMA and VLT/MUSE
Abstract
ALMA’s high resolution and high sensitivity images enable us to obtain kinematics of molecular gas in the center of early-type galaxies (~1kpc) complementarily to the stellar dynamics obtained with optical IFU instrument. The cold molecular gas dynamics is a powerful tracer of mass distribution of galaxies because the velocity dispersion is low(~10km/s) and the simple rotational model is applicable. To understand the interaction between dark matter and baryonic matter in the galaxy evolution history, it is fundamental to measure dark matter distribution in galaxies. However, it is difficult to derive the dark matter profile in the central region of early-type galaxies because of the lack of neutral hydrogen gas in early-type galaxies and the degeneracy between dynamical stellar M/L and dark matter distribution. To resolve this difficulty, we conducted a combined analysis of ALMA cold molecular gas kinematics data and MUSE stellar kinematics data of early-type fast rotator galaxy NGC1380. Our strategy is to measure BH mass and stellar mass well in the central region (~radius of 6”, 500pc) with the cold gas kinematics. Then we derive dark matter profile with the stellar kinematics which is available in a wide field of view(~radius of 120’’, 10kpc) with the help of information of the central cold gas modeling. Dynamical measurement of stellar M/L and BH mass is conducted with ALMA high angular resolution data (0.24”×0.18” ~ 21pc×16pc where BH sphere of influence of the resulted BH mass is 0.37”~ 33pc). Simple gas rotational disk model reproduce observed data cube well. The obtained BH mass of 3.38×10^8^{+0.30}_{-0.24} solar masses is close to the estimated value of 3.9×10^8 solar masses from the empirical M – sigma relation. With Jeans Anisotropic Models (JAM; Cappellari 2008) of stellar kinematics, we found that the substantial dark matter halo needs to exist to maintain flat velocity profile at large radius.
However, the mass model obtained with ALMA cold gas modeling cannot reproduce the central high-velocity dispersion peak in the stellar kinematics data (~10” 900pc ), which may indicate several possibilities including the steep M/L variation and hidden non-axisymmetric bar structure. We obtained dark matter profile by using information from the central gas rotational disk model as a prior knowledge with Bayesian inference. The obtained central slope of the dark matter was gamma=0.45^{+0.11}_{-0.10} which is lower than 1.0 NFW profile predict.
Speaker
Takaharu Sisido
Affiliation
SOKENDAI 3rd year (D1) (Supervisor: Takayuki Tomaru, Yoichi Aso, Ryutaro Takahashi)
Title
TBD
Facilitator
-Name:Kei Ito

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

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7月17日(水)

キャンパス
三鷹
セミナー名
ATCセミナー
定例・臨時の別
臨時
日時
7月17日(水曜日)13時30分~14時30分
場所
すばる棟 大セミナー室
講演者
田村 友範 氏
所属
国立天文台 ATC
タイトル
 PFS分光器室の流体解析シミュレーション
Abstract
ハワイ観測所では新しい観測装置PFS(Prime Focus Spectrograph)の
導入を予定している。観測所ではPFSの分光器4台を設置するための
断熱室を山頂施設に準備しており、また熱交換器を用いて分光器室の
温度を一定に制御するための温度制御システムの開発を行っている。
またPHOENICSという熱流体解析ソフトウエアを使用したシミュレーション
を実施して冷却システムが分光器の要求を満たすかどうか評価している。
シミュレーションの現状と分光器室の準備状況について報告する。

連絡先
-名前:永井 誠
備考
日本語での講演

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7月17日(水)

キャンパス
三鷹
セミナー名
科学研究部コロキウム
定例・臨時の別
定例
日時
 7月 17日(水曜日) 13時30分 ~ 15時
場所
開発棟3号館3F会議室
講演者
Yoko Oya
所属
Univ. of Tokyo
タイトル
低質量原始星天体の原始星円盤形成領域における物理的・化学的構造
Abstract
Disk-formation around protostars is of fundamental interest for both of astrophysics and astrochemistry, because protostellar/protoplanetary disks are the birthplaces of planets. With the advent of ALMA (Atacama Large Millimeter/submillimeter Array), infalling envelope and rotating disks are spatially resolved in radio observations. We have delineated physical and chemical structures around several young (Class 0/I) low-mass protostellar sources with ALMA. On a 100 au scale, chemical compositions of the gas have been found to drastically change from envelopes to disks. This chemical change helps us to disentangle the kinematic structures of the gas into the two fundamental components (an envelope and a disk), like `molecular markers’. More interestingly, the chemical characteristics on a disk scale are different among sources, as previoiusly reported for the cloud core scale (~1000 au). On a 10 au scale, finer structures in disks are being delineated; in IRAS 16293-2422 Source A, the kinetic temperature of H2CS increases locally at the boundary between the envelope and the disk. This feature indicates a weak accretion shock and/or thermal heating in the transition zone, and moreover, it would be responsible to the drastic chemical change. The 1.2 mm continuum emission from this source also shows sub-structures in the disk. The connection from envelopes into disks is thus the current target for observational studies from both the physical and chemical aspects. The physical/chemical changes and the chemical diversity of young low-mass sources will have a substantial impact on understanding the initial condition of disk/planetary formation.

連絡先
-名前:Akimasa Kataoka

備考
使用する言語は英語

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