2011.11.7-11.13

11月7日（月）10:00～16:00 総研大博士論文予備審査・発表会　　　三鷹大会議室
Nov 7 Mon Sokendai Doctor Thesis Presentation Large Conference Room

11月7日（月）10:30～11:30 国立天文台談話会（臨時） コスモス会館会議室
Nov 7 Mon NAOJ Seminar Cosmos Lodge

11月7日（月）13:30～15:00 太陽系小天体セミナー 南棟2階会議室
Nov 7 Mon Solar System Minor Body Seminar 2F Conference Room, South Bldg.

11月7日（月）16:00～17:00 国立天文台談話会（臨時） コスモス会館会議室
Nov 7 Mon NAOJ Seminar Cosmos Lodge

11月7日（月）16:00～17:00 Galaxy Workshop Subaru すばる棟 1F 院生セミナー室
Nov 7 Mon Galaxy Workshop Subaru Student Seminar Room, Subaru Bldg. 1F

11月9日（水）14:00～ 　　　理論コロキウム 　　　　　 　コスモス会館会議室
Nov 9 Wed Colloquium of Theoretical Astronomy Division Cosmos Lodge

11月10日（木）16:00～17:00 Galaxy Workshop Subaru 中央棟 1F 第一会議室
Nov 10 Thu Galaxy Workshop Subaru 1st Conference Room, Main Bldg (prefab)

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

詳細は以下をご覧ください。

11月7日(月)

キャンパス
三鷹
セミナー名
総研大博士学位論文予備審査発表会
臨時・定例の別
臨時
日時
11月7日（月）10:00～16:00
場所
中央棟大会議室
所属
総合研究大学院大学天文科学専攻
発表者
内海　洋輔　(10:10-10:50）
題目
Testing Cosmological Paradigm with Wide Field Observation
発表者
大井　渚　(11:10-11:50）
題目
NIR J, H, K Imaging Study of Host Galaxies of ULIRGs and LIRGs – Implication for SMBH Growth –
発表者
秦　和弘　(13:00-13:40）
題目
Toward the Origin of AGN Jet: VLBI Study of Messier 87
発表者
富田　賢吾　(14:00-14:40）
題目
Radiation Magnetohydrodynamic Simulations of Star Formation Processes
発表者
貴島　政親　(15:10-15:50）
題目
The Application of VLBI Data to Obtain Long-Term Light Curves for AGN Science
連絡先
名前：総務課研究支援係
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
臨時
日時
11月07日(月) 10:30-11:30
場所
コスモス会館会議室
講演者
Steven Majewski
所属
University of Virginia
タイトル
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) and Its Southern Hemisphere Extension (APOGEE-South)
Abstract
The Apache Point Observatory Galactic Evolution Experiment (APOGEE) in SDSS-III is a large-scale, near-infrared, high-resolution (R >~ 22,500) spectroscopic survey of the Milky Way (MW) using a newly-constructed, 300-fiber, cryogenic spectrograph operating over 1.51-1.68 microns (i.e., most of the H-band).
Because of the lower H band dust extinction compared to optical wavelengths (A_H/A_V = 0.16), APOGEE will effectively pierce through dust obscuration to provide a vast, uniform database of chemical abundances and radial velocities for stars across all Galactic populations (bulge, thin and thick disks, halo).
APOGEE started observations in May 2011 and will use the remaining ~3 years of SDSS-III bright time to observe ~100,000 giant star candidates selected from the Two Micron All-Sky Survey (2MASS) down to H=11-13.5 across hundreds of sightlines.
With its high resolution and S/N (>100 per pixel), APOGEE will determine precision radial velocities (presently 200 m/s accuracy) and accurate abundances for numerous chemical species, including C, N, O and Fe, as well as other alpha, odd-Z, and iron-peak elements.
Among the main APOGEE scientific objectives are to: (1) measure in an unbiased, uniform manner the spatial variations of metallicity distributions and abundance patterns with statistically large samples of MW stars,
(2) study the processes of star formation, feedback, mixing and chemical evolution in the MW with sensitivity to numerous nucleosynthetic pathways,
(3) survey Galactic dynamics, particularly in the bulge and disk, where constraints on the nature and influence of the Galactic bar and spiral arms will be defined,
(4) look for chemodynamical evidence of Galactic substructure from accretion events, postulated by hierarchical formation models to be responsible ultimately for the formation of all MW stellar populations, and
(5) use these extensive chemodynamical data, particularly in the inner Galaxy, to unravel the overall formation and evolution of the MW.
The first APOGEE results are in hand and will be discussed.
To extend APOGEE’s coverage of the Galactic bulge, inner Galaxy and third and fourth Galactic quadrants, as well as the Magellanic Clouds, omega Centauri, the Sagittarius dwarf spheroidal and other interesting, Southern Hemisphere targets, a duplicate APOGEE instrument is being proposed for the Du Pont 2.5-m as part of the “After Sloan-III” collaboration.
Collaborators are being sought for this new, southern component of the APOGEE survey, expected to begin in 2014.
連絡先
名前：廣田朋也
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7日（月）13:30～15:00
場所
南棟2階会議室
講演者
渡部潤一
所属
国立天文台天文情報センター
内容
CMOSセンサーによる流星観測＠木曽
連絡先
名前：渡部潤一
備考
テレビ参加可
Campus
Mitaka
Seminar
Solar System Minor Body Seminar
Regular/Irregular
Regular
Date
November 7th 13:30～15:00
Place
the Conference Room of South Building (2F), NAOJ
Speaker
Jun-ichi Watanabe
Affiliation
Public Relations Center, NAOJ
Contents
meteor observations using CMOS sensor at Kiso
Facilitator
Name：Jun-ichi Watanabe
Comment
・welcome to participate via TV conference system
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
臨時
日時
11月07日(月) 16:00-17:00
場所
コスモス会館会議室
講演者
Sheperd Doeleman
所属
MIT Haystack Observatory
タイトル
The Event Horizon Telescope: Observing Black Holes with Schwarzschild Radius Resolution
Abstract
It is now almost certain that at the center of our Milky Way Galaxy lies a super massive black hole – 4 million times more massive than our Sun.
Because of its proximity to Earth, this object, known as Sagittarius A*, presents astronomers with the best opportunity in the Universe to spatially resolve and image a black hole Event Horizon.
To do this requires using Very Long Baseline Interferometry (VLBI), the technique whereby radio telescopes around the world are linked together in a Global phased array.
Very short wavelength VLBI observations have now confirmed structure on ~4 Schwarzschild radius scales within SgrA*, and have revealed time variability in this source on the same spatial scales.
For the much more massive (6 billion solar mass) black hole powering the relativistic jet in M87, similarly compact structures have been detected.
I will describe the instrumentation efforts that enable these observations, discuss what current and future VLBI observations can tell us about these super-massive black holes, and describe plans for assembling a submm-VLBI Event Horizon Telescope.
連絡先
名前：廣田朋也
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
11月7日（月）16時～17時
場所
すばる棟 1F 院生セミナー室
講演者
Alan McConnachie
所属
NRC Herzberg Institute of Astrophysics
タイトル
Near field cosmology with Local Group galaxies
Abstract
It is on galactic scales that our understanding of the cosmological evolution of matter is most incomplete.
Many of the predicted features of galaxies, such as faint satellites and diffuse stellar haloes, are extremely low surface brightness, and so the Milky Way, M31 and M33 are some of the only large galaxies in the Universe and that can provide robust tests of many fundamental aspects of galaxy formation models.
The Pan-Andromeda Archaeological Survey (PAndAS) is a large, deep, photometric survey that has surveyed nearly 400 sq.degrees in the surroundings of the M31/M33 sub-group, and which is providing the deepest and most complete panorama of galaxy haloes available.
Here, I will review recent results from PAndAS, and discuss the future development of this field with an eye on the next generation of astronomical facilities.
連絡先
名前：須田拓馬
備考
テレビ参加不可

11月9日(水)

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9日（水曜日）14時～
場所
コスモス会館会議室
講演者
富田 賢吾 氏
所属
総研大/理論研究部
タイトル
原始星形成過程の輻射磁気流体シミュレーション
Abstract
我々は輻射磁気流体シミュレーションを用いて星形成過程を研究してきた。
これまでは主に星形成の初期に形成されるファーストコアに着目して研究を進めてきたが、最近化学反応の効果を取り入れた状態方程式を取り入れることで、星形成のより後期段階であるセカンドコラプスとそれに続く原始星コアの形成を直接輻射磁気流体シミュレーションすることに成功した。
回転・磁場のない場合には先行する精密な球対称輻射流体計算と整合的な結果を得ることができた。
磁場が強い場合には初期に回転があっても、磁場による効率的な角運動量輸送の結果形成される原始星コアはその形成直後はほぼ球対称的になることがわかった。
最近このような原始星コア形成まで分解する計算が行われ始めているが、磁場を含む計算は本研究が初めてであり、その進化は定性的に異なることを見出した。
現実的には星形成過程では理想MHD近似は成立しないと考えられているため、余裕があれば現在開発を進めている Super Time Stepping法による抵抗性MHD計算についても紹介したい。
連絡先
名前：山崎 大

11月10日(木)

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
11月10日（木）16時～17時
場所
中央棟 1F 第一会議室
講演者
小野寺彰人
所属
ETH Zurich
タイトル
“Near-infrared spectroscopy of passively evolving galaxies at z>1.4 with Subaru/MOIRCS”
Abstract
Typical spectroscopic surveys aiming at z>1.4 galaxies have been conducted with optical instruments and targetingstar-forming galaxies relatively blue in rest-frame UV.
Thus, high redshift passive galaxies are almost fully missed inthese surveys because they are very faint in the optical and usually there is no detectable emission line.
In thisrespect, near-IR spectroscopy offers a great advantage for passive galaxies at z>1.4 as strongest spectral features suchas 4000A break and Ca H+K absorption lines are redshifted into near-IR, and rest-frame optical continuum is muchbrighter than that in the rest-frame UV.
By taking advantages of such nature of passive galaxies and the capability ofmulti-object spectroscopy of MOIRCS on Subaru, we have carried out near-IR spectroscopic observations of passivelyevolving galaxies at z>1.4.
We have selected a sample of massive BzK-selected passively evolving galaxies (pBzKs) atz>1.4 from the COSMOS field and observed them with Subaru/MOIRCS.
With a exposure time ranging from 7.5 hours to 9.5hours per object, 18 pBzKs among 34 observed in 3 masks have been identified spectroscopically.
I will show the resultson their stellar populations based on broad-band SEDs and rest-frame optical spectral features, environments, andvelocity dispersion analysis for the brightest object.
I will also show average properties of z>1.4 passive galaxiesbased on a composite spectrum of identified pBzKs.
連絡先
名前：須田拓馬
備考
テレビ参加不可

11月11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11日(金) 16:00-17:00
場所
大セミナー室
講演者
住 貴宏
所属
大阪大学大学院理学研究科宇宙地球科学専攻
タイトル
Unbound or distant planetary mass population detected by gravitational microlensing – Free-floating planets may be common –
Abstract
We discover a population of unbound or distant Jupiter-mass objects, which are almost twice as common as main-sequence stars, based on two years of gravitational microlensing survey observations toward the Galactic Bulge.
These planetary-mass objects have no host stars that can be detected within about ten astronomical units by gravitational microlensing.
However a comparison with constraints from direct imaging suggests that most of these planetary-mass objects are not bound to any host star.
An abrupt change in the mass function at about a Jupiter mass favours the idea that their formation process is different from that of stars and brown dwarfs.
They may have formed in proto-planetary disks and subsequently scattered into unbound or very distant orbits.
We also review the recent results on bound planets by microlensing and prospects for the space-based observation by the NASA’s Wide-Field Infrared Survey Telescope (WFIRST).
連絡先
名前：廣田朋也

以上