Colloquium 2010.4-2011.3, Dept Astronomy, Kyoto Univ

題目Title:Super-massive Black Holes Across 
         the Cosmic History
講師Speaker:Ezequiel Treister 氏 (ハワイ大学) 
日時:3月9日(水) 午後4時 〜 
Date:  Wednesday, March 9th, 2011 starting at 4 p.m.
 It is now clear that the formation of the super-massive black hole (mass greater than a million solar masses) that can be now found in the center of most 
massive galaxies is directly connected to the evolution of the host galaxy. However, the details of this connection are still not well understood, in spite 
of significant progress in the last years. In order to fully understand galaxy formation we need to know when in the cosmic history are black holes growing 
more intensively, in what type of galaxies this growth is happening and what fraction of these sources are invisible at most wavelengths due to obscuration 
by the surrounding dusty medium.
Super-massive black holes grow by accreting surrounding matter and by mergers. In this talk, I will review observations of the density of black hole 
accretion from the nearby Universe at z~0 to early growth episodes at z~6, when the Universe was less than a billion years old. This is done by combining 
multiwavelength data ranging from infrared to soft gamma rays in both wide/shallow and narrow/deep surveys. We find that a large fraction of the black hole 
growth, ~75%, is obscured, and report evidence for a strong connection between significant black hole growth episodes and major galaxy mergers from z~0 to 
z~3. We then measure from deep optimally-stacked X-ray observations the amount of black hole growth in z=6-8 galaxies (0.7-1 billion years after the Big 
Bang). Finally, I will describe the impact of future deep observations at hard X-ray energies with upcoming missions like NuSTAR and Astro-H.

            Galaxy Formation in High Redshift Proto-Cluster Regions
講師Speaker:山田 亨 氏 (東北大学 大学院理学研究科) 
        Mr. Toru Yamada
日時:1月27日(木) 午後4時 〜 
Date:  Friday, January 27th, 2011 starting at 4 p.m.
 我々は、数年来 SSA22 z=3.1 銀河高密度領域における多波長広視野観測を行い、「原始銀河団」領域をより明確に検出して密度超過を定量化し、また、同領域における若
今回のコロキウムでは、最近完了した合計約2.5平方度におよぶすばる望遠鏡 Suprime Cam による輝線銀河分布の解析から、
(1) 3-30 Mpc スケールでの非常に大きな密度超過と
(2)  広がった輝線天体 Lyα Blobs の分布とその性質
(3) Lyα輝線銀河の輝線等価巾分布と非常に大きな輝線等価巾を持つ輝線銀河
(4)  約半数の輝線銀河が、特徴的なダブルピークを持つ
なお、最後の10分間程度は、このような広視野深宇宙探査を赤方偏移 10を越える宇宙にまでおし広げる、「超広視野初期宇宙探査衛星 WISH 計画」についても、紹介す

題目Title:「The extragalactic sky observed with H.E.S.S.」
講師Speaker:Mr. Andreas Zech (Paris Observatory) 
日時:1月19日(水) 午後4時 〜 
Date:  Wednesday, January 19th, 2011 starting at 4 p.m.
The four Imaging Air Cherenkov Telescopes of the H.E.S.S. array in Namibia have been observing gamma-ray sources at very high energies (>  ~100 GeV) since 
2003. The many results from galactic and extragalactic objects have played an important role for our current understanding of the non-thermal universe.
In my seminar I will concentrate on recent results from H.E.S.S. on extragalactic objects. The extragalactic sources detected so far at very high energies 
are all AGN (blazars or radio galaxies) or, since 2010, starburst galaxies. A special focus will be put on the interpretation of the observed spectral 
features of the detected AGN using Synchrotron Self-Compton emission models.
Apart from the obvious astrophysical interest, observations of extragalactic objects at the highest energies provide also a useful tool for probing the 
extragalactic background light, dark matter and Lorentz invariance violation, which will be discussed briefly.

題目Title:「Cataclysmic binaries as turbulence laboratory (flickering activity).」
講師Speaker:Andrej Dobrotka 氏 (京都大学 GCOEポスドク) 
日時:1月14日(金) 午後4時 〜 
Date:  Friday, January 14th, 2011 starting at 4 p.m.
  Flickering is a stochastic brightness variability with red noise
characteristics in power density spectra. In binary accreating systems
it can be caused by turbulent flow in the accretion disc or in the
matter stream from the secondary star. The statistics of the flickering
events then reflect the characteristics of turbulences in these
astronomical flow. The Reynolds number in these systems reach high
values non achievable in today's laboratories (up to 1012). We are
modeling the flickering statistics and we apply this models to
observations of few cataclysmic variables and related object. We are
trying to get some informations about the turbulence characteristics
(dimension scales).

講師Speaker:植村 誠 氏 (広島大学 宇宙科学センター) 
      Dr. Makoto Uemura
日時:1月12日(水) 午後4時 〜 
Date:  Wednesday, January 12th, 2011 starting at 4 p.m.
i)   ブレーザーの可視偏光データを利用した長期・短期変動成分の分離
ii)  矮新星のアウトバースト頻度を考慮した軌道周期分布の推定
iii) 矮新星の早期スーパーハンプを利用した降着円盤の高さマップの再構成

講師Speaker:川口俊宏 氏 (筑波大学 計算科学研究センター) 
      Dr. Toshihiro Kawaguchi
日時:1月7日(金) 午後4時 〜 
Date:  Friday, January 7th, 2011 starting at 4 p.m.



文献:T. Kawaguchi & M. Mori, ApJL, 2010年12月, 724巻, 183--187頁

講師Speaker:川中宣太 氏 (KEK) 
      Dr. Norita Kawanaka
日時:12月17日(金) 午後4時 〜 
Date:  Friday, December 17th, 2010 starting at 4 p.m.

題目Title:「Dynamics of Interstellar Dust」
講師Speaker:Prof. Alex Lazarian
(University of Wisconsin, USA)
日時:12月9日(木) 午後1時 〜 
Date:  Thursday, December 9th, 2010 starting at 1 p.m.
Dust grains get accelerated, get spun up, get aligned. These processes are 
important for understanding of dust grain size distribution, evolution of dust, 
microwave emission of dust as well as dust tracing the direction of magnetic field. 
A number of advances along all of these direction have been done 
within the last decade. In particular, it is now clear that the dust grains 
are moving in typical astrophysical environments with velocities much in 
excess of Brownian velocities. I shall discuss both direct charge - charge 
interaction of grains and the interaction of charged dust with MHD turbulence. 
In terms of the microwave emission, I shall discuss the spinning dust emissivity 
and show how subtle effects of grain wobbling and grain-ion interactions 
change this emissivity. As for grain alignment, radiative torques have been 
established as the major alignment mechanism with the quantitative analytical 
theory of alignment available. Understanding of these basic processes provide 
researchers with tools that they can use to handle quantitatively many 
astrophysical problems, including those related to star and planet formation.

題目:「New Puzzles in Supermassive Black Hole Evolution」
講師:Dr. Charles Steinhardt (IPMU, Univ. of Tokyo) 
日時:10月29日(金) 午後3時 〜
      Friday, October 29th, 2010 starting at 3 p.m.
The standard model of cosmology has been remarkably successful in explaining 
the detailed evolution of galaxies and large-scale structure beginning from 
primordial density perturbations.
Supermassive black holes, however, seem to present a more difficult challenge. 
The standard cosmological model, as currently understood, cannot explain how 
supermassive black holes are born, how they grow, and why or how they die.  
This talk will present a novel approach for analyzing data from quasar surveys 
that reveals new information about the luminosity and evolution of black 
Instead of resolving these problems, the results suggest even deeper puzzles that 
may require new ideas in astrophysics or fundamental physics to resolve.

題目:「The WiggleZ Dark Energy Survey」
講師:Dr. Karl Glazebrook (Swinburne University)
日時:9月30日(木) 午後4時 〜 
      Thursday, September 30, 2010 starting at 4 p.m.
The AAT WiggleZ Dark Energy Survey is measuring 240,000 spectroscopic
redshifts out to z=1 of UV-selected galaxies from the GALEX satellite.
The goal is the FIRST measurement of Baryon Acoustic Oscillations, the
standard ruler in the galaxy distribution, at these high redshifts, as
well as growth of structure and other cosmological parameter
measurements. I will give a short review of the WiggleZ survey  and
present some early cosmological results including our first BAO detection.

題目:「Mapping Reionization in the Local Universe」
講師:Dr. Lee Spitler (Swinburne University of Technology)
日時:9月28日(火) 午後4時 〜 
(September 28 (Tue), 2010,  16:00 -  )
場所:理学研究科4号館 3階 328号室 ●場所に注意!●
(Room 328[3F], Building No.4)
In a cold dark matter dominated Universe, structure grows via assembly
and hierarchical merging of small dark matter halos.  Recent N-body
cosmological simulations have shown that the present-day spatial and
kinematic distribution of objects formed within dark matter halos that
collapsed early in the Universe (z > 10) can be used to constrain the
epoch of their formation.  For certain classes of objects, this method
can yield important constraints on the epoch of reionization around a
given galaxy.  In this talk, I will apply this technique to
observations of a globular cluster system in a nearby massive
elliptical galaxy.  I will show that despite various uncertainties,
the derived epoch of reionization is competitive with other estimates.
 Future work could help determine how reionization propagated from
galaxy to galaxy in the local Universe.

題目: 「UV radiation effect on the dynamical evolution of 
       Molecular clouds (BRCs) at HII Regions」
講師: Jingqi  Miao 氏
       (School of Physical Sciences, University of Kent)
日時: 2010年7月28日(水)午後4時〜	
       Wednesday, July 28th, 2010 starting at 4 p.m.	
概 要  Abstract:
Formation of elephant trunks and BRCs at HII boundary opens an window
for one to investigate the feedback of the newly formed OB stars to
their surrounding molecular clouds.  We have investigated the UV
radiation triggered morphological evolution and star(s) formation in
BRCs by using a comprehensive 3D model based on SPH. The mechanism of
the formation of different types of morphologies of BRCs have been fully
addressed and a new type of BRC morphology is defined. The relation of
BRC’s morphology to the possibility of triggered star formation in some
of the observed BRCs is discussed, which provides a signpost for
astronomers in the field.
Further simulations on prolate and initially clumpy MCs will reveal new
insight to the UV radiation effects on the dynamical evolutions of
molecular clouds of more realistic initial conditions. The possibility
of triggered star cluster formation in BRCs by the UV radiation from
nearby OB stars will be discussed.

題目: 「活動銀河ジェットの理解にむけて:最近の話題から(仮)」
講師: 片岡 淳 氏 (早稲田大学 理工学術院)
日時: 2010年7月15日(木)午後3時30分〜	
       Thursday, July 15, 2010 starting at 3:30 p.m.	
概 要  Abstract:
マ でありながら、その生成メカニスムや加速機構、さらには組成(レプ

題目: 「Chemical abundances in planet harbouring stars」
講師: Garik Israelian 氏 
      (Institute of Astrophysics of Canary Islands, Spain)
日時: 2010年7月2日(金)午後2時〜	
     Friday, July 2nd, 2010 starting at 2 p.m.	
概 要  Abstract:
Extensive spectroscopic studies of stars with and without planets have
concluded that stars hosting planets are significantly more metal-rich
than those without planets. More subtle trends of different chemical
elements begin to appear as the number of detected extrasolar planetary
systems continues to grow reaching almost 500.
I review our current knowledge concerning the observed abundance trends
of various chemical elements in stars with exoplanets and their possible
implications. Most interesting trends appear for light elements Li and
Be which may hide a link between rotation of stars and disks and
formation of planets.

題目: On the Evolution of Quasar Host Galaxies
講師: Malte Schramm 氏 (Dept. of Astronomy, Kyoto Univ.)
日時: 2010年6月4日(金)午後4時〜
       Friday, June 4, 2010 4 p.m. -

概 要  Abstract:
Quasars are extremely luminous galactic nuclei, drawing their energy
through gravitational accretion of matter onto supermassive black holes
in the galaxy centres. The tight observed correlations of the mass of
the central black hole with the global properties of the host galaxy
bulge (i.e. stellar velocity dispersion sigma, mass, and luminosity)
indicate a close connection between galaxy formation and nuclear
activity. Outside of the very local universe, quasars (more generally:
Active Galactic Nuclei) are the only galaxies where we can more or less
robustly estimate black hole masses. Therefore, they become also
important for the study of galaxy evolution in a cosmological context.
The evolution of quasar host galaxies is still hardly studied at high
redshifts (z>~2), although this is a very interesting redshift range as
both the quasar activity and the star formation rate density have their
peak at z~2-3. I report on recent advances in quasar host galaxy studies
involving mostly data from the Hubble Space Telescope and the ESO-VLT. I
will show our progress in the determination of the stellar mass content
of the hosting bulges for various cosmological epochs. Finally, I will
discuss the results of our studies on the relations between the growth
of supermassive black holes and their host galaxy.

題目: 「すざく」による天の川銀河中心領域の観測と今後の展望
講師: 鶴 剛 氏 (京大物理・宇宙線研究室)
日時: 2010年5月21日(金)午後4時〜
    Friday, May 21st, 2010 starting at 4 p.m.

概 要  Abstract:
つは冷たい中性鉄が放射する蛍光Kα 輝線(6.4keV輝線)である。GCDXの発見から