## 第243回: 2014/04/17 (Thu) 15:30-16:30 †

### Title: 重力波天文学時代の突発天体観測 †

Abstract:
2017年頃からの稼働を予定している次世代重力波望遠鏡によって、

しかし、重力波による位置決定精度は数10平方度程度であり、

(2) 連星中性子星合体から期待される電磁波放射の理論的研究を紹介します。
これらをもとに、重力波天文学時代にどのような電磁波観測が必要かを議論します。

## 第244回: 2014/04/24 (Thu) 15:30-16:30 †

### Title: 南極天文学開拓のための可搬型サブミリ波望遠鏡の開発 †

Abstract:ドームふじ基地は昭和基地から1000km内陸の高地にある

グループはドームふじ基地に10m級のテラヘルツ望遠鏡、2.5m級の

すべくサイト開拓と望遠鏡開発を進めている。
テラヘルツ望遠鏡の設置に向け、私たちはプロトタイプとなる

500GHz帯ヘテロダイン受信機を備え、南極での望遠鏡運用技術の

および[CI](3P1-3P0)輝線での銀河面サーベイを行う。本講演では、

での運用に先立ちチリで実施した試験観測の結果およびテラヘルツ

## 第245回: 2014/05/08 (Thu) 15:30-16:30 †

### Title: N体シミュレーションで探る星団の形成と進化 †

Abstract: N体シミュレーションは星一つ一つの運動を計算することで、恒星系全体の進化
を明らかにすることができる強力なツールである。N体シミュレーショ ンを用いた

モデルから、近年、より現実の星形成領域に近いフィラメ ント状やクランプ状の

## 第246回: 2014/05/12 (Mon) 16:00-17:00 ※曜日、開始時刻注意 †

### Title: Reversals and Dynamics of the magnetic field generated by dynamo instability †

Abstract: The magnetic field of astrophysical objects is generated by the dynamo
effect: an instability that converts kinetic energy into magnetic one.
Since the beginning of the 20th century, it is known that the magnetic
field of the Earth does not remain of same direction at all time but
from time to time it  reverses and changes polarity.

I will show results of recent laboratory experiments in which a magnetic
field is generated by dynamo effect and reverses in an apparently random
manner. I will explain what mechanism is responsible for magnetic field
reversals in the experiment and show that this mechanism explains
several properties of the dynamics of the Earth's magnetic field.

## 第247回: 2014/05/15 (Thu) 15:30-16:30 †

### Title: The first stars: their diversity and beyond †

Abstract: 初期宇宙で生まれた星(初代星)は銀河系の星と比べると質量が大きかったと考えられている。具体的にその典型質量が

いくらだったのか、またその質量分布がどんな形をしていたのかという問題は最も基本的かつ未解決の問題である。
このセミナーでは、特に最近活発に議論されているこの初代星の質量、質量分布問題の最近の進展についてまとめる。

すでに10^9Msunを上回る超巨大ブラックホールが存在することが観測的に知られるようになり、この起源として超大質量天体の

## 第248回: 2014/06/19 (Thu) 15:30-16:30 †

### Title: 星周環境における PAH とそのスペクトルの進化 †

Abstract:
Polycyclic Aromatic Hydrocarbons (PAHs) はベンゼン環が多重縮合した構造を持った分子であり，

メカニズムから， PAH の放射は星間輻射場強度の指標としても注目されている．銀河系において PAH は

## 第249回: 2014/06/26 (Thu) 15:30-16:30 †

### Title: 星形成銀河の星間物質の電離状態 †

Abstract:

## 第250回: 2014/07/03 (Thu) 15:30-16:30 †

### Title: Two gamma-ray bursts from dusty regions with little molecular gas †

Abstract: Long-duration gamma-ray burst (GRB)は、大質量星の爆発に関係しており、

GRB母銀河におけるCO分子輝線（分子ガスのトレーサー）探査では、放射は全く

CO輝線及び1.2mm連続波の観測を行った。その結果、両銀河においてCO輝線と連続波を、

GRB発生場所で強く検出された。連続波は、その検出位置やSED等から星形成活動に

GRBが発生した星形成領域に存在する大質量星からの強いUV輻射場によって分子ガスが

## 第251回: 2014/07/17 (Thu) 15:30-16:30 †

### Title: Analytical computation of generalized Fermi-Dirac integrals by truncated Sommerfeld expansions †

Abstract:
For the generalized Fermi-Dirac integrals, $F_k(\eta,\beta)$, of orders
$k=-$1/2, 1/2, 3/2, and 5/2, we explicitly obtained the first 11 terms of
their Sommerfeld expansions. The main terms of the last three orders
are rewritten so as to avoid the cancellation problem. If $\eta$ is not so small,
say not less than 13.5, 12.0, 10.9, and 9.9 when $k=-1/2$, $1/2$, $3/2$,
and $5/2$, respectively, the first 8 terms of the expansion assure the single
precision accuracy for arbitrary value of $\beta$. Similarly, the 15-digits
accuracy is achieved by the 11 terms expansion if $\eta$ is greater than
36.8, 31.6, 30.7, and 26.6 when $k=-1/2$, $1/2$, $3/2$, and $5/2$, respectively.
Since the truncated expansions are analytically given in a closed form,
their computational time is sufficiently small, say at most 4.9 and 6.7 times
that of the integrand evaluation for the 8- and 11-terms expansions,
respectively. When $\eta$ is larger than a certain threshold value as indicated,
these appropriately-truncated Sommerfeld expansions provide a factor of
10-80 acceleration of  the computation of the generalized Fermi-Dirac integrals
when compared with the direct numerical quadrature.

## 第252回: 2014/08/21 (Thu) 15:30-16:30 †

### Title: 最盛期の銀河形成を解剖する †

Abstract:
z=1-3の時代は銀河形成・進化の最盛期と考えられており、近年ではこの時代の銀河を空間分解して、

すばる望遠鏡による観測成果と共にレビューする。

## 第253回: 2014/10/8 (Wed) 13:30-14:30 †

### Title: "Native Andean and Amazonian Astronomy" †

Abstract: (N/A)

### Title: "Archaeology and cultural heritage in the context of ALMA and TAO project" †

Abstract: The ALMA Project is the largest astronomical project worldwide.
It develops on the Chilean high plateau named
Chajnantor, located in the Atacama Desert at 5200 m. above sea level. The TAO
Observatory from University of Tokyo is on the summit of Chajnantor Mountain,
being the highest in the world at over 5800 m.a.s.l.
I studied both places where they have developed these projects, identifying the
cultural findings that they may have, as an environmental consultant,
discovering archaeological sites, and creating a Site Museum. As an environmental
consultant, I worked all over the Atacama Desert. From the Andes High Mountain
Range to the Pacific Ocean with a multidisciplinary team, that knows everything
about the cultural heritage, environmental laws, social problems, flora and fauna.
In a zone where today has many mine development projects, renewable energy
sources projects, roads and constructions projects. A zone that is fragile and at the
same time, a zone that is very harsh to live in.

## 第254回: 2014/10/16 (Thu) 15:30-16:30 †

### Title: The Puzzle of Massive Star Formation: A Multi-wavelength Approach †

Abstract: The mystery of high-mass star formation can be solved like a puzzle,
whose pieces are of different sizes/shapes and hidden in different star-forming regions.
This talk will feature observational results of a number massive star formation regions
(Cepheus A, Gem OB1, NGC 6334, AFGL-333) at different wavelengths and angular resolution.
Considering that no single star-forming region can provide us with all the pieces of the puzzle,
I have extracted clues from as many regions as possible to describe the different stages
and scenarios of massive star formation.

## 第255回: 2014/10/23 (Thu) 15:30-16:30 †

### Title: Decomposition of the 3 micron feature in AKARI grism spectra †

A significant percentage of the carbon in our galaxy is expected to be contained
within large polycyclic aromatic hydrocarbon (PAH) molecules and related carbonaceous species.
However, the specific details of these species are still a topic of active research.
This work analyses the 3.3 micron feature and the sub-features contained therein,
in order to better understand the morphology and nature of the molecular carriers.
Current results are discussed in terms of line intensity ratios, and molecular stability
and fragmentation pathways.

## 第256回: 2014/11/20 (Thu) 15:30-16:30 †

### Title: Spatially resolved physical conditions in M83, revealed by the Herschel SPIRE FTS †

Since the launch of the Herschel Space Observatory, our understanding about the photo-dissociation
regions (PDR) has taken a step forward. In the bandwidth of the Fourier Transform Spectrometer (FTS)
of the Spectral and Photometric Imaging REceiver (SPIRE) on board Herschel, ten CO rotational transitions,
including J=4-3 to J=13-12, and three fine structure lines, including [CI] 609, [CI] 370, and [NII] 250 micron,
are covered. In this talk, I present our findings from the FTS observations at the nuclear region of M83,
based on the spatially resolved physical parameters derived from the CO spectral line energy distribution
(SLED) map and the comparisons with the dust properties and star-formation tracers. I will discuss
(1) the potential of using [NII] 250 and [CI] 370 micron as star-formation tracers; (2) the reliability of
tracing molecular gas with CO; (3) the excitation mechanisms of warm CO; (4) the possibility of studying
stellar feedback by tracing the thermal pressure of molecular gas in the nuclear region of M83.

## 第257回: 2014/12/04 (Thu) 15:30-16:30 †

### Title: 銀河衝突に伴う巨大ブラックホールの進化 †

　銀河が周辺銀河と衝突・合体しながら成長するの
にあわせ、銀河中心の巨大ブラックホールも同様に

ションと放射スペクトルの理論計算を基に、アンド
ロメダ銀河に衝突した衛星銀河の元中心ブラックホ
ールを探査する研究を行ってきました(Miki et al.
2014; Kawaguchi et al. 2014)。
衛星銀河の大部分は、潮汐力により散り散りにな
りアンドロメダストリームなどを形成している一方、

アンドロメダ銀河円盤の外縁部に居ると考えられま
す。我々の計算結果は、漂う巨大ブラックホールへ
の星間ガスの降着流は電波波長域で、星団は近赤外

近年の電波・可視光・X線観測結果が示す、このよ
うな漂う巨大ブラックホールが原因と考えられる天

## 第258回: 2015/1/29 (Thu) 15:30-16:30 †

### Title: The E-ELT project and stellar populations †

We briefly outline the current status of the E-ELT project.
In particular, we will focus our attention first light and
first generation of E-ELT instruments. We present a selection of
stellar astrophysics science cases for E-ELT. We will also disucss
the role that E-ELT will have on a few open problems concerning
evolved stellar populations in nearby stellar systems.
We will also outline the role that deep NIR photometry and
multi-object spectropgraph will have in  addressing
current challenges of resolved and unresolved stellar populations.

## 第259回: 2015/2/16 (Mon) 14:00-15:00 †

### Title: MaNGA: Mapping Nearby Galaxies at APO An IFU Survey of 10,000 Galaxies †

I will discuss the design and execution of a new survey to obtain resolved spectroscopy
for 10,000 nearby galaxies called MaNGA (Mapping Nearby Galaxies at Apache Point Observatory).
One of three core programs in the 6-year SDSS-IV project that began on July 1st, 2014,
MaNGA will deploy 17 fiber-bundle IFUs across the Sloan 2.5m Telescope's 3 degree field-of-view,
targeting a mass-selected sample with a median redshift of 0.03, typical spatial resolution of 1-2 kpc,
and a per-fiber signal-to-noise ratio of 4-8 in the outskirts of target galaxies.  For each galaxy
in the sample, MaNGA will provide maps and measured gradients of the composition
and dynamics of both stars and gas.  I will present early results using a prototype instrument
that highlight MaNGA's potential to shed light on the ionization and chemical enrichment of gas
in galaxies, spatial patterns in their star formation histories, and the internal makeup of
stellar populations.  MaNGA's unprecedented data set will not only provide powerful new
insight on galaxy formation and evolution but will serve as a valuable benchmark for future
high-z observations from large telescopes as well as JWST.

## 第260回: 2015/2/19 (Thu) 15:30-16:30 †

### Title: Resolving the Obscured Cosmic Accretion History and Modes of Galaxy Assembly †

Dust obscuration has hidden at least half of the cosmic accretion
activity and concealed the most intense sites of star formation during
the peak epoch for both processes in galaxy evolution at 1 < z < 3.
Centimetric radio interferometry is the only means of identifying the
AGNs and tracing star-forming activities at sub-arcsecond resolution,
in an extinction-independent manner.  I will discuss the use of radio
survey to study star formation and AGN at 1 < z < 3, focusing on the
early results from two ultra-deep 4-8 GHz Jansky VLA (JVLA) radio
observations at 0.3" resolution in the UDS and HUDF fields. The goals
of these surveys are to combine the radio data with the existing
panchromatic observations to produce a complete census of AGN and to
spatially resolve the star-forming galaxies. The ongoing survey in the
HUDF, in particular, will reach 0.3 microJy/beam RMS and will provide
the definitive radio dataset for spatially-resolved, ultra-deep,
broadband extragalactic studies until the SKA era.