[Speaker 1]
Giono Gabriel D1, SOKENDAI, Mitaka（supervisor : Yoshinori Suematsu）
[Title]
Experimental confirmation for CLASP’s spectrograph alignment procedure
[Abstract]
–

[Speaker 2]
Onoue Masfusa M1, SOKENDAI, Mitaka（supervisor : Nobunari Kashikawa）
[Title]
High-z Quasar Selection with Hyper Suprime-Cam
[Abstract]
Quasars at high (>6) redshift are one of the best tracers of early Universe,
thanks to its high luminosity and characteristic spectrum.
However, quasars are very rare objects and it is important to establish a method to
select quasars effectively.
Based on the above, I will present the strategy for identifying high-z quasars by using SED fitting (#HSC project 47).
The goal of this study is to effectively isolate high-z quasars from contaminating sources such as brown dwarfs.
We are going to apply SED fitting method for quasar selection along with conservative two-color selection.
I will report the current status of SED fitting code development, and preliminary results of its application.
In addition, I would like to introduce the recently found three z~7 quasars (Venemans+13).

[Speaker 1]
Anjali John K D3, SOKENDAI, Mitaka（supervisor : Suematsu Yoshinori）
[Title]
Temporal evolution of the Sun’s Polar Magnetic Patches as observed with Hinode
[Abstract]
The Sun’s polar region is covered by countless discrete flux elements called as magnetic patches. The magnetic patches are believed to be formed from the remnant magnetic flux from the active latitudes which is transported to the polar region through diffusion and meridional circulation. It is likely that large unipolar patches with magnetic flux >10^18 Mx determine the magnetic polarity of each poles and their total flux is modulated by the solar cycle. It is important to understand the temporal evolution of these large patches to derive information of magnetic activities in the polar region, especially, the mechanism of magnetic polarity reversal. We also like to investigate the interaction between magnetic patches and the polar faculae whose occurrence tends to be associated with the large magnetic patches, according to our previous study. We obtained Hinode/SP and FG data for six hours of the south polar region in March 2013. We will show results obtained from this analysis.

[Speaker 2]
Ayumu Matsuzawa D1, SOKENDAI, Mitaka（supervisor : Satoru Iguchi）
[Title]
Absorbing spectrum in galactic nucleus of M87 from VLBA archive data
[Abstract]
Super Massive Black Hole (SMBH) in Active Galactic Nuclei (AGN) attracts matters to form an accretion disk by its strong gravity. AGN is very bright than normal galaxy due to huge luminosity of accretion disk. In order to emit the huge luminosity, that requires a lot of accretion matter accreting to SMBH. The absorption was seen in spectrum of VLBI observation near SMBH. There are the two possibilities that absorption as synchrotron-self-absorption (SSA) from optically thin region of AGN jet or free-free-absorption (FFA) from cold dense plasma around SMBH. This cold dense plasma (we called FFA plasma) was considered as accreting matter to SMBH. The analysis of FFA around SMBH has been used to investigate this kind of accretion process at very vicinity (~pc-scale) of the BH. The purpose of my research is probing the FFA plasma around SMBH of M87. M87 is one of very important object, because M87 has the second-largest apparent Schwarzschild radius next to SrgA*.In order to probe the FFA plasma around SMBH of M87, we required the absorption spectrum of VLBI observation near SMBH of M87.We make the SED with seven frequencies (0.324, 1.6, 2.2, 4.9, 8.4, 15, 22GHz) on SMBH of M87 from VLBA archive data to confirm the absorption spectrum and the SED shown absorption spectrum.

[Speaker 1]
Junya Sakurai M2, SOKENDAI, Mitaka（supervisor : Satoshi Mitayaki）
[Title]
Mass map measurement for Deep Lens Survey Field
[Abstract]
Measurement the evolution of dark matter distribution is the important
cosmological probe. For this probe, one of the promising techniques is
weak gravitational lensing. This measurement is sensitive to any
systematic biases in measured quantities. lensfit (L. Miller et al., 2007)
we use is able to yield unbiased measurement. Since lensfit has
recognized as one of the most reliable tools based on mock simulation
data analysis, we try to apply lensfit to Subaru Suprime-Cam data
analysis.

We get optical imaging data of Deep Lens Survey Field 2 from SMOKA. We
select galaxies with 23

　本年も、国立天文台の特別公開（10/18-19）に合わせて総合研究大学院大学（以下総研大）天文科学専攻の特別公開が行われました。
　天文科学専攻には現在約30名の学生が在籍し、国立天文台の施設を拠点に日々の研究生活を送っています。「総研大生の研究ライフ2013」と題した今回の企画では、天文科学専攻の学生が普段どのようなテーマで研究を行っているのかをポスターや映像で紹介しました。これらの準備には約1ヶ月を費やしましたが、担当学生がそれぞれのアイデアを出しあって例年以上に充実した内容となりました。
　特別公開当日は幅広い年代の方（300人以上）が来場し、総研大、及び天文科学専攻について広く知って頂くことができました。また、来場者の中には学部生なども多く、総研大への進学を検討している方には重要な機会となっているようです。そのため、今後はオープンキャンパスのような一面を企画に盛り込むことも検討することにしました。他にも多くの反省点が挙げられ、国立天文台に所属する学生としての特別公開への関わり方を議論していく必要がありそうです。

文責：　総合研究大学院大学　天文科学専攻　博士過程3年　橋詰　克也

[Speaker 1] Sukom Amnart
AffiliationD3, SOKENDAI, Mitaka（supervisor : Saeko Hayashi）
[Title]TBA
[Abstract]TBA

[Speaker 2]Sako Nobuharu
AffiliationD3, SOKENDAI, Mitaka（supervisor : Tetsuya Watanabe）
[Title]
An energetics study of X-ray jets
[Abstract]For plasma acceleration in X-ray jets, three mechanisms have been considered, based on the reconnection model of X-ray jets; The reconnection jet produced by magnetic tension, the evaporation flow produced by pressure gradient, and the twisted jet produced by magnetic pressure. There are some evidences of X-ray jets in active regions (ARs) produced by pressure gradient. On the other hands, there is no observational evidence of X-ray jets by the other forces. In order to distinguish the evaporation flow from the other types of jets, I have studied the energetics of the X-ray jets.
Using over 100 X-ray jets greater than 3×104 km in length in ARs, quiet regions (QRs), and coronal holes (CHs), I have find no large differences in the life time, the width of the jets, and the area of the footpoint flares in such regions. On the other hands, the plasma number density of the X-ray jets and flares in ARs is ten times larger than those in QRs and CHs. From a comparison of the energy flux of the jets with the energy flux from the reconnection sites, which is estimated from the footpoint flares, I have found that the some events are consistent with the prediction from the evaporation flow. The energy fluxes of the other events are larger than the energy flux from the reconnection site. The kinetic energy fluxes of these jets are larger than the thermal fluxes. In my presentation, I will discuss the details.