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

[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.

[Speaker 1]
Yuriko Saito
D1, SOKENDAI, Hawaii（supervisor : Masatoshi Imanishi）
[Title]
Investigating the coevolution between SMBHs and galaxies at z~3
-our first result-
[Abstract]
In the local universe, there is a tight correlation between the masses
of super massive black holes (SMBHs) and stars in the spheroidal
components (bulge and elliptical galaxies), suggesting that their formation
is physically closely related. Various models assuming different physical
mechanisms are proposed to explain the observational result at z=0.
Since these models predict different redshift evolution of the
SMBH-spheroid mass ratio, it is important to observationally constrain
the mass ratio at high redshift. As the predicted difference becomes
larger at higher redshift, going to higher redshift is better to distinguish
among these models, but at the same time observational difficulties
increase at higher redshift. By taking into account these factors,
we have concluded that z=3-3.5 is practically the best redshift range.
However, previous studies have mostly been limited to z<2. We have embarked on (1) systematic near-infrared spectroscopy of z=3-3.5 QSOs, to derive the SMBH masses, based on the the Balmer beta emission line width and nearby continuum luminosity, and (2) Subaru LGS-AO near-infrared multi-color imaging observations, to estimate spheroidal stellar masses in the host galaxies of these QSOs. We obtained spectroscopic data for 34 objects, and succeeded to derive BH masses for 24 objects among them. We have also performed Subaru AO imaging observations of 8 QSOs with estimated SMBH masses, and so far completed AO imaging data analysis of J0725. In this talk, I will present our first result of SMBH mass – bulge mass ratio calculated for J0725. [Speaker 2] Shogo Ishikawa M2, SOKENDAI, Mitaka（supervisor : Nobunari Kashikawa） [Title] The clustering properties of star-forming galaxies at z~2 by extremely wide-field survey [Abstract] One of the most critical method to trace the evolution history of galaxies is to compare the mass of dark haloes. Dark halo mass monotonically grows by merging with cosmic time、 so this parameter reflects the growing history of galaxy directly. In recent years, a number of LBGs/LAEs at z>3 are obtained and dark halo masses of z>3 galaxies are revealed.
On the other hand, dark halo masses at z~2 is not so much explored because there are technical difficulties to observe galaxies at z~2. That is why z~2 is known as “redshift-desert”; however, z~2 is also thought to be a important era to study galaxy formation and evolution.
We conducted the wide field survey to obtain star-forming galaxies at z~2, applying so called “BzK selection technique”. In this talk, we report the results of clustering analysis of star-forming galaxies at z~2. Especially, we performed the full HOD analysis of z~2 galaxies the first in the world.