[Speaker1]
Yuriko Saito, D2, SOKENDAI, Mitaka(supervisor: Masatoshi Imanishi)
[Title]
Investigating the coevolution between SMBHs and galaxies at z~3 -error estimate-
[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.

To achieve our goal, we have been carried out both spectroscopic and imaging observations, and obtained 37 spectroscopic data and 9 imaging data of z~3 quasars. We completed to analyze spectroscopic data and obtained BH masses for 28 out of 37 objects.
Now we have started imaging data analysis and obtained preliminary result of SMBH-spheroid mass ratio at z~3 (previous talk).
However, there is too large uncertainty to constrain the mass ratio and it is important to reduce the error.

There are three noise sources that contribute to the total error of SMBH-spheroid mass ratio.
1) BH mass error : BH mass is estimated from the Balmer beta emission line width and AGN luminosity at 5100A. So this error is dominated by line width error (i.e. spectral fitting error) and luminosity error (i.e. S/N ratio at ~5100A), and has been already estimated for 28 objects.
2) Spheroidal luminosity error : spheroidal luminosity is estimated by decomposing AGN and host galaxy radiation by fitting both components.Thus, we should consider the fitting error carefully and try to reduce it.
3) Mass to luminosity ratio (M/L) error : to estimate spheroidal mass,we convert spheroidal luminosity to mass using M/L ratio which is derived from host galaxy color in this study. Therefore, accurate M/L determination and reducing its error is crucial.

In my past talks, I have been presented BH mass estimates, our preliminary results of spheroidal mass estimates and the redshift evolution of SMBH-spheroid mass ratio.
In this talk, I will explain errors that we should care for the accurate mass ratio determination with introducing related papers,and present current progress of error estimate.

[Speaker2]
Anjali John, D3, SOKENDAI, Mitaka(supervisor: Y.Suematsu)
[Title]
Unipolar Appearance and Disappearance of the Sun’s Polar Magnetic Patches

[Speaker 1]
GIONO Gabriel, D2, SOKENDAI, Mitaka（supervisor：Suematsu Yoshinori, Katsukawa Yukio, Hara Hirohisa）
[Title]
Current progress on the CLASP telescope alignment.
[Abstract]
The Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) is a sounding rocket instrument currently under development at NAOJ. CLASP aims to measure for the first time the polarization of the Lyman-Alpha line (121.6nm) emitted from the solar upper-chromosphere and transition region, and derived the magnetic field strength and orientation through the Hanle effect.
CLASP instrument is composed of a classical Cassegrain telescope focusing the light inside an inverse-mount Wadsworth spectrograph. A polarization analyzer is located on both of the two channels, and a rotating half-waveplate is used for the polarization modulation.
As part of CLASP development, both telescope’s primary and secondary mirrors have to be properly align in order to ensure a good image and spectrum quality.
In this colloquium, the current progress on the telescope’s alignment will be presented. As an introduction, the experiment “double-pass” configuration will be explained as well as the basic principle of telescope’s alignment. Then, the measured wavefront error (WFE) and how it was retrieved from the interferences fringes will be shown. Finally, the adjustment estimation on the secondary mirror tilt will be derived by comparing the WFE aberration coefficient to ray-tracing simulations.

[Speaker 1]
Taiki Suzuki, D1, SOKENDAI, Mitaka（supervisor：Masatoshi Ohishi）
[Title]
Survey Observations and Formation Process of Methylenimine (CH2NH)

[Speaker 2]
Jun Toshikawa, D3, SOKENDAI, Mitaka（supervisor：Nobunari Kashikawa）
[Title]
High Redshift Protoclusters: comparison with theoretical model

[Speaker 1]
Rhythm Shimakawa M2, SOKENDAI, Mitaka（supervisor : Kodama Tadayuki）
[Title]
Metal enhancement of the protocluster galaxies at z=2.2
[Abstract]
Protoclusters are the ideal laboratories to study how the strong environmental dependence in galaxy properties seen today was initially set up. We conducted a near-infrared spectroscopy of star-forming galaxies (H-alpha emitters) associated with two protoclusters at z=2.2&2.5 with MOIRCS/Subaru.
Shimakawa et al. (2014) have confirmed that the two protoclusters are the right ancestors of today’s largest clusters like ‘Coma’, and now we are studying the physical characteristics of the memberships in the respective protoclusters.
This talk focuses on one of our recent results regarding the environmental dependence of mass-metallicity relation seen in the protocluster, PKS1138-262 at z=2.2. The mass-metallicity relation provides crucial insights into star formation history, gaseous inflows and outflows.
As a result, we find a clear excess of the gaseous metallicities of the protocluster galaxies at the stellar mass of < 1E11 Msun. We suggest that it can be explained by the 'downsizing effect' or 'gas recycling' in the protocluster region.

[Speaker 1]
Nobuyuki Sakai D3, SOKENDAI, Mitaka（supervisor : Mareki Honma）
[Title]
The first astrometry result of the Perseus arm beyond a Galactic longitude l of ~ 190 deg with VERA
[Abstract]
Contexts. Currently, VERA and VLBA have been conducting kpc-scales astrometry to make a 3D map of the Milky Way Galaxy.
AIms. We aim to expand previous astrometry coverage of the Perseus arm from a Galactic longitude l of ~ 190 deg to that of ~ 240 deg.
This is crucial to accurately understand large scale structure of the Perseus arm.
Methods. We carried out nine-epochs VERA astrometry observations toward massive star-forming region IRAS 07427-2400 (l = 240.3 deg, b = 0.1 deg, Vlsr = 68.0 km/s) between January 20, 2012 and September 16, 2013.
Results. The measured parallactic distance is 5.18 +0.79/-0.59 kpc, which places the source in the 3rd Galactic quadrant of the Perseus arm.
Discussions. A combination of our astrometry result and previous ones reveal that the pitch angle of the Perseus arm is constant (i = 17.7 +/- 1.8 deg) in 94.60 deg < l < 240.32 deg, although the pitch angle is changed significantly (i = 11.5 +/- 1.3 deg) in 43.17 deg < l < 94.60 deg. The difference indicates that bifurcation or spur as seen in external disk galaxies may occur in 43.17 deg < l < 94.60 deg for the Perseus arm. [Speaker 2] Shino Nagisa D2, SOKENDAI, Mitaka（supervisor : Mareki Honma） [Title] Methanol maser observation of massive star formation region IRAS 18089-1732 [Abstract] The formation scenario of massive star is not yet fully understand. Methanol maser is regarded as the signpost of the formation process of the massive star. Particular, the 44GHz methanol maser is associated with an outflow, and it is said that the 6.7GHz methanol maser is associated with an accretion disk. If this is true, 44GHz methanol maser is expected to be distributed perpendicularly with respect to rotating disk. Detecting (or rejecting) this will play a major role in understanding the scenario of massive star formation. In order to test this, we observed 6.7GHz methanol maser using JVN and obtained space distribution map. We also analyzed the VLA archive data of the 44GHz methanol maser. We were able to get the space distribution map of the 44GHz methanol maser and the 6.7GHz methanol maser of IRAS18089-1732. We argue about each emission position from the result.