[Speaker1]
Tsuguru Ryu, SOKENDAI D3 (Supervisor; Motohide Tamura)
[Title]
Direct imaging of intermediate mass giants with RV trends IV

[Speaker2]
Noriharu Watanabe, SOKENDAI M2 (Supervisor; Norio Narita)
[Title]
Doppler Tomographic Mesurent for Planetary Orbital Obliquities

[Speaker1]
Kotomi Taniguch, SOKENDAI D3 (Supervisor; Masao Saito)
[Title]
Survey Observations in the 45 GHz and 90 GHz Bands toward High-Mass Star-Forming Regions
[Abstract]
We carried out survey observations of carbon-chain molecules and N2H+ in the 45 GHz and 90 GHz bands toward high-mass starless cores (HMSCs) and high-mass protostellar objects (HMPOs) with the Nobeyama 45-m radio telescope in the last two observational seasons. Our main purpose is to investigate the chemical evolution in the high-mass star-forming regions. We compare the I(N2H+)/I(HC3N) ratios using the 90 GHz band lines among HMSCs and HMPOs, and found that the ratios decrease from HMSCs to HMPOs, in contrast to the low-mass star-forming regions and giant molecular clouds. The column density of HC3N derived from 45 GHz line is well correlated with the integrated intensity of CCS, but that derived from 82 GHz line is not correlated. The high-excitation energy HC3N is enhanced in HMSCs where SiO has been detected. From these results, we propose that HC3N is re-generated in the shock regions driven by molecular outflows.

[Speaker2]
Misaki Ando, SOKENDAI D1 (Supervisor; Daisuke Iono)
[Title]
Molecular Gas Obsarvation in Local Merging U/LIRGs

[Speaker1]
Haruka Baba, SOKENDAI D3 (Supervisor; Motohide Tamura)
[Title]
Imaging analysis of Taurus Molecular Cloud

[Speaker2]
Hiroyuki Ishikawa, SOKENDAI M2 (Supervisor; Takayuki Kotani)
[Title]
Reduction and Future Applications of IRD Data

[Speaker1]
Pathak Prashant, SOKENDAI D3 (Supervisor; Prof. Hideki Takami)
[Title]
On-sky Closed-loop Atmospheric Dispersion Compensation: Demonstration of Sub-milliarcsecond Residual Dispersion Across H-band.

[Speaker2]
Tadafumi Matsuno, SOKENDAI D1 (Supervisor; Wako Aoki)
[Title]
Chemical Abundances of Extremely Metal-Poor Turn-Off Star
[Abstract]
I will start my talk with introduction to the
Galactic Archaeology and metal-poor stars. In the latter part, we
present our latest results of abundance analysis for extremely
metal-poor turn-off stars. The discussion includes i) lithium
abundance below [Fe/H]=-3.5, ii) chemical inhomogeneity in the early
Universe in comparison to supernova yield with special focus on
[Na/Fe] bimodality, and iii) binary mass transfer of materials
enriched with slow neutron capture process elements enhancement and
thermohaline mixing.

[Speaker1]
Tomonari Michiyama, SOKENDAI D2 (Supervisor; Daisuke Iono)
[Title]
Dense molecular outflows from the merging LIRG NGC3256
[Abstract]
We report the new ALMA Cycle 3 results of line survey towards a late stage merging galaxy NGC 3256. NGC 3256 hosts two merging nuclei and the starburst and AGN activities are strongly affecting the chemical and physical properties of the ISM. We have detected more than 20 molecules (e.g., c-C3H2, H13CN, H13CO+, SiO, CCH, HCN, HCO+, HNC, CH3OH, CS, HC3N, CH3CCH, C18O, 13CO) at 2” angular resolution, which is high enough to resolve the double nuclei. In this presentation, we focus on CO, HCN and HCO+ to discuss the high velocity components detected only by those bright molecular lines. Such high velocity components are though to be molecular gas outflow from northern and southern nuclei. Including the CO(1-0) and CO(3-2) archived data, the line ratios suggest that (1) The excitation condition become weak towards edge of the outflow in the starburst triggered outflow. (2) In the case of low luminous AGN like southern nucleus in NGC 3256, the outflowing gas is associated with AGN jet, and warm and dense gas can be newly formed due to interaction between jet and ISM interaction.
(3) The HCN is enhanced due to shock especially in red-shifted outflow. In addition, we conducted radiative transfer modeling. By using a Bayesian likelihood analysis, we found that the CO column density and filling factor of outflowing gas is smaller than the gas around nuclei.

[Speaker2]
Satoshi Kikuta, SOKENDAI D1 (Supervisor; Masatoshi Imanishi)
[Title]
Lyman-alpha emission as a tool to probe galaxy formation
[Abstract]
Lyman-alpha emission line is the strongest line from astrophysical sources and can be used to probe galaxy formation especially at high-redshift (z>2) Universe. In this talk, I will review the basic physics about Lyman-alpha line and recent works on galaxy formation which used the line. Finally I will also talk about my research plan using the Lyman-alpha line from the gas in young galaxies around bright QSOs at z~3 to study the importance of gas in galaxy formation.