「コロキウム」カテゴリーアーカイブ

The environmental impacts on the mass-metallicity relation at z=1.52: Final report & Future works/Combining SCExAO and IRD to characterize exoplanets

[Speaker 1]
Shigeru Namiki,
SOKENDAI 2nd year (M2)
(Supervisor: Yusei Koyama,Masato Onodera,Masayuki Tanaka)

[Title 1]
The environmental impacts on the mass-metallicity relation at z=1.52: Final report & Future works

[Speaker 2]
Ananya Sahoo,
SOKENDAI 3rd year (D1)
(Supervisor: Yosuke Minowa,Takayuki Kotani,Naruhisa Takato)

[Title 2]
Combining SCExAO and IRD to characterize exoplanets

Tensile Strength of Porous Dust Aggregates/Review of High-Resolution Near-IR Spectroscopy of M-dwarfs with CARMENES

[Speaker 1]
Misako Tatsuuma,
University of Tokyo D1
(Supervisor: Eiichiro Kokubo)

[Title 1]
Tensile Strength of Porous Dust Aggregates

[Speaker 2]
Hiroyuki Tako ISHIKAWA,
SOKENDAI 3rd year (D1)
(Supervisor: Tomonori Usuda,Saeko Hayashi,Takayuki Kotani)

[Title 2]
Review of High-Resolution Near-IR Spectroscopy of M-dwarfs with CARMENES

[Abstract 2]
I am now attempting to establish the abundance analysis of late-M dwarfs by using Subaru-IRD data. In Europe, the CARMENES group also performs the high-resolution near-infrared spectroscopy on M dwarfs in search of exoplanets. In this talk, I will review the papers written by the CARMENES group, especially those related to the stellar characterization (mainly, V. M. Passegger et al. 2018, A&A).
Please note that the presenter information posted here is not necessarily listed in order of presentation.

M87 Jets Investigations with East Asian VLBI Network (EAVN)

[Speaker1]
Yuzhu, Cui, SOKENDAI 3rd year (D1)(Supervisor: Mareki, HONMA,Kazuhiro, HADA,Hiroshi, NAGAI)

[Title]
M87 Jets Investigations with East Asian VLBI Network (EAVN)

[Abstract]
The radio galaxy M87 offers an privileged opportunity to probe the jet launching and formation scales thanks to the proximity and large mass of the central black hole. This makes M87 a prime target for the Event Horizon Telescope (EHT) along with SgrA*. In April 2017, M87 was for the first time observed by EHT+ALMA. This may allow the first imaging of the black hole shadow and jet-launching regions at scales of a few Schwarzschild radii. However, due to the sparse uv-coverage of the EHT, a proper interpretation of the EHT image (emission features surrounding the shadow) may require contemporaneous complementary observations at the lower frequencies that provides the higher fidelity jet images. Here we will report partial results from detailed EAVN 22/43GHz monitoring observations of M87 that were performed from January to May 2017 (so-called the “EAVN campaign 2017”), covering well the EHT-2017 observing window. We obtained data for a total of >15 epochs, and for each session 7-15 telescopes joined from East Asia, boosting the sensitivity and imaging capability compared to KaVA. These data will uniquely monitor the detailed structural evolution of the jet, velocity fields and possible component ejections near in time to the EHT period.

Disk Structures around the Class I Protostar L1489 IRS Revealed by ALMA / Dynamics of jets/outflows from high-mass young stellar objects revealed by KaVA and ALMA observations

[Speaker1]
SAI Jinshi, D1 at the University of Tokyo(Supervisor: OHASHI Nagayoshi,,)

[Title]
Disk Structures around the Class I Protostar L1489 IRS Revealed by ALMA

[Abstract ]
We observed a Class I protostar, L1489 IRS with ALMA at high spatial resolutions of ~0.3” in ALMA Band 6 (230 GHz). Our new observations in C18O 2-1 emission allowed us to confirm that the Keplerian disk extends to ~600 au in radius. We also found a gap structure at a radius ~200-300 au on a disk in C18O 2-1, and that the gas disk of L1489 IRS consists of two disks, an inner disk extending to ~200 au and an outer disk extending to ~300-600 au in radius. Furthermore, it was found that the inner disk and outer disk are misaligned by ~15 deg by comparison between observations and a kinematic model of a Keplerian disk. This misaligned disk system suggests that the axis of angular momentum of an accretion changes its direction during the star and circumstellar disk formation process. 1.3 mm dust continuum extends to ~ 370 au continuously however a gap structure is seen in C18O. It infers that the gap in C18O is due to CO depletion but the origin of the C18O gas gap is still on debated.

[Speaker2]
Jungha Kim, SOKENDAI 4th year (D2)(Supervisor: Mareki Honma,Tomoya Hirota,Katsunori Shibata)
[Title]
Dynamics of jets/outflows from high-mass young stellar objects revealed by KaVA and ALMA observations