年別アーカイブ: 2016年

Interpreting the double-ridge structure in high-frequency time-distance diagrams / Close loop correction of residual atmospheric dispersion in high-contrast imaging systems

[Speaker1]
Nagaaki Kambara, M2 , Sokendai, Mitaka (supervisor : Takashi Sekii, Tetsuya Watanabe, Masahito Kubo)

[Title]
Interpreting the double-ridge structure in high-frequency time-distance diagrams

[Speaker2]
Prashant Pathak, D3, Sokendai, Hawaii (supervisor : Prof. Hideki Takami)

[Title]
Close loop correction of residual atmospheric dispersion in high-contrast imaging systems

[Abstract]
For direct imaging of habitable exoplanets from ground-based telescopes, it is crucial to correct for all the wavefront errors. One such error comes atmospheric refraction, in this talk, I will talk about why it is important to correct for refraction to the highest degree and how it can be achieved.

Control Strategy of Vibration Isolation System in KAGRA / Chemical composition in merging galaxy NGC3256

[Speaker1]
Koki Okutomi ,SOKENDAI, D2 (Supervisor; Yoichi Aso)
[Title]
Control Strategy of Vibration Isolation System in KAGRA
[Abstract]
Laser interferometric gravitational-wave detector KAGRA has vibration isolation systems called SAS which attenuate fluctuation of mirrors from seismic disturbance. The largest type of SAS is a multi-stage pendulum consists of 9 suspended stages. We need to control the mirror with the complicated system to operate the laser interferometer. In this talk, I present a strategy how to control the SAS and measurements for a sensor/actuator unit related to the control strategy.

[Speaker2]
Tomonari Michiyama ,SOKENDAI, D1 (Supervisor; Daisuke Iono)
[Title]
Chemical composition in merging galaxy NGC3256

Asteroseismic measurement of surface-to-core rotation in a main-sequence A star, KIC11145123 / High Dispersion Spectroscope for Detecting Exoplanet Atmospheres / The Research for Orbital Evolution of Various Exoplanets from Misalignment Observation

[Speaker 1]
Yoshiki Hatta, M1, SOKENDAI (Supervisor; Takashi Sekii)
[Title]
Asteroseismic measurement of surface-to-core rotation in a main-sequence A star, KIC11145123

[Speaker 2]
Ko Hosokawa, M1, SOKENDAI (Supervisor; Takayuki Kotani)
[Title]
High Dispersion Spectroscope for Detecting Exoplanet Atmospheres

[Speaker 3]
Noriharu Watanabe, M1, SOKENDAI (Supervisor; Norio Narita)
[Title]
The Research for Orbital Evolution of Various Exoplanets from Misalignment Observation

Towards Direct Measurement of the Coating Thermal Noise using Cryogenic Optical Cavities / Metallicity determination of M dwarfs through synthetic spectral fitting in the near-infrared / Evaluation of 0.8K refrigerator for the development of photon counting detector

[Speaker 1]
Satoshi Tanioka, M1, SOKENDAI (Supervisor; Yoichi Aso)
[Title]
Towards Direct Measurement of the Coating Thermal Noise using Cryogenic Optical Cavities

[Speaker 2]
Hiroyuki Ishikawa, M1, SOKENDAI (Supervisor; Takayuki Kotani)
[Title]
Metallicity determination of M dwarfs through synthetic spectral fitting in the near-infrared
[Abstract]
Recently many exoplanet surveys targeting M dwarfs have been planned or conducted around the world. In order to discuss the parameters and population of the planets they will find, our understanding of their host stars are important. The precise parallaxes of the stars measured by Gaia or Hipparcos can be used to derive luminosities and then infer masses and radii, but not metallicities. The most common method to determine the metallicities of FGK-type stars is the synthetic spectral fitting in the optical region. However, M dwarfs have cool atmosphere which enable the formation of molecules with complex absorption bands, and so it is difficult to apply the method. Therefore, most of the studies about the metallicities of M dwarfs have been based on empirical methods so far. Thesedays, some high-resolution near-infrared spectroscopes are constructed and the synthetic spectral fitting begins to become possible in the near-infrared. It is promising method because M dwarfs is brighter and have fewer molecular lines in the near-infrared region than optical. In this presentation I introduce the paper by Onehag et al. (2012) who challenged it for the first time using CRIRES at ESO-VLT. We are planning to apply such method to later type M dwarfs by use of the data of IRD planet survey at Subaru.

[Speaker 3]
Yuta Kawamura, M1, SOKENDAI (Supervisor;Hiroshi Matsuo)
[Title]
Evaluation of 0.8K refrigerator for the development of photon counting detector