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2018-05

2018 国立天文台特別公開講座/総研大入試ガイダンス(関東会場)

 2018年5月19日(土)、国立天文台三鷹キャンパスにおいて、特別公開講演および総研大入試ガイダンスが行われました。本年も学部1年生の方から大学院生まで、総勢54名の方々にご来場いただきました。

 今年度は『国立天文台における天文学研究の最前線』テーマに、片岡章雅助教、田中賢幸准教教、大石雅寿准教授、松本晃治准教授の4名の先生方から、それぞれの分野の視点に立った興味深いご講演をいただきました。今年度は大学1年生の参加者が例年に比べ多く、大学に入ったばかりにもかかわらず、大学院へ進学することを考えている意識の高さに感心しました。講演の後の質問の時間には、一般的な天文学に関するものから非常に専門性の高いものまで、多くの質問がありました。

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2018 国立天文台特別公開講座/総研大入試ガイダンス(関西会場)

 2018年5月12日(土)、メルパルク京都で行われた国立天文台特別公開講座/総研大天文科学専攻入試ガイダンスには、14名の方々にご来場いただきました。“国立天文台における天文学研究の最前線”というテーマのもと、今西 昌俊 助教(ハワイ観測所)、松田 有一 助教(チリ観測所)、宮﨑 聡 准教授(先端技術センター)、林 左絵子 准教授(TMT推進室)の4名の講師による講演が行われました。

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bKAGRA Phase 1 From Kamioka with Love / status of the frequency dependent squeezing experiment at TAMA

[Speaker1]
Satoshi Tanioka, SOKENDAI 3rd year (D1)(Supervisor: Yoichi Aso,Ryutaro Takahashi,Tomotada Akutsu)
[Title]
bKAGRA Phase 1 From Kamioka with Love
[Abstract]
bKAGRA Phase 1 operation was held in April 28th to May 6th. I will report the overview.

[Speaker2]
zhao yuhang, SOKENDAI 3rd year (D1)(Supervisor: Matteo Leonardi,,)
[Title]
status of the frequency dependent squeezing experiment at TAMA
[Abstract]
It is expected that the second-generation gravitational wave detectors will be quantum noise limited in the whole detection frequency band. This expectation was partially confirmed by the LIGO-Virgo O1 and O2 runs. KAGRA will be the first 2.5-generation GW detector, and the quantum noise limit is expected to be even more severe than the second-generation detectors. The implement of frequency dependent squeezed(FDS) light source is one of the most promising solutions to this problem. After several years of table top experiments and proof of principle experiments, the implement of squeezing into GW detector is a mature technique. The most studied solution to realize an FDS is the coupling between a frequency independent squeezer to a Fabry-Perot cavity(usually addressed as filter cavity). One of the main parameter of this kind of experiment is the intra-cavity losses per meter of the filter cavity. One solution to mitigate this problem is to use hundred-meter scale filter cavity.

The purpose of our experiment, that is in the TAMA300 facility, is to realize FDS with a 300m long filter cavity. The filter cavity is hosted in an arm of the former TAMA300 interferometer. As of today, the filter cavity has been installed and is locked stably with a green field. The characterization work of the filter cavity is ongoing but almost finished. The assembling of the frequency independent squeezer is on going. The next step will be the characterization of the frequency independent squeezing and its injection into the filter cavity.

Dense molecular outflows from the merging LIRG NGC3256

[Speaker]
Tomonari Michiyama, SOKENDAI: D3 (Supervisor : Daisuke Iono, Kouichiro Nakanishi, Masatoshi Imanishi)
[Title]
Dense molecular outflows from the merging LIRG NGC3256

The current understanding of the stellar differential rotation / Doppler Tomographic Measurement for Orbital Precession of WASP-33b

[Speaker1]
Yoshiki Hatta, SOKENDAI: D1 (Supervisor : Takashi Sekii , Tetsuya Watanabe, Yukio Katsukawa)
[Title]
The current understanding of the stellar differential rotation

[Speaker2]
Noriharu Watanabe, SOKENDAI: D1 (Supervisor : Motohide Usuda, Norio Narita)
[Title]
Doppler Tomographic Measurement for Orbital Precession of WASP-33b

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