「コロキウム」カテゴリーアーカイブ

Search for massive overdensities at z~2.2 with Subaru HSC / Wave-front error measurements and optical alignment of CLASP2 telescope

[Speaker1]
Yongming Liang, SOKENDAI 1st year (M1)(Supervisor: Nobunari Kashikawa (U.Tokyo),Masayuki Tanaka,Yuichi Matsuda)
[Title]
Search for massive overdensities at z~2.2 with Subaru HSC

[Speaker2]
Masaki Yoshida, SOKENDAI 4th year (D2)(Supervisor: Yoshinori Suematsu,Hirohisa Hara,Ryohko Ishikawa)
[Title]
Wave-front error measurements and optical alignment of CLASP2 telescope

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.

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

Detecting proto-BCG candidates at z~4 by using HSC-SSP / Gas inflow and outflow of star forming galaxies at redshift 1.4 as revealed by chemical evolution

[Speaker1]
Kei Ito, SOKENDAI 2nd year (M2)(Supervisor: Nobunari Kashikawa,Yuichi Matsuda,Yusei Koyama)
[Title]
Detecting proto-BCG candidates at z~4 by using HSC-SSP

[Speaker2]
Nao Fukagawa, SOKENDAI 3rd year (D1)(Supervisor: Prof. Tadayuki Kodama,,)
[Title]
Gas inflow and outflow of star forming galaxies at redshift 1.4 as revealed by chemical evolution
[Abstract]
Gas inflow and outflow are processes that control star formation history of galaxies. Using chemical evolution models, we attempt to extract information about gas inflow and outflow of star forming galaxies at redshift z~1.4. In this talk, we discuss our results.