Tatsumi, Daisuke and Takahashi, Ryutaro and Arai, Koji and Nakagawa, Noriyasu and Agatsuma, Kazuhiro and Yamazaki, Toshitaka and Fukushima, Mitsuhiro and Fujimoto , Masa-Katsu and Takamori, Akiteru and Bertolini, Alessandro and Sannibale, Virginio and DeSalvo, Riccardo and Márka, Szabolcs and Ando, Masaki and Tsubono, Kimio and Akutsu, Tomomi and Yamamoto, Kazuhiro and Ishitsuka, Hideki and Uchiyama, Takashi and Miyoki, Shinji and Ohashi, Masatake and Kuroda, Kazuaki and Awaya, Norichika and Kanda, Nobuyuki and Araya, Akito and Telada, Souichi and Tomaru, Takayuki and Haruyama, Tomiyoshi and Yamamoto, Akira and Sato, Nobuaki and Suzuki, Toshitaka and Shintomi, Takakazu (2007) Current status of Japanese detectors. Classical and Quantum Gravity, 24 (19). S399-S403. ISSN 0264-9381 http://resolver.caltech.edu/CaltechAUTHORS:20091116-105758604
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The current status of the TAMA and CLIO detectors in Japan is reported in this paper. These two interferometric gravitational wave detectors are being developed for the large cryogenic gravitational wave telescope (LCGT) which is a future plan for detecting gravitational wave signals at least once per year. TAMA300 is being upgraded to improve the sensitivity in a low-frequency region after the last observational experiment in 2004. To reduce the seismic noises, we are installing a new seismic isolation system, called the TAMA seismic attenuation system, for the four test masses. We confirmed stable mass locks of a cavity and improvements of length and angular fluctuations by using two SASs. We are currently optimizing the performance of the third and fourth SASs. We continue TAMA300 operation and R&D studies for the LCGT. The next data taking is planned for the summer of 2007. CLIO is a 100 m baseline length prototype detector for LCGT to investigate interferometer performance in cryogenic condition. The key features of CLIO are that it locates the Kamioka underground site for a low-seismic noise level, and adopts cryogenic Sapphire mirrors for low-thermal noise level. The first operation of the cryogenic interferometer was successfully demonstrated in February 2006. Current sensitivity at room temperature is close to the target sensitivity within a factor of 4. Several observational experiments at room temperature have been done. Once the displacement noise reaches the thermal noise level of room temperature, its improvement by cooling test mass mirrors should be demonstrated.
|Additional Information:||© 2007 IOP Publishing Ltd. Received 22 May 2007, in final form 17 June 2007. Published 19 September 2007. TAMA and CLIO projects are supported in part by a grant-in-aid for Scientific Research on Priority Areas (415) of the Ministry of Education, Culture, Sports, Science and Technology and a grant-in-aid for Scientific Research (A), no.18204021, 2006 of Japan Society for the Promotion of Science. Developments of TAMA SAS were supported by the Advanced Technology Center of the National Astronomical Observatory of Japan and the US National Science Foundation under cooperative agreement no. PHY-0107417.|
|Classification Code:||PACS number: 95.55.Ym|
|Official Citation:||Current status of Japanese detectors Daisuke Tatsumi, Ryutaro Takahashi, Koji Arai, Noriyasu Nakagawa, Kazuhiro Agatsuma, Toshitaka Yamazaki, Mitsuhiro Fukushima, Masa-Katsu Fujimoto, Akiteru Takamori, Alessandro Bertolini, Virginio Sannibale, Riccardo DeSalvo, Szabolcs Márka, Masaki Ando, Kimio Tsubono, Tomomi Akutsu, Kazuhiro Yamamoto, Hideki Ishitsuka, Takashi Uchiyama, Shinji Miyoki, Masatake Ohashi, Kazuaki Kuroda, Norichika Awaya, Nobuyuki Kanda, Akito Araya, Souichi Telada, Takayuki Tomaru, Tomiyoshi Haruyama, Akira Yamamoto, Nobuaki Sato, Toshitaka Suzuki and Takakazu Shintomi 2007 Class. Quantum Grav. 24 S399-S403 doi: 10.1088/0264-9381/24/19/S03|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||25 Nov 2009 21:50|
|Last Modified:||26 Dec 2012 11:33|
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