Current status of Japanese detectors

Autor: D. Tatsumi, Virginio Sannibale, Masa Katsu Fujimoto, T. Haruyama, Nobuaki Sato, Alessandro Bertolini, Ryutaro Takahashi, Akito Araya, Kazuhiro Agatsuma, Kazuhiro Yamamoto, Akira Yamamoto, Koji Arai, Souichi Telada, K. Tsubono, Hideki Ishitsuka, Toshitaka Yamazaki, Shinji Miyoki, Takashi Uchiyama, Nobuyuki Kanda, N. Nakagawa, Masatake Ohashi, Norichika Awaya, T. Akutsu, Akiteru Takamori, Takayuki Tomaru, Szabolcs Marka, Mitsuhiro Fukushima, Kazuaki Kuroda, Riccardo DeSalvo, T. Suzuki, T. Shintomi, Masaki Ando
Rok vydání: 2007
Předmět:
Zdroj: Classical and Quantum Gravity. 24:S399-S403
ISSN: 1361-6382
0264-9381
DOI: 10.1088/0264-9381/24/19/s03
Popis: Current status of TAMA and CLIO detectors in Japan is reported in this article. 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 low frequency region after the last observation experiment in 2004. To reduce the seismic noises, we are installing new seismic isolation system, which is called 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 LCGT. Next data taking in the summer of 2007 is planned. 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 Kamioka underground site for 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 of 2006. Current sensitivity at room temperature is close to the target sensitivity within a factor of 4. Several observation experiments at room temperature have been done. Once the displacement noise reaches at thermal noise level of room temperature, its improvement by cooling test mass mirrors should be demonstrated.
6 pages, 5 figures, Proceedings of GWDAW-11
Databáze: OpenAIRE
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