Current status of Japanese detectors

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dc.creatorTatsumi, Daisuke
dc.creatorTakahashi, Ryutaro
dc.creatorArai, Koji
dc.creatorNakagawa, Noriyasu
dc.creatorAgatsuma, Kazuhiro
dc.creatorYamazaki, Toshitaka
dc.creatorFukushima, Mitsuhiro
dc.creatorFujimoto, Masa-Katsu
dc.creatorTakamori, Akiteru
dc.creatorBertolini, Alessandro
dc.creatorSannibale, Virginio
dc.creatorDeSalvo, Riccardo
dc.creatorMarka, Szabolcs
dc.creatorAndo, Masaki
dc.creatorTsubono, Kimio
dc.creatorAkutsu, Tomomi
dc.creatorYamamoto, Kazuhiro
dc.creatorIshitsuka, Hideki
dc.creatorUchiyama, Takashi
dc.creatorMiyoki, Shinji
dc.creatorOhashi, Masatake
dc.creatorKuroda, Kazuaki
dc.creatorAwaya, Norichika
dc.creatorKanda, Nobuyuki
dc.creatorAraya, Akito
dc.creatorTelada, Souichi
dc.creatorTomaru, Takayuki
dc.creatorHaruyama, Tomiyoshi
dc.creatorYamamoto, Akira
dc.creatorSato, Nobuaki
dc.creatorSuzuki, Toshitaka
dc.creatorShintomi, Takakazu
dc.date2007-04-22
dc.date.accessioned2026-07-07T10:35:40Z
dc.date.available2026-07-07T10:35:40Z
dc.descriptionCurrent 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.
dc.description6 pages, 5 figures, Proceedings of GWDAW-11
dc.identifierhttps://arxiv.org/abs/0704.2881
dc.identifierhttp://arxiv.org/abs/0704.2881
dc.identifierClass.Quant.Grav.24:S399-S404,2007
dc.identifierdoi:10.1088/0264-9381/24/19/S03
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/179806
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleCurrent status of Japanese detectors
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