K Kuroda et al 2002 Class. Quantum Grav. 19 1237 doi:10.1088/0264-9381/19/7/302
K Kuroda1, M Ohashi1, S Miyoki1, H Ishizuka1, C T Taylor1, K Yamamoto1, O Miyakawa1, M-K Fujimoto2, S Kawamura2, R Takahashi2, T Yamazaki2, K Arai2, D Tatsumi2, A Ueda2, M Fukushima2, S Sato2, T Shintomi3, A Yamamoto3, T Suzuki3, Y Saito3, T Haruyama3, N Sato3, Y Higashi3, T Uchiyama3, T Tomaru3, K Tsubono4, M Ando4, A Takamori4, K Numata4, K-I Ueda5, H Yoneda5, K Nakagawa5, M Musha5, N Mio6, S Moriwaki6, K Somiya6, A Araya7, N Kanda8, S Telada9, M Sasaki10, H Tagoshi10, T Nakamura11, T Tanaka11 and K Ohara12
Show affiliationsThe objective of the TAMA 300 interferometer was to develop advanced technologies for kilometre scale interferometers and to observe gravitational wave events in nearby galaxies. It was designed as a power-recycled Fabry–Perot–Michelson interferometer and was intended as a step towards a final interferometer in Japan.
The present successful status of TAMA is presented. TAMA forms a basis for LCGT (large-scale cryogenic gravitational wave telescope), a 3 km scale cryogenic interferometer to be built in the Kamioka mine in Japan, implementing cryogenic mirror techniques. The plan of LCGT is schematically described along with its associated R&D.
04.80.Nn Gravitational wave detectors and experiments
95.30.Sf Relativity and gravitation
98.35.-a Characteristics and properties of the Milky Way galaxy
Issue 7 (7 April 2002)
Received 1 October 2001, in final form 21 November 2001
Published 11 March 2002
K Kuroda et al 2002 Class. Quantum Grav. 19 1237
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