Present status of large-scale cryogenic gravitational wave telescope

被引：45

作者：

Uchiyama, T ^{[1
]}

Kuroda, K

Ohashi, M

Miyoki, S

Ishitsuka, H

Yamamoto, K

Hayakawa, H

Kasahara, K

Fujimoto, MK

Kawamura, S

Takahashi, R

Yamazaki, T

Arai, K

Tatsumi, D

Ueda, A

Fukushima, M

Sato, S

Tsunesada, Y

Zhu, ZH

Shintomi, T

Yamamoto, A

Suzuki, T

Saito, Y

Haruyama, T

Sato, N

Higashi, Y

Tomaru, T

Tsubono, K

Ando, M

Numata, K

Aso, Y

Ueda, KI

Yoneda, H

Nakagawa, K

Musha, M

Mio, N

Moriwaki, S

Somiya, K

Araya, A

Takamori, A

Kanda, N

Telada, S

Tagoshi, H

Nakamura, T

Sasaki, M

Tanaka, T

Ohara, KI

Takahashi, H

Nagano, S

Miyakawa, O

机构：

[1] Univ Tokyo, ICRR, Kashiwa, Chiba 2778582, Japan

[2] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan

[3] High Energy Accelerator Res Org, Tsukuba, Ibaraki 3050801, Japan

[4] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan

[5] Univ Electrocommun, ILS, Chofu, Tokyo 1828585, Japan

[6] Univ Tokyo, Dept Adv Mat Sci, Tokyo 1138656, Japan

[7] Univ Tokyo, ERI, Tokyo 1130032, Japan

[8] Osaka City Univ, Dept Phys, Sumiyoshi Ku, Osaka 5588585, Japan

[9] NMI, Tsukuba, Ibaraki 3058563, Japan

[10] Osaka Univ, Dept Earth & Space Sci, Toyonaka, Osaka 5600043, Japan

[11] Kyoto Univ, Dept Phys, Sakyo Ku, Kyoto 6068502, Japan

[12] Kyoto Univ, YITP, Kyoto 6068502, Japan

[13] Niigata Univ, Dept Phys, Niigata 9502102, Japan

[14] Commun Res Labs, Tokyo 1848795, Japan

[15] CALTECH, Pasadena, CA 91125 USA

[16] Univ Western Australia, Dept Phys, Nedlands, WA 6009, Australia

来源：

CLASSICAL AND QUANTUM GRAVITY | 2004年 / 21卷 / 05期

关键词：

D O I：

10.1088/0264-9381/21/5/115

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The large-scale cryogenic gravitational wave telescope (LCGT) is the future project of the Japanese gravitational wave group. Two sets of 3 km arm length laser interferometric gravitational wave detectors will be built in a tunnel of Kamioka mine in Japan. LCGT will detect chirp waves from binary neutron star coalescence at 240 Mpc away with a S/N of 10. The expected number of detectable events in a year is two or three. To achieve the required sensitivity, several advanced techniques will be employed such as a low-frequency vibration-isolation system, a suspension point interferometer, cryogenic mirrors, a resonant side band extraction method, a high-power laser system and so on. We hope that the beginning of the project will be in 2005 and the observations will start in 2009.

引用

页码：S1161 / S1172

页数：12

共 29 条

[1] LIGO - THE LASER-INTERFEROMETER-GRAVITATIONAL-WAVE-OBSERVATORY [J].

ABRAMOVICI, A ;

ALTHOUSE, WE ;

DREVER, RWP ;

GURSEL, Y ;

KAWAMURA, S ;

RAAB, FJ ;

SHOEMAKER, D ;

SIEVERS, L ;

SPERO, RE ;

THORNE, KS ;

VOGT, RE ;

WEISS, R ;

WHITCOMB, SE ;

ZUCKER, ME .

SCIENCE, 1992, 256 (5055) :325-333

[2] Stable operation of a 300-m laser interferometer with sufficient sensitivity to detect gravitational-wave events within our galaxy [J].

Ando, M ;

Arai, K ;

Takahashi, R ;

Heinzel, G ;

Kawamura, S ;

Tatsumi, D ;

Kanda, N ;

Tagoshi, H ;

Araya, A ;

Asada, H ;

Aso, Y ;

Barton, MA ;

Fujimoto, MK ;

Fukushima, M ;

Futamase, T ;

Hayama, K ;

Horikoshi, G ;

Ishizuka, H ;

Kamikubota, N ;

Kawabe, K ;

Kawashima, N ;

Kobayashi, Y ;

Kojima, Y ;

Kondo, K ;

Kozai, Y ;

Kuroda, K ;

Matsuda, N ;

Mio, N ;

Miura, K ;

Miyakawa, O ;

Miyama, SM ;

Miyoki, S ;

Moriwaki, S ;

Musha, M ;

Nagano, S ;

Nakagawa, K ;

Nakamura, T ;

Nakao, K ;

Numata, K ;

Ogawa, Y ;

Ohashi, M ;

Ohishi, N ;

Okutomi, S ;

Oohara, K ;

Otsuka, S ;

Saito, Y ;

Sasaki, M ;

Sato, S ;

Sekiya, A ;

Shibata, M .

PHYSICAL REVIEW LETTERS, 2001, 86 (18) :3950-3954

[3]

[Anonymous], 1970, THERMOPHYSICAL PROPE

[4]

ASO Y, 2001, THESIS U TOKYO

[5]

DANZMANN K, 1994, 190 M PLANCK I QUAT

[6] Some considerations about future interferometric GW detectors [J].

Giazotto, A ;

Cella, G .

CLASSICAL AND QUANTUM GRAVITY, 2004, 21 (05) :S1183-S1190

[7] The coalescence rate of double neutron star systems [J].

Kalogera, V ;

Narayan, R ;

Spergel, DN ;

Taylor, JH .

ASTROPHYSICAL JOURNAL, 2001, 556 (01) :340-356

[8]

KASAHARA K, 2003, IN PRESS TEION KOGAK

[9] The probability distribution of binary pulsar coalescence rates. I. Double neutron star systems in the Galactic field [J].

Kim, C ;

Kalogera, V ;

Lorimer, DR .

ASTROPHYSICAL JOURNAL, 2003, 584 (02) :985-995

[10] Current status of large-scale cryogenic gravitational wave telescope [J].

Kuroda, K ;

Ohashi, M ;

Miyoki, S ;

Uchiyama, T ;

Ishitsuka, H ;

Yamamoto, K ;

Kasahara, K ;

Fujimoto, MK ;

Kawamura, S ;

Takahashi, R ;

Yamazaki, T ;

Arai, K ;

Tatsmui, D ;

Ueda, A ;

Fukushima, M ;

Sato, S ;

Nagano, S ;

Tsunesada, Y ;

Zhu, ZH ;

Shintomi, T ;

Yamamoto, A ;

Suzuki, T ;

Saito, Y ;

Haruyama, T ;

Sato, N ;

Higashi, Y ;

Tomaru, T ;

Tsubono, K ;

Ando, M ;

Takamori, A ;

Numata, K ;

Aso, Y ;

Ueda, KI ;

Yoneda, H ;

Nakagawa, K ;

Musha, M ;

Mio, N ;

Moriwaki, S ;

Somiya, K ;

Araya, A ;

Kanda, N ;

Telada, S ;

Tagoshi, H ;

Nakamura, T ;

Sasaki, M ;

Tanaka, T ;

Oohara, K ;

Takahashi, H ;

Miyakawa, O ;

Tobar, ME .

CLASSICAL AND QUANTUM GRAVITY, 2003, 20 (17) :S871-S884

← 1 2 3 →