Stable Operation of a 300-m Laser Interferometer with Sufficient Sensitivity to Detect Gravitational-Wave Events within Our Galaxy | Zendy

Masaki Ando | Zendy; K. Arai | Zendy; Ryutaro Takahashi | Zendy; Gerhard Heinzel | Zendy; Seiji Kawamura | Zendy; Daisuke Tatsumi | Zendy; Nobuyuki Kanda | Zendy; Hideyuki Tagoshi | Zendy; Akito Araya | Zendy; Hideki Asada | Zendy; Y. Aso | Zendy; M. A. Barton | Zendy; Masa-Katsu Fujimoto | Zendy; Mitsuhiro Fukushima | Zendy; Toshifumi Futamase | Zendy; K. Hayama | Zendy; G. Horikoshi | Zendy; Hideki Ishizuka | Zendy; N. Kamikubota | Zendy; K. Kawabe | Zendy; Nobuki Kawashima | Zendy; Yoshinori Kobayashi | Zendy; Yasufumi Kojima | Zendy; Kazuhiro Kondo | Zendy; Y. Kozai | Zendy; Kazuaki Kuroda | Zendy; Namio Matsuda | Zendy; Norikatsu Mio | Zendy; Kazuyuki Miura | Zendy; O. Miyakawa | Zendy; Shoken M. Miyama | Zendy; S. Miyoki | Zendy; Shigenori Moriwaki | Zendy; Mitsuru Musha | Zendy; Shigeo Nagano | Zendy; K. Nakagawa | Zendy; Takashi Nakamura | Zendy; Kenichi Nakao | Zendy; Kenji Numata | Zendy; Yujiro Ogawa | Zendy; M. Ohashi | Zendy; N. Ohishi | Zendy; Satoshi Okutomi | Zendy; Ken-ichi Oohara | Zendy; Shigemi Otsuka | Zendy; Yoshio Saito | Zendy; Misao Sasaki | Zendy; Shuichi Sato | Zendy; Atsushi Sekiya | Zendy; Masaru Shibata | Zendy; K. Somiya | Zendy; T. Suzuki | Zendy; Akiteru Takamori | Zendy; Takahiro Tanaka | Zendy; Shinsuke Taniguchi | Zendy; S. Telada | Zendy; Kuniharu Tochikubo | Zendy; T. Tomaru | Zendy; Kimio Tsubono | Zendy; Nobuhiro TSUDA | Zendy; Takashi Uchiyama | Zendy; Akitoshi Ueda | Zendy; Ken-ichi Ueda | Zendy; Koichi Waseda | Zendy; Yuko Watanabe | Zendy; Hiromi Yakura | Zendy; Kazuhiro Yamamoto | Zendy; Toshitaka Yamazaki | Zendy

Open Access

Stable Operation of a 300-m Laser Interferometer with Sufficient Sensitivity to Detect Gravitational-Wave Events within Our Galaxy

Author(s) -

Masaki Ando,

K. Arai,

Ryutaro Takahashi,

Gerhard Heinzel,

Seiji Kawamura,

Daisuke Tatsumi,

Nobuyuki Kanda,

Hideyuki Tagoshi,

Akito Araya,

Hideki Asada,

Y. Aso,

M. A. Barton,

Masa-Katsu Fujimoto,

Mitsuhiro Fukushima,

Toshifumi Futamase,

K. Hayama,

G. Horikoshi,

Hideki Ishizuka,

N. Kamikubota,

K. Kawabe,

Nobuki Kawashima,

Yoshinori Kobayashi,

Yasufumi Kojima,

Kazuhiro Kondo,

Y. Kozai,

Kazuaki Kuroda,

Namio Matsuda,

Norikatsu Mio,

Kazuyuki Miura,

O. Miyakawa,

Shoken M. Miyama,

S. Miyoki,

Shigenori Moriwaki,

Mitsuru Musha,

Shigeo Nagano,

K. Nakagawa,

Takashi Nakamura,

Kenichi Nakao,

Kenji Numata,

Yujiro Ogawa,

M. Ohashi,

N. Ohishi,

Satoshi Okutomi,

Ken-ichi Oohara,

Shigemi Otsuka,

Yoshio Saito,

Misao Sasaki,

Shuichi Sato,

Atsushi Sekiya,

Masaru Shibata,

K. Somiya,

T. Suzuki,

Akiteru Takamori,

Takahiro Tanaka,

Shinsuke Taniguchi,

S. Telada,

Kuniharu Tochikubo,

T. Tomaru,

Kimio Tsubono,

Nobuhiro TSUDA,

Takashi Uchiyama,

Akitoshi Ueda,

Ken-ichi Ueda,

Koichi Waseda,

Yuko Watanabe,

Hiromi Yakura,

Kazuhiro Yamamoto,

Toshitaka Yamazaki

Publication year - 2001

Publication title -

physical review letters

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 3.688

H-Index - 673

eISSN - 1079-7114

pISSN - 0031-9007

DOI - 10.1103/physrevlett.86.3950

Subject(s) - physics , gravitational wave , interferometry , sensitivity (control systems) , atom interferometer , gravitational wave observatory , neutron star , galaxy , astrophysics , detector , coalescence (physics) , binary number , astronomical interferometer , optics , astronomy , arithmetic , mathematics , electronic engineering , engineering

TAMA300, an interferometric gravitational-wave detector with 300-m baseline length, has been developed and operated with sufficient sensitivity to detect gravitational-wave events within our galaxy and sufficient stability for observations; the interferometer was operated for over 10 hours stably and continuously. With a strain-equivalent noise level of h approximately 5x10(-21)/sqrt[Hz], a signal-to-noise ratio of 30 is expected for gravitational waves generated by a coalescence of 1.4M-1.4M binary neutron stars at 10 kpc distance. We evaluated the stability of the detector sensitivity with a 2-week data-taking run, collecting 160 hours of data to be analyzed in the search for gravitational waves.

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