Abstract
DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational wave antenna. The goal of DECIGO is to detect gravitational waves from various kinds of sources mainly between 0.1 Hz and 10 Hz and thus to open a new window of observation for gravitational wave astronomy. DECIGO will consist of three drag-free spacecraft, 1000 km apart from each other, whose relative displacements are measured by a Fabry - Perot Michelson interferometer. We plan to launch DECIGO pathfinder first to demonstrate the technologies required to realize DECIGO and, if possible, to detect gravitational waves from our galaxy or nearby galaxies.
Original language | English |
---|---|
Article number | 012006 |
Journal | Journal of Physics: Conference Series |
Volume | 122 |
DOIs | |
Publication status | Published - 2008 |
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ASJC Scopus subject areas
- Physics and Astronomy(all)
Cite this
The Japanese space gravitational wave antenna - DECIGO. / Kawamura, S.; Ando, M.; Nakamura, T.; Tsubono, K.; Tanaka, T.; Funaki, I.; Seto, N.; Numata, K.; Sato, S.; Ioka, K.; Kanda, N.; Takashima, T.; Agatsuma, K.; Akutsu, T.; Akutsu, T.; Aoyanagi, K. S.; Arai, K.; Arase, Y.; Araya, A.; Asada, H.; Aso, Y.; Chiba, T.; Ebisuzaki, T.; Enoki, M.; Eriguchi, Y.; Fujimoto, M. K.; Fujita, R.; Fukushima, Mitsuhiro; Futamase, T.; Ganzu, K.; Harada, T.; Hashimoto, T.; Hayama, K.; Hikida, W.; Himemoto, Y.; Hirabayashi, H.; Hiramatsu, T.; Hong, F. L.; Horisawa, H.; Hosokawa, M.; Ichiki, K.; Ikegami, T.; Inoue, K. T.; Ishidoshiro, K.; Ishihara, H.; Ishikawa, T.; Ishizaki, H.; Ito, H.; Itoh, Y.; Kamagasako, S.; Kawashima, N.; Kawazoe, F.; Kirihara, H.; Kishimoto, N.; Kiuchi, K.; Kobayashi, S.; Kohri, K.; Koizumi, H.; Kojima, Y.; Kokeyama, K.; Kokuyama, W.; Kotake, K.; Kozai, Y.; Kudoh, H.; Kunimori, H.; Kuninaka, H.; Kuroda, K.; Maeda, Keiichi; Matsuhara, H.; Mino, Y.; Miyakawa, O.; Miyoki, S.; Morimoto, Y.; Morioka, T.; Morisawa, T.; Moriwaki, S.; Mukohyama, S.; Musha, M.; Nagano, S.; Naito, I.; Nakagawa, N.; Nakamura, K.; Nakano, H.; Nakao, K.; Nakasuka, S.; Nakayama, Y.; Nishida, E.; Nishiyama, K.; Nishizawa, A.; Niwa, Y.; Ohashi, M.; Ohishi, N.; Ohkawa, M.; Okutomi, A.; Onozato, K.; Oohara, K.; Sago, N.; Saijo, Motoyuki; Sakagami, M.; Sakai, S. I.; Sakata, S.; Sasaki, M.; Sato, T.; Shibata, M.; Shinkai, H.; Somiya, K.; Sotani, H.; Sugiyama, N.; Suwa, Y.; Tagoshi, H.; Takahashi, K.; Takahashi, K.; Takahashi, T.; Takahashi, H.; Takahashi, R.; Takahashi, R.; Takamori, A.; Takano, T.; Taniguchi, K.; Taruya, A.; Tashiro, H.; Tokuda, M.; Tokunari, M.; Toyoshima, M.; Tsujikawa, S.; Tsunesada, Y.; Ueda, K. I.; Utashima, M.; Yamakawa, H.; Yamamoto, K.; Yamazaki, T.; Yokoyama, J.; Yoo, C. M.; Yoshida, S.; Yoshino, T.
In: Journal of Physics: Conference Series, Vol. 122, 012006, 2008.Research output: Contribution to journal › Article
}
TY - JOUR
T1 - The Japanese space gravitational wave antenna - DECIGO
AU - Kawamura, S.
AU - Ando, M.
AU - Nakamura, T.
AU - Tsubono, K.
AU - Tanaka, T.
AU - Funaki, I.
AU - Seto, N.
AU - Numata, K.
AU - Sato, S.
AU - Ioka, K.
AU - Kanda, N.
AU - Takashima, T.
AU - Agatsuma, K.
AU - Akutsu, T.
AU - Akutsu, T.
AU - Aoyanagi, K. S.
AU - Arai, K.
AU - Arase, Y.
AU - Araya, A.
AU - Asada, H.
AU - Aso, Y.
AU - Chiba, T.
AU - Ebisuzaki, T.
AU - Enoki, M.
AU - Eriguchi, Y.
AU - Fujimoto, M. K.
AU - Fujita, R.
AU - Fukushima, Mitsuhiro
AU - Futamase, T.
AU - Ganzu, K.
AU - Harada, T.
AU - Hashimoto, T.
AU - Hayama, K.
AU - Hikida, W.
AU - Himemoto, Y.
AU - Hirabayashi, H.
AU - Hiramatsu, T.
AU - Hong, F. L.
AU - Horisawa, H.
AU - Hosokawa, M.
AU - Ichiki, K.
AU - Ikegami, T.
AU - Inoue, K. T.
AU - Ishidoshiro, K.
AU - Ishihara, H.
AU - Ishikawa, T.
AU - Ishizaki, H.
AU - Ito, H.
AU - Itoh, Y.
AU - Kamagasako, S.
AU - Kawashima, N.
AU - Kawazoe, F.
AU - Kirihara, H.
AU - Kishimoto, N.
AU - Kiuchi, K.
AU - Kobayashi, S.
AU - Kohri, K.
AU - Koizumi, H.
AU - Kojima, Y.
AU - Kokeyama, K.
AU - Kokuyama, W.
AU - Kotake, K.
AU - Kozai, Y.
AU - Kudoh, H.
AU - Kunimori, H.
AU - Kuninaka, H.
AU - Kuroda, K.
AU - Maeda, Keiichi
AU - Matsuhara, H.
AU - Mino, Y.
AU - Miyakawa, O.
AU - Miyoki, S.
AU - Morimoto, Y.
AU - Morioka, T.
AU - Morisawa, T.
AU - Moriwaki, S.
AU - Mukohyama, S.
AU - Musha, M.
AU - Nagano, S.
AU - Naito, I.
AU - Nakagawa, N.
AU - Nakamura, K.
AU - Nakano, H.
AU - Nakao, K.
AU - Nakasuka, S.
AU - Nakayama, Y.
AU - Nishida, E.
AU - Nishiyama, K.
AU - Nishizawa, A.
AU - Niwa, Y.
AU - Ohashi, M.
AU - Ohishi, N.
AU - Ohkawa, M.
AU - Okutomi, A.
AU - Onozato, K.
AU - Oohara, K.
AU - Sago, N.
AU - Saijo, Motoyuki
AU - Sakagami, M.
AU - Sakai, S. I.
AU - Sakata, S.
AU - Sasaki, M.
AU - Sato, T.
AU - Shibata, M.
AU - Shinkai, H.
AU - Somiya, K.
AU - Sotani, H.
AU - Sugiyama, N.
AU - Suwa, Y.
AU - Tagoshi, H.
AU - Takahashi, K.
AU - Takahashi, K.
AU - Takahashi, T.
AU - Takahashi, H.
AU - Takahashi, R.
AU - Takahashi, R.
AU - Takamori, A.
AU - Takano, T.
AU - Taniguchi, K.
AU - Taruya, A.
AU - Tashiro, H.
AU - Tokuda, M.
AU - Tokunari, M.
AU - Toyoshima, M.
AU - Tsujikawa, S.
AU - Tsunesada, Y.
AU - Ueda, K. I.
AU - Utashima, M.
AU - Yamakawa, H.
AU - Yamamoto, K.
AU - Yamazaki, T.
AU - Yokoyama, J.
AU - Yoo, C. M.
AU - Yoshida, S.
AU - Yoshino, T.
PY - 2008
Y1 - 2008
N2 - DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational wave antenna. The goal of DECIGO is to detect gravitational waves from various kinds of sources mainly between 0.1 Hz and 10 Hz and thus to open a new window of observation for gravitational wave astronomy. DECIGO will consist of three drag-free spacecraft, 1000 km apart from each other, whose relative displacements are measured by a Fabry - Perot Michelson interferometer. We plan to launch DECIGO pathfinder first to demonstrate the technologies required to realize DECIGO and, if possible, to detect gravitational waves from our galaxy or nearby galaxies.
AB - DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) is the future Japanese space gravitational wave antenna. The goal of DECIGO is to detect gravitational waves from various kinds of sources mainly between 0.1 Hz and 10 Hz and thus to open a new window of observation for gravitational wave astronomy. DECIGO will consist of three drag-free spacecraft, 1000 km apart from each other, whose relative displacements are measured by a Fabry - Perot Michelson interferometer. We plan to launch DECIGO pathfinder first to demonstrate the technologies required to realize DECIGO and, if possible, to detect gravitational waves from our galaxy or nearby galaxies.
UR - http://www.scopus.com/inward/record.url?scp=65649117704&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=65649117704&partnerID=8YFLogxK
U2 - 10.1088/1742-6596/122/1/012006
DO - 10.1088/1742-6596/122/1/012006
M3 - Article
AN - SCOPUS:65649117704
VL - 122
JO - Journal of Physics: Conference Series
JF - Journal of Physics: Conference Series
SN - 1742-6588
M1 - 012006
ER -