Phys. Rev. D
71,
082002
(2005)
[17 pages]
Observation results by the TAMA300 detector on gravitational wave bursts from stellar-core collapses
Masaki Ando et al.
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Masaki Ando1, Koji Arai2, Youichi Aso1, Peter Beyersdorf2, Kazuhiro Hayama3, Yukiyoshi Iida1, Nobuyuki Kanda4, Seiji Kawamura2, Kazuhiro Kondo5, Norikatsu Mio6, Shinji Miyoki5, Shigenori Moriwaki6, Shigeo Nagano7, Kenji Numata8, Shuichi Sato2, Kentaro Somiya6, Hideyuki Tagoshi9, Hirotaka Takahashi9,10, Ryutaro Takahashi2, Daisuke Tatsumi2, Yoshiki Tsunesada2, Zong-Hong Zhu2, Tomomi Akutsu5, Tomotada Akutsu3, Akito Araya11, Hideki Asada12, Mark A. Barton5, Youhei Fujiki10, Masa-Katsu Fujimoto2, Ryuichi Fujita9, Mitsuhiro Fukushima2, Toshifumi Futamase13, Yusaku Hamuro10, Tomiyoshi Haruyama14, Hideaki Hayakawa5, Gerhard Heinzel15, Gen’ichi Horikoshi14,†, Hideo Iguchi16, Kunihito Ioka17, Hideki Ishitsuka5, Norihiko Kamikubota14, Takaharu Kaneyama10, Yoshikazu Karasawa13, Kunihiko Kasahara5, Taketoshi Kasai12, Mayu Katsuki4, Keita Kawabe18, Mari Kawamura19, Nobuki Kawashima20, Fumiko Kawazoe21, Yasufumi Kojima22, Keiko Kokeyama21, Yoshihide Kozai2, Hideaki Kudoh19,23, Kazuaki Kuroda5, Takashi Kuwabara10, Namio Matsuda24, Kazuyuki Miura25, Osamu Miyakawa26, Shoken Miyama2, Hiromi Mizusawa10, Mitsuru Musha27, Yoshitaka Nagayama4, Ken’ichi Nakagawa27, Takashi Nakamura19, Hiroyuki Nakano4, Ken-ichi Nakao4, Yuhiko Nishi1, Yujiro Ogawa14, Masatake Ohashi5, Naoko Ohishi2, Akira Okutomi5, Ken-ichi Oohara10, Shigemi Otsuka1, Yoshio Saito14, Shihori Sakata21, Misao Sasaki28, Kouichi Sato29, Nobuaki Sato14, Youhei Sato27, Hidetsugu Seki1, Aya Sekido30, Naoki Seto31, Masaru Shibata32, Hisaaki Shinkai33, Takakazu Shintomi14, Kenji Soida1, Toshikazu Suzuki14, Akiteru Takamori11, Shuzo Takemoto19, Kohei Takeno6, Takahiro Tanaka19, Keisuke Taniguchi34, Shinsuke Taniguchi1, Toru Tanji6, C. T. Taylor5, Souichi Telada35, Kuniharu Tochikubo1, Masao Tokunari5, Takayuki Tomaru14, Kimio Tsubono1, Nobuhiro Tsuda29, Takashi Uchiyama5, Akitoshi Ueda2, Ken-ichi Ueda27, Fumihiko Usui36, Koichi Waseda2, Yuko Watanabe25, Hiromi Yakura25, Akira Yamamoto14, Kazuhiro Yamamoto5, Toshitaka Yamazaki2, Yuriko Yanagi21, Tatsuo Yoda1, Jun’ichi Yokoyama9, and Tatsuru Yoshida13
1Department of Physics, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
2National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
3Department of Astronomy, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
4Graduate School of Science, Osaka City University, Sumiyoshi-ku, Osaka 558-8585, Japan
5Institute for Cosmic Ray Research, The University of Tokyo, Kashiwa, Chiba 277-8582, Japan
6Department of Advanced Materials Science, The University of Tokyo, Kashiwa, Chiba 277-8561, Japan
7National Institute of Information and Communications Technology, Koganei, Tokyo 184-8795, Japan
8NASA Goddard Space Flight Center, Greenbelt, Maryland 20771, USA
9Graduate School of Science, Osaka University, Toyonaka, Osaka 560-0043, Japan
10Faculty of Science, Niigata University, Niigata, Niigata 950-2102, Japan
11Earthquake Research Institute, The University of Tokyo, Bunkyo-ku, Tokyo 113-0032, Japan
12Faculty of Science and Technology, Hirosaki University, Hirosaki, Aomori 036-8561, Japan
13Graduate School of Science, Tohoku University, Sendai, Miyagi 980-8578, Japan
14High Energy Accelerator Research Organization, Tsukuba, Ibaraki 305-0801, Japan
15Max-Planck-Institut fuer Gravitationsphysik, Callinstrasse 38, D-30167 Hannover, Germany
16Tokyo Institute of Technology, Meguro-ku, Tokyo 152-8551, Japan
17Physics Department, Pennsylvania State University, University Park, Pennsylvania 16802, USA
18LIGO Hanford Observatory, Richland, Washington 99352, USA
19Faculty of Science, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan
20Kinki University, Higashi-Osaka, Osaka 577-8502, Japan
21Ochanomizu University, Bunkyo-ku, Tokyo 112-8610, Japan
22Department of Physics, Hiroshima University, Higashi-Hiroshima, Hiroshima 739-8526, Japan
23Theoretical Astrophysics Group, Department of Physics, The University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan
24Tokyo Denki University, Chiyoda-ku, Tokyo 101-8457, Japan
25Department of Physics, Miyagi University of Education, Aoba Aramaki, Sendai 980-0845, Japan
26California Institute of Technology, Pasadena, California 91125, USA
27Institute for Laser Science, University of Electro-Communications, Chofugaoka, Chofu, Tokyo 182-8585, Japan
28Yukawa Institute for Theoretical Physics, Kyoto University, Sakyo-ku, Kyoto 606-8502, Japan
29Precision Engineering Division, Faculty of Engineering, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
30Waseda University, Shinjyuku-ku, Tokyo 169-8555, Japan
31Theoretical Astrophysics, California Institute of Technology, Pasadena, California 91125, USA
32Graduate School of Arts and Sciences, The University of Tokyo, Meguro-ku, Tokyo 153-8902, Japan
33RIKEN, Wako, Saitaka 351-0198, Japan
34Department of Physics, University of Illinois at Urbana-Champaign, Urbana, Illinois 61801-3080, USA
35National Institute of Advanced Industrial Science and Technology, Tsukuba, Ibaraki 305-8563, Japan
36ISAS/JAXA, Sagamihara, Kanagawa 229-8510, Japan
Received 22 January 2005; published 27 April 2005
We present data-analysis schemes and results of observations with the TAMA300 gravitational wave detector, targeting burst signals from stellar-core collapse events. In analyses for burst gravitational waves, the detection and fake-reduction schemes are different from well-investigated ones for a chirp wave analysis, because precise waveform templates are not available. We used an excess -power filter for the extraction of gravitational wave candidates, and developed two methods for the reduction of fake events caused by nonstationary noises of the detector. These analysis schemes were applied to real data from the TAMA300 interferometric gravitational wave detector. As a result, fake events were reduced by a factor of about 1000 in the best cases. In addition, in order to interpret the event candidates from an astronomical viewpoint, we performed a Monte-Carlo simulation with an assumed Galactic event distribution model and with burst waveforms obtained from numerical simulations of stellar-core collapses. We set an upper limit of 5.0×103 events/sec on the burst gravitational wave event rate in our Galaxy with a confidence level of 90%. This work shows prospects on the search for burst gravitational waves, by establishing an analysis scheme for the observation data from an interferometric gravitational wave detector.
© 2005 The American Physical Society
URL:
http://link.aps.org/doi/10.1103/PhysRevD.71.082002
DOI:
10.1103/PhysRevD.71.082002
PACS:
04.80.Nn, 07.05.Kf, 95.55.Ym, 95.85.Sz
*Email address: ando@granite.phys.s.u-tokyo.ac.jp †Deceased
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