Search for gravitational waves associated with the gamma ray burst GRB030329 using the LIGO detectors

Creators: Abbott, B.; Drever, R. W. P.; Williams, R.; Buonanno, A.; Chen, Y.; Pan, Y.; Thorne, K. S.; Vallisneri, M.; Anderson, S. B.; Araya, M.; Armandula, H.; Asiri, F.; Barish, B. C.; Barnes, M.; Barton, M. A.; Bhawal, B.; Billingsley, G.; Black, E.; Blackburn, K.; Bogue, L.; Bork, R.; Busby, D.; Cardenas, L.; Chandler, A.; Chapsky, J.; Charlton, P.; Coyne, D.; Creighton, T. D.; D'Ambrosio, E.; DeSalvo, R.; Ding, H.; Edlund, J. A.; Ehrens, P.; Etzel, T.; Evans, M.; Farnham, D.; Fine, M.; Gillespie, A.; Grimmett, D.; Hartunian, A.; Heefner, J.; Hoang, P.; Hrynevych, M.; Ivanov, A.; Jones, L.; Jungwirth, D.; Kells, W.; King, C.; King, P.; Kozak, D.; Lazzarini, A.; Lei, M.; Libbrecht, K.; Lindquist, P.; Liu, S.; Logan, J.; Lyons, T. T.; Mageswaran, M.; Mailand, K.; Majid, W.; Mann, F.; Márka, S.; Maros, E.; Mason, J.; Meshkov, S.; Miyakawa, O.; Miyoki, S.; Nash, T.; Nocera, F.; Ouimette, D.; Pedraza, M.; Rao, S. R.; Redding, D.; Regehr, M. W.; Reilly, K. T.; Reithmaier, K.; Robison, L.; Romie, J.; Rose, D.; Russell, P.; Salzman, I.; Sanders, G. H.; Sannibale, V.; Schmidt, V.; Sears, B.; Seel, S.; Shawhan, P.; Sievers, L.; Smith, M. R.; Spero, R.; Sumner, M. C.; Sutton, P. J.; Sylvestre, J.; Takamori, A.; Tariq, H.; Taylor, R.; Tilav, S.; Torrie, C.; Tyler, W.; Vass, S.; Wallace, L.; Ware, B.; Webber, D.; Weinstein, A. J.; Wen, L.; Whitcomb, S. E.; Willems, P. A.; Wilson, A.; Yamamoto, H.; Zhang, L.; Zweizig, J.; LIGO Scientific Collaboration

Abstract

We have performed a search for bursts of gravitational waves associated with the very bright gamma ray burst GRB030329, using the two detectors at the LIGO Hanford Observatory. Our search covered the most sensitive frequency range of the LIGO detectors (approximately 80–−2048 Hz), and we specifically targeted signals shorter than ≃150 ms. Our search algorithm looks for excess correlated power between the two interferometers and thus makes minimal assumptions about the gravitational waveform. We observed no candidates with gravitational-wave signal strength larger than a predetermined threshold. We report frequency-dependent upper limits on the strength of the gravitational waves associated with GRB030329. Near the most sensitive frequency region, around ≃250 Hz, our root-sum-square (RSS) gravitational-wave strain sensitivity for optimally polarized bursts was better than h_(RSS)≃6×10^(−21) Hz^(−1/2). Our result is comparable to the best published results searching for association between gravitational waves and gamma ray bursts.

Additional Information

© 2005 The American Physical Society. Received 21 February 2005; published 12 August 2005. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Particle Physics and Astronomy Research Council of the United Kingdom, the Max-Planck-Society and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Natural Sciences and Engineering Research Council of Canada, the Council of Scientific and Industrial Research of India, the Department of Science and Technology of India, the Spanish Ministerio de Ciencia y Tecnologia, the John Simon Guggenheim Foundation, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. We are grateful to Scott Barthelmy and the GCN network and Kevin Hurley and the IPN network for providing us with near real time GRB triggers and to the Ulysses, Konus, SAX, and HETE experiments, who detect and generate the events distributed by GCN and IPN. This research has made use of data obtained from the HETE science team via the website in Ref. [75]. HETE is an international mission of the NASA Explorer program, run by the Massachusetts Institute of Technology.

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