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Upper limits on gravitational wave bursts in LIGO's second science run.
Physical Review D, 72
Art. No. 062001.
- Published Version
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We perform a search for gravitational wave bursts using data from the second science run of the LIGO detectors, using a method based on a wavelet time-frequency decomposition. This search is sensitive to bursts of duration much less than a second and with frequency content in the 100–1100 Hz range. It features significant improvements in the instrument sensitivity and in the analysis pipeline with respect to the burst search previously reported by LIGO. Improvements in the search method allow exploring weaker signals, relative to the detector noise floor, while maintaining a low false alarm rate, O(0.1) μHz. The sensitivity in terms of the root-sum-square (rss) strain amplitude lies in the range of hrss∼10^-20 - 10^-19 Hz^-1/2. No gravitational wave signals were detected in 9.98 days of analyzed data. We interpret the search result in terms of a frequentist upper limit on the rate of detectable gravitational wave bursts at the level of 0.26 events per day at 90% confidence level. We combine this limit with measurements of the detection efficiency for selected waveform morphologies in order to yield rate versus strength exclusion curves as well as to establish order-of-magnitude distance sensitivity to certain modeled astrophysical sources. Both the rate upper limit and its applicability to signal strengths improve our previously reported limits and reflect the most sensitive broad-band search for untriggered and unmodeled gravitational wave bursts to date.
|Additional Information:||© 2005 American Physical Society.
Received 7 June 2005; published 8 September 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 Educacion y Ciencia, the John Simon Guggenheim Foundation, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. This document has been assigned LIGO Laboratory document number LIGO-P040040-A-R.|
|Funding Agency||Grant Number|
|National Science Foundation||UNSPECIFIED|
|Particle Physics and Astronomy Research Council (PPARC)||UNSPECIFIED|
|State of Niedersachsen (Germany)||UNSPECIFIED|
|Australian Research Council||UNSPECIFIED|
|Natural Sciences and Engineering Research Council of Canada (NSERC)||UNSPECIFIED|
|Council of Scientific and Industrial Research of India||UNSPECIFIED|
|Department of Science and Technology of India||UNSPECIFIED|
|Ministerio de Educación y Ciencia (Spain)||UNSPECIFIED|
|John Simon Guggenheim Foundation||UNSPECIFIED|
|David and Lucile Packard Foundation||UNSPECIFIED|
|Alfred P. Sloan Foundation||UNSPECIFIED|
|Subject Keywords:||gravitational wave detectors; gravitational waves; light interferometry; time-frequency analysis; waveform analysis |
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|Other Numbering System Name||Other Numbering System ID|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited On:||05 Feb 2009 23:15|
|Last Modified:||25 Feb 2014 22:54|
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