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P. and Waldman, S. J. and Wallace, L. and Ward, R. L. and Weidner, A. and Weinert, M. and Weiss, R. and Wen, L. and Wen, S. and Wette, K. and Whelan, J. T. and Whitcomb, S. E. and Whiting, B. F. and Wilkinson, C. and Willems, P. A. and Williams, H. R. and Williams, L. and Willke, B. and Wilmut, I. and Winkelmann, L. and Winkler, W. and Wipf, C. C. and Wiseman, A. G. and Woan, G. and Wooley, R. and Worden, J. and Wu, W. and Yakushin, I. and Yamamoto, H. and Yan, Z. and Yoshida, S. and Zanolin, M. and Zhang, J. and Zhang, L. and Zhao, C. and Zotov, N. and Zucker, M. E. and zur-Mühlen, H. and Zweizig, J. and Weinstein, Alan J. (2009) Search for gravitational waves from low mass binary coalescences in the first year of LIGO's S5 data. Physical Review D, 79 (12). Art. 122001. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:20091007-073406265
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We have searched for gravitational waves from coalescing low mass compact binary systems with a total mass between 2M_([sun]) and 35Mz-([sun]) and a minimum component mass of 1M_([sun]) using data from the first year of the fifth science run of the three LIGO detectors, operating at design sensitivity. Depending on the mass, we are sensitive to coalescences as far as 150 Mpc from the Earth. No gravitational-wave signals were observed above the expected background. Assuming a population of compact binary objects with a Gaussian mass distribution representing binary neutron star systems, black hole–neutron star binary systems, and binary black hole systems, we calculate the 90% confidence upper limit on the rate of coalescences to be 3.9×10^(-2) yr^(-1)L_(10)^(-1), 1.1×10^(-2) yr^(-1)L_(10)^(-1), and 2.5×10^(-3)yr^(-1)L_(10)^(-1), respectively, where L_(10) is 10^(10) times the blue solar luminosity. We also set improved upper limits on the rate of compact binary coalescences per unit blue-light luminosity, as a function of mass.
|Additional Information:||©2009 The American Physical Society. Received 11 February 2009; published 5 June 2009. The authors thank Marie Anne Bizouard for her time and help in reviewing the accuracy of this research. The authors gratefully acknowledge the support of the U.S. National Science Foundation for the construction and operation of the LIGO Laboratory, and the Science and Technology Facilities 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 Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educaciόn y Ciencia, the Conselleria d’Economia, Hisenda i Innovaciό of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation.|
|Classification Code:||PACS: 95.85.Sz; 04.80.Nn; 07.05.Kf; 97.60.Jd|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||09 Oct 2009 21:30|
|Last Modified:||10 Mar 2017 22:01|
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