Paper abstract bibtex

We report on a search for gravitational waves from the coalescence of compact binaries during the third and fourth LIGO science runs. The search focused on gravitational waves generated during the inspiral phase of the binary evolution. In our analysis, we considered three categories of compact binary systems, ordered by mass: (i) primordial black hole binaries with masses in the range 0.35M_$\odot$\ensuremath

@article{caltechauthors44559, volume = {77}, number = {6}, month = {March}, author = {B. Abbott and R. W. P. Drever and D. A. Brown and P. Savov and K. S. Thorne and M. Vallisneri and R. Abbott and Rana X. Adhikari and J. Agresti and S. B. Anderson and M. Araya and H. Armandula and S. Ballmer and B. C. Barish and B. Bhawal and G. Billingsley and E. Black and K. Blackburn and R. Bork and V. Boschi and D. Busby and L. Cardenas and C. Cepeda and S. Chatterji and D. Coyne and T. D. Creighton and E. D'Ambrosio and R. De Salvo and R. J. Dupuis and P. Ehrens and E. Espinoza and T. Etzel and M. Evans and S. Fairhurst and D. Fazi and L. Goggin and J. Heefner and A. Ivanov and W. Kells and D. G. Keppel and P. King and V. Kondrashov and D. Kozak and A. Lazzarini and M. Lei and K. Libbrecht and P. Lindquist and M. Mageswaran and K. Mailand and V. Mandic and E. Maros and J. N. Marx and S. Meshkov and E. Messaritaki and D. Meyers and O. Miyakawa and T. Nash and F. Nocera and P. Patel and M. Pedraza and N. A. Robertson and P. Russell and M. Samidi and G. H. Sanders and V. Sannibale and B. Sears and M. R. Smith and P. J. Sutton and M. Tarallo and R. Taylor and W. Tyler and M. Varvella and S. Vass and A. Villar and S. J. Waldman and L. Wallace and R. Ward and D. Webber and A. J. Weinstein and S. E. Whitcomb and P. A. Willems and H. Yamamoto and L. Zhang and J. Zweizig}, note = {{\copyright} 2008 The American Physical Society. Received 26 April 2007; published 7 March 2008. The authors gratefully acknowledge the support of the United States 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 Educaci?n y Ciencia, the Conselleria d?Economia, Hisenda i Innovaci? of the Govern de les Illes Balears, 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.}, title = {Search for gravitational waves from binary inspirals in S3 and S4 LIGO data}, publisher = {American Physical Society}, year = {2008}, journal = {Physical Review D}, pages = {Art. No. 062002}, url = {http://resolver.caltech.edu/CaltechAUTHORS:20140401-081124003}, abstract = {We report on a search for gravitational waves from the coalescence of compact binaries during the third and fourth LIGO science runs. The search focused on gravitational waves generated during the inspiral phase of the binary evolution. In our analysis, we considered three categories of compact binary systems, ordered by mass: (i) primordial black hole binaries with masses in the range 0.35M\_{$\odot$}{\ensuremath{<}}m\_1, m\_2{\ensuremath{<}}1.0M\_{$\odot$}, (ii) binary neutron stars with masses in the range 1.0M\_{$\odot$}{\ensuremath{<}}m\_1, m\_2{\ensuremath{<}}3.0M\_{$\odot$}, and (iii) binary black holes with masses in the range 3.0M\_{$\odot$}{\ensuremath{<}}m\_1, m\_2{\ensuremath{<}}m\_(max) with the additional constraint m\_1+m\_2{\ensuremath{<}}m\_(max), where m\_(max) was set to 40.0M\_{$\odot$} and 80.0M\_{$\odot$} in the third and fourth science runs, respectively. Although the detectors could probe to distances as far as tens of Mpc, no gravitational-wave signals were identified in the 1364 hours of data we analyzed. Assuming a binary population with a Gaussian distribution around 0.75?0.75M\_{$\odot$}, 1.4?1.4M\_{$\odot$}, and 5.0?5.0M\_{$\odot$}, we derived 90\%-confidence upper limit rates of 4.9 yr{\^{ }}(?1)L{\^{ }}(?1)\_(10) for primordial black hole binaries, 1.2 yr{\^{ }}(?1)L{\^{ }}(?1)\_(10) for binary neutron stars, and 0.5 yr{\^{ }}(?1)L{\^{ }}(?1)\_(10) for stellar mass binary black holes, where L\_(10) is 10{\^{ }}(10) times the blue-light luminosity of the Sun.} }

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