Paper abstract bibtex

We present the results of a directed search for continuous gravitational waves from unknown, isolated neutron stars in the Galactic center region, performed on two years of data from LIGO?s fifth science run from two LIGO detectors. The search uses a semicoherent approach, analyzing coherently 630 segments, each spanning 11.5 hours, and then incoherently combining the results of the single segments. It covers gravitational wave frequencies in a range from 78 to 496 Hz and a frequency-dependent range of first-order spindown values down to ?7.86$\times$10\^ (?8) Hz/s at the highest frequency. No gravitational waves were detected. The 90% confidence upper limits on the gravitational wave amplitude of sources at the Galactic center are $\sim$3.35$\times$10\^ (?25) for frequencies near 150 Hz. These upper limits are the most constraining to date for a large-parameter-space search for continuous gravitational wave signals.

@article{caltechauthors43510, volume = {88}, number = {10}, month = {November}, author = {J. Aasi and J. Abadie and R. Abbott and M. R. Abernathy and R. X. Adhikari and R. A. Anderson and K. Arai and M. C. Araya and L. Austin and J. C. Barayoga and E. Black and J. K. Blackburn and R. Bork and A. F. Brooks and C. Cepeda and R. Chakraborty and T. Chalermsongsak and D. C. Coyne and B. Daudert and V. Dergachev and J. C. Driggers and P. Ehrens and T. Etzel and N. Fotopoulos and K. E. Gushwa and E. K. Gustafson and E. Hall and J. Harms and J. Heefner and A. W. Heptonstall and K. A. Hodge and A. Ivanov and M. Jacobson and E. James and P. Kalmus and W. Kells and P. J. King and V. Kondrashov and W. Z. Korth and D. Kozak and A. Lazzarini and J. B. Lewis and V. Litvine and D. Lloyd and M. Mageswaran and K. Mailand and E. Maros and D. Martynov and J. N. Marx and G. McIntyre and S. Meshkov and T. Nash and G. H. Ogin and C. Osthelder and M. Pedraza and M. Phelps and C. Poux and L. R. Price and S. Privitera and E. Quintero and V. Raymond and D. H. Reitze and N. A. Robertson and J. G. Rollins and V. Sannibale and F. Seifert and A. Singer and L. Singer and M. R. Smith and N. D. Smith-Lefebvre and R. Taylor and M. P. Thirugnanasambandam and E. Thrane and C. I. Torrie and S. Vass and L. Wallace and A. J. Weinstein and S. E. Whitcomb and R. Williams and H. Yamamoto and D. Yeaton-Massey and L. Zhang and J. Zweizig and B. P. Abbott and S. B. Anderson and G. Billingsley and Y. Chen and S. Gossan and T. Hong and K. Kaufman and J. Luan and H. Miao and K. S. Thorne and M. Vallisneri and H. Yang and R. W. P. Drever}, note = {{\copyright} 2013 American Physical Society. Received 27 September 2013; published 18 November 2013. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory, 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, and the Italian Istituto Nazionale di Fisica Nucleare and the French Centre National de la Recherche Scientifique for the construction and operation of the Virgo detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages program of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Econom{\'i}a y Competitividad, the Conselleria d?Economia Hisenda i Innovaci{\'o} of the Govern de les Illes Balears, the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, the Polish Ministry of Science and Higher Education, the FOCUS Programme of Foundation for Polish Science, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, 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 No. LIGO-P1300037.}, title = {Directed search for continuous gravitational waves from the Galactic center}, publisher = {American Physical Society}, year = {2013}, journal = {Physical Review D}, pages = {Art. No. 102002}, url = {http://resolver.caltech.edu/CaltechAUTHORS:20140124-110416768}, abstract = {We present the results of a directed search for continuous gravitational waves from unknown, isolated neutron stars in the Galactic center region, performed on two years of data from LIGO?s fifth science run from two LIGO detectors. The search uses a semicoherent approach, analyzing coherently 630 segments, each spanning 11.5 hours, and then incoherently combining the results of the single segments. It covers gravitational wave frequencies in a range from 78 to 496 Hz and a frequency-dependent range of first-order spindown values down to ?7.86{$\times$}10{\^{ }}(?8) Hz/s at the highest frequency. No gravitational waves were detected. The 90\% confidence upper limits on the gravitational wave amplitude of sources at the Galactic center are {$\sim$}3.35{$\times$}10{\^{ }}(?25) for frequencies near 150 Hz. These upper limits are the most constraining to date for a large-parameter-space search for continuous gravitational wave signals.} }

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