Paper abstract bibtex

We report on an all-sky search for periodic gravitational waves in the frequency range 50?1000 Hz with the first derivative of frequency in the range ?8.9 $\times$ 10\^ (?10) Hz s\^ (?1) to zero in two years of data collected during LIGO's fifth science run. Our results employ a Hough transform technique, introducing a \ensuremathḩi\^ 2 test and analysis of coincidences between the signal levels in years 1 and 2 of observations that offers a significant improvement in the product of strain sensitivity with compute cycles per data sample compared to previously published searches. Since our search yields no surviving candidates, we present results taking the form of frequency dependent, 95% confidence upper limits on the strain amplitude h0. The most stringent upper limit from year 1 is 1.0 $\times$ 10\^ (?24) in the 158.00?158.25 Hz band. In year 2, the most stringent upper limit is 8.9 $\times$ 10\^ (?25) in the 146.50?146.75 Hz band. This improved detection pipeline, which is computationally efficient by at least two orders of magnitude better than our flagship Einstein@Home search, will be important for 'quick-look' searches in the Advanced LIGO and Virgo detector era.

@article{caltechauthors46042, volume = {31}, number = {8}, month = {April}, author = {J. Aasi and J. Abadie and B. P. Abbott and R. Abbott and M. R. Abernathy and R. X. Adhikari and P. Ajith and R. A. Anderson and S. B. Anderson and K. Arai and M. C. Araya and L. Austin and J. C. Barayoga and G. Billingsley 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 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 Y. Chen and S. Gossan and T. Hong and K. Kaufman and J. Luan and H. Miao and C. D. Ott and K. S. Thorne and M. Vallisneri and H. Yang and R. W. P. Drever}, note = {{\copyright} 2014 Institute of Physics. Received 28 November 2013, revised 18 February 2014. Accepted for publication 7 March 2014. Published 3 April 2014. 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? 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, 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 number LIGO-P1300071.}, title = {Application of a Hough search for continuous gravitational waves on data from the fifth LIGO science run}, publisher = {Institute of Physics}, year = {2014}, journal = {Classical and Quantum Gravity}, pages = {Art. No. 085014}, keywords = {gravitational waves, LIGO, neutron stars}, url = {http://resolver.caltech.edu/CaltechAUTHORS:20140603-092556549}, abstract = {We report on an all-sky search for periodic gravitational waves in the frequency range 50?1000 Hz with the first derivative of frequency in the range ?8.9 {$\times$} 10{\^{ }}(?10) Hz s{\^{ }}(?1) to zero in two years of data collected during LIGO's fifth science run. Our results employ a Hough transform technique, introducing a {\ensuremath{\chi}}{\^{ }}2 test and analysis of coincidences between the signal levels in years 1 and 2 of observations that offers a significant improvement in the product of strain sensitivity with compute cycles per data sample compared to previously published searches. Since our search yields no surviving candidates, we present results taking the form of frequency dependent, 95\% confidence upper limits on the strain amplitude h0. The most stringent upper limit from year 1 is 1.0 {$\times$} 10{\^{ }}(?24) in the 158.00?158.25 Hz band. In year 2, the most stringent upper limit is 8.9 {$\times$} 10{\^{ }}(?25) in the 146.50?146.75 Hz band. This improved detection pipeline, which is computationally efficient by at least two orders of magnitude better than our flagship Einstein@Home search, will be important for 'quick-look' searches in the Advanced LIGO and Virgo detector era.} }

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