Paper abstract bibtex

We report results from a search for gravitational waves produced by perturbed intermediate mass black holes (IMBH) in data collected by LIGO and Virgo between 2005 and 2010. The search was sensitive to astrophysical sources that produced damped sinusoid gravitational wave signals, also known as ringdowns, with frequency 50$\leq$f_0/Hz$\leq$2000 and decay timescale 0.0001$\lesssim$\ensuremath\tau/s$\lesssim$0.1 characteristic of those produced in mergers of IMBH pairs. No significant gravitational wave candidate was detected. We report upper limits on the astrophysical coalescence rates of IMBHs with total binary mass 50$\leq$M/M_$\odot$$\leq$450 and component mass ratios of either 1:1 or 4:1. For systems with total mass 100$\leq$M/M_$\odot$$\leq$150, we report a 90% confidence upper limit on the rate of binary IMBH mergers with nonspinning and equal mass components of 6.9$\times$10\^ (?8) Mpc\^ (?3) yr\^ (?1). We also report a rate upper limit for ringdown waveforms from perturbed IMBHs, radiating 1% of their mass as gravitational waves in the fundamental, ?=m=2, oscillation mode, that is nearly three orders of magnitude more stringent than previous results.

@article{caltechauthors46579, volume = {89}, number = {10}, month = {May}, author = {J. Aasi and B. P. Abbott and R. Abbott and D. L. Abernathy and R. X. Adhikari and R. Anderson and S. B. Anderson and K. Arai and M. C. Araya and L. Austin and J. C. Barayoga and B. C. Barish 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 V. Dergachev and R. W. P. Drever and J. C. Driggers and P. Ehrens and T. Etzel and K. Gushwa and E. K. Gustafson and J. Harms and A. W. Heptonstall and K. A. Hodge and A. Ivanov and M. Jacobson and E. James and P. Kalmus and J. B. Kanner and W. Kells and P. J. King and V. Kondrashov and W. Z. Korth and D. B. Kozak and A. Lazzarini and J. Lewis and T. G. F. Li and K. Libbrecht and V. Litvine and M. Mageswaran and K. Mailand and E. Maros and D. Martynov and J. N. Marx and G. McIntyre and S. Meshkov and C. Osthelder and M. Pedraza and M. Phelps and L. R. Price and S. Privitera and E. Quintero and V. Raymond and J. G. Rollins and V. Sannibale and A. Singer and L. Singer and M. Smith and R. J. E. 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 L. Zhang and J. Zweizig and Y. Chen and S. Gossan and H. Miao and P. Moesta and K. S. Thorne and M. Vallisneri and H. Yang and D. H. Reitze and N. A. Robertson}, note = {{\copyright} 2014 American Physical Society. Received 28 March 2014; published 27 May 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 Educaci{\'o}n y Ciencia, 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, the Carnegie Trust, the Leverhulme Trust, the David and Lucille Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation.}, title = {Search for gravitational wave ringdowns from perturbed intermediate mass black holes in LIGO-Virgo data from 2005?2010}, publisher = {American Physical Society}, year = {2014}, journal = {Physical Review D}, pages = {Art. No. 102006}, url = {http://resolver.caltech.edu/CaltechAUTHORS:20140630-140920794}, abstract = {We report results from a search for gravitational waves produced by perturbed intermediate mass black holes (IMBH) in data collected by LIGO and Virgo between 2005 and 2010. The search was sensitive to astrophysical sources that produced damped sinusoid gravitational wave signals, also known as ringdowns, with frequency 50{$\leq$}f\_0/Hz{$\leq$}2000 and decay timescale 0.0001{$\lesssim$}{\ensuremath{\tau}}/s{$\lesssim$}0.1 characteristic of those produced in mergers of IMBH pairs. No significant gravitational wave candidate was detected. We report upper limits on the astrophysical coalescence rates of IMBHs with total binary mass 50{$\leq$}M/M\_{$\odot$}{$\leq$}450 and component mass ratios of either 1:1 or 4:1. For systems with total mass 100{$\leq$}M/M\_{$\odot$}{$\leq$}150, we report a 90\% confidence upper limit on the rate of binary IMBH mergers with nonspinning and equal mass components of 6.9{$\times$}10{\^{ }}(?8) Mpc{\^{ }}(?3) yr{\^{ }}(?1). We also report a rate upper limit for ringdown waveforms from perturbed IMBHs, radiating 1\% of their mass as gravitational waves in the fundamental, ?=m=2, oscillation mode, that is nearly three orders of magnitude more stringent than previous results.} }

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