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P. and Waldman, S. J. and Wallace, L. and Ward, R. L. and Weidner, A. and Weinert, M. and Weinstein, A. J. 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. (2009) Search for gravitational wave ringdowns from perturbed black holes in LIGO S4 data. Physical Review D, 80 (6). Art. No.062001. ISSN 0556-2821 http://resolver.caltech.edu/CaltechAUTHORS:20091023-111958820
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According to general relativity a perturbed black hole will settle to a stationary configuration by the emission of gravitational radiation. Such a perturbation will occur, for example, in the coalescence of a black hole binary, following their inspiral and subsequent merger. At late times the waveform is a superposition of quasinormal modes, which we refer to as the ringdown. The dominant mode is expected to be the fundamental mode, l = m = 2. Since this is a well-known waveform, matched filtering can be implemented to search for this signal using LIGO data. We present a search for gravitational waves from black hole ringdowns in the fourth LIGO science run S4, during which LIGO was sensitive to the dominant mode of perturbed black holes with masses in the range of 10M_☉ to 500M_☉, the regime of intermediate-mass black holes, to distances up to 300 Mpc. We present a search for gravitational waves from black hole ringdowns using data from S4. No gravitational wave candidates were found; we place a 90%-confidence upper limit on the rate of ringdowns from black holes with mass between 85M_☉ and 390M_☉ in the local universe, assuming a uniform distribution of sources, of 3:2 X 10^(-5) yr^(-1) Mpc^(-3)= 1:6 X 10^(-3) yr^(-1)L_10-^1 L_(10) ; where L_(10) is 10^(10) times the solar blue-light luminosity.
|Additional Information:||© 2009 The American Physical Society. Received 22 June 2009; published 9 September 2009. 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 Educaciόn y Ciencia, the Conselleria d’Economia, Hisenda i Innovaciό 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. This paper was assigned LIGO document number LIGO-P080093.|
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|Classification Code:||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:||26 Oct 2009 21:02|
|Last Modified:||26 Dec 2012 11:30|
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