Abadie, J. and Abbott, B. P. and Abbott, R. and Adhikari, R. and Anderson, S. B. and Arai, K. and Araya, M. C. and Ballmer, S. and Betzwieser, J. and Billingsley, G. and Black, E. and Blackburn, J. K. and Bork, R. and Boyle, M. and Brooks, A. F. and Cannon, K. and Cepeda, C. and Chalermsongsak, T. and Chen, Y. and Coyne, D. C. and Dannenberg, R. and Daudert, B. and Dergachev, V. and DeSalvo, R. and Drever, R. W. P. and Driggers, J. C. and Ehrens, P. and Engel, R. and Etzel, T. and Gustafson, E. K. and Hanna, C. and Harms, J. and Heefner, J. and Heptonstall, A. W. and Hodge, K. A. and Hong, T. and Ivanov, A. and Kalmus, P. and Kells, W. and Keppel, D. G. and King, P. J. and Kondrashov, V. and Korth, W. Z. and Kozak, D. and Lazzarini, A. and Lindquist, P. E. and Luan, J. and Mageswaran, M. and Mailand, K. and Maros, E. and Marx, J. N. and McIntyre, G. and Meshkov, S. and Mino, Y. and Nash, T. and Ogin, G. H. and Osthelder, C. and Ott, C. D. and Parameswaran, A. and Patel, P. and Pedraza, M. and Phelps, M. and Privitera, S. and Sannibale, V. and Searle, A. C. and Seifert, F. and Sengupta, A. S. and Singer, A. and Singer, L. and Smith, M. R. and Somiya, K. and Stochino, A. and Taylor, R. and Thorne, K. S. and Torrie, C. I. and Turner, L. and Vallisneri, M. and Vass, S. and Villar, A. E. and Wallace, L. and Wen, L. and Whitcomb, S. E. and Willems, P. A. and Yamamoto, H. and Yang, H. and Yeaton-Massey, D. and Zweizig, J. and Zhang, L. and Weinstein, Alan J. (2011) Beating the Spin-down Limit on Gravitational Wave Emission from the Vela Pulsar. Astrophysical Journal, 737 (2). Art. No. 93. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20110909-103003031
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We present direct upper limits on continuous gravitational wave emission from the Vela pulsar using data from the Virgo detector's second science run. These upper limits have been obtained using three independent methods that assume the gravitational wave emission follows the radio timing. Two of the methods produce frequentist upper limits for an assumed known orientation of the star's spin axis and value of the wave polarization angle of, respectively, 1.9 × 10^(–24) and 2.2 × 10^(–24), with 95% confidence. The third method, under the same hypothesis, produces a Bayesian upper limit of 2.1 × 10^(–24), with 95% degree of belief. These limits are below the indirect spin-down limit of 3.3 × 10^(–24) for the Vela pulsar, defined by the energy loss rate inferred from observed decrease in Vela's spin frequency, and correspond to a limit on the star ellipticity of ~10^(–3). Slightly less stringent results, but still well below the spin-down limit, are obtained assuming the star's spin axis inclination and the wave polarization angles are unknown.
|Additional Information:||© 2011 The American Astronomical Society. Received 2011 May 3; accepted 2011 June 11; published 2011 August 8. 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, 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 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 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.|
|Subject Keywords:||gravitational waves; pulsars: individual (PSR J0835–4510); stars: neutron|
|Classification Code:||PACS: 97.60.Gb; 04.30.-w|
|Official Citation:||Beating the Spin-down Limit on Gravitational Wave Emission from the Vela Pulsar J. Abadie et al. 2011 ApJ 737 93|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||09 Sep 2011 18:46|
|Last Modified:||23 Jul 2013 00:09|
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