Beating the Spin-down Limit on Gravitational Wave Emission from the Vela Pulsar
Creators
- Abadie, J.
- Abbott, B. P.
- Abbott, R.
-
Adhikari, Rana X.
- Anderson, S. B.
-
Arai, K.
- Araya, M. C.
- Ballmer, S.
- Betzwieser, J.
-
Billingsley, G.
- Black, E.
-
Blackburn, J. K.
- Bork, R.
- Boyle, M.
-
Brooks, A. F.
- Cannon, K.
- Cepeda, C.
- Chalermsongsak, T.
-
Chen, Y.
-
Coyne, D. C.
- Dannenberg, R.
- Daudert, B.
- Dergachev, V.
- DeSalvo, R.
- Drever, R. W. P.
- Driggers, J. C.
- Ehrens, P.
- Engel, R.
- Etzel, T.
- Gustafson, E. K.
- Hanna, C.
-
Harms, J.
- Heefner, J.
- Heptonstall, A. W.
- Hodge, K. A.
- Hong, T.
- Ivanov, A.
- Kalmus, P.
- Kells, W.
- Keppel, D. G.
- King, P. J.
- Kondrashov, V.
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Korth, W. Z.
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Kozak, D.
- Lazzarini, A.
- Lindquist, P. E.
- Luan, J.
- Mageswaran, M.
- Mailand, K.
- Maros, E.
- Marx, J. N.
- McIntyre, G.
- Meshkov, S.
- Mino, Y.
- Nash, T.
- Ogin, G. H.
- Osthelder, C.
-
Ott, C. D.
- Parameswaran, A.
- Patel, P.
- Pedraza, M.
- Phelps, M.
- Privitera, S.
- Sannibale, V.
- Searle, A. C.
- Seifert, F.
- Sengupta, A. S.
- Singer, A.
- Singer, L.
- Smith, M. R.
- Somiya, K.
- Stochino, A.
- Taylor, R.
- Thorne, K. S.
- Torrie, C. I.
- Turner, L.
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Vallisneri, M.
- Vass, S.
- Villar, A. E.
- Wallace, L.
- Wen, L.
- Whitcomb, S. E.
- Willems, P. A.
- Yamamoto, H.
- Yang, H.
- Yeaton-Massey, D.
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Zweizig, J.
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Zhang, L.
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Weinstein, Alan J.
-
Marandi, A.
- LIGO Scientific Collaboration
- Virgo Collaboration
Abstract
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.Attached Files
Published - Abadie2011p15732Astrophys_J.pdf
Submitted - 1104.2712.pdf
Files
1104.2712.pdf
Additional details
Identifiers
- Eprint ID
- 25270
- Resolver ID
- CaltechAUTHORS:20110909-103003031
Related works
- Describes
- https://arxiv.org/abs/1104.2712 (URL)
Funding
- NSF
- Science and Technology Facilities Council (STFC)
- Max-Planck-Society
- State of Niedersachsen/Germany
- Istituto Nazionale di Fisica Nucleare (INFN)
- Centre National de la Recherche Scientifique (CNRS)
- Australian Research Council
- Council of Scientific and Industrial Research (India)
- Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)
- Ministerio de Educaciόn y Ciencia (MEC)
- Conselleria d'Economia Hisenda i Innovaciό of the Govern de les Illes Balears
- Stichting voor Fundamenteel Onderzoek der Materie (FOM)
- Ministry of Science and Higher Education
- FOCUS Programme of Foundation for Polish Science
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- NASA
- Carnegie Trust
- Leverhulme Trust
- David and Lucile Packard Foundation
- Research Corporation
- Alfred P. Sloan Foundation
Dates
- Created
-
2011-09-09Created from EPrint's datestamp field
- Updated
-
2021-11-09Created from EPrint's last_modified field
Caltech Custom Metadata
- Caltech groups
- TAPIR , LIGO , Physics Department