BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR
Identifieur interne : 004519 ( PascalFrancis/Curation ); précédent : 004518; suivant : 004520BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR
Auteurs : J. Abadie [États-Unis] ; B. P. Abbott [États-Unis] ; R. Abbott [États-Unis] ; M. Abernathy [Royaume-Uni] ; T. Accadia [France] ; F. Acernese [Italie] ; C. Adams [États-Unis] ; R. Adhikari [États-Unis] ; C. Affeldt [Allemagne] ; B. Allen [Allemagne, États-Unis] ; G. S. Allen [États-Unis] ; E. Amador Ceron [États-Unis] ; D. Amariutei [États-Unis] ; R. S. Amin [États-Unis] ; S. B. Anderson [États-Unis] ; W. G. Anderson [États-Unis] ; F. Antonucci [Italie] ; K. Arai [États-Unis] ; M. A. Arain [États-Unis] ; M. C. Araya [États-Unis] ; S. M. Aston [Royaume-Uni] ; P. Astone [Italie] ; D. Atkinson [États-Unis] ; P. Aufmuth [Allemagne] ; C. Aulbert [Allemagne] ; B. E. Aylott [Royaume-Uni] ; S. Babak [Allemagne] ; P. Baker [États-Unis] ; G. Ballardin [Italie] ; S. Ballmer [États-Unis] ; D. Barker [États-Unis] ; S. Barnum [États-Unis] ; F. Barone [Italie] ; B. Barr [Royaume-Uni] ; P. Barriga [Australie] ; L. Barsotti [États-Unis] ; M. Barsuglia [France] ; M. A. Barton [États-Unis] ; I. Bartos [États-Unis] ; R. Bassiri [Royaume-Uni] ; M. Bastarrika [Royaume-Uni] ; A. Basti [Italie] ; J. Bauchrowitz [Allemagne] ; Th. S. Bauer ; B. Behnke [Allemagne] ; M. Bejger ; M. G. Beker ; A. S. Bell [Royaume-Uni] ; A. Belletoile [France] ; I. Belopolski [États-Unis] ; M. Benacquista ; A. Bertolini [Allemagne] ; J. Betzwieser [États-Unis] ; N. Beveridge [Royaume-Uni] ; P. T. Beyersdorf ; I. A. Bilenko ; G. Billingsley [États-Unis] ; J. Birch [États-Unis] ; S. Birindelli ; R. BiswasSource :
- The Astrophysical journal [ 0004-637X ] ; 2011.
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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 x 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 x 10-24, with 95% degree of belief. These limits are below the indirect spin-down limit of 3.3 x 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.
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<author><name sortKey="Barriga, P" sort="Barriga, P" uniqKey="Barriga P" first="P." last="Barriga">P. Barriga</name>
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<author><name sortKey="Barsotti, L" sort="Barsotti, L" uniqKey="Barsotti L" first="L." last="Barsotti">L. Barsotti</name>
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<author><name sortKey="Bauchrowitz, J" sort="Bauchrowitz, J" uniqKey="Bauchrowitz J" first="J." last="Bauchrowitz">J. Bauchrowitz</name>
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<author><name sortKey="Bauer, Th S" sort="Bauer, Th S" uniqKey="Bauer T" first="Th. S." last="Bauer">Th. S. Bauer</name>
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<author><name sortKey="Behnke, B" sort="Behnke, B" uniqKey="Behnke B" first="B." last="Behnke">B. Behnke</name>
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<affiliation wicri:level="1"><inist:fA14 i1="23"><s1>Columbia University</s1>
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<author><name sortKey="Bertolini, A" sort="Bertolini, A" uniqKey="Bertolini A" first="A." last="Bertolini">A. Bertolini</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
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<author><name sortKey="Beveridge, N" sort="Beveridge, N" uniqKey="Beveridge N" first="N." last="Beveridge">N. Beveridge</name>
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</author>
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</author>
<author><name sortKey="Birch, J" sort="Birch, J" uniqKey="Birch J" first="J." last="Birch">J. Birch</name>
<affiliation wicri:level="1"><inist:fA14 i1="06"><s1>LIGO-Livingston Observatory</s1>
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<author><name sortKey="Birindelli, S" sort="Birindelli, S" uniqKey="Birindelli S" first="S." last="Birindelli">S. Birindelli</name>
</author>
<author><name sortKey="Biswas, R" sort="Biswas, R" uniqKey="Biswas R" first="R." last="Biswas">R. Biswas</name>
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</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">11-0379596</idno>
<date when="2011">2011</date>
<idno type="stanalyst">PASCAL 11-0379596 INIST</idno>
<idno type="RBID">Pascal:11-0379596</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">001A25</idno>
<idno type="wicri:Area/PascalFrancis/Curation">004519</idno>
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<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR</title>
<author><name sortKey="Abadie, J" sort="Abadie, J" uniqKey="Abadie J" first="J." last="Abadie">J. Abadie</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
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</affiliation>
</author>
<author><name sortKey="Abbott, B P" sort="Abbott, B P" uniqKey="Abbott B" first="B. P." last="Abbott">B. P. Abbott</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
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</author>
<author><name sortKey="Abbott, R" sort="Abbott, R" uniqKey="Abbott R" first="R." last="Abbott">R. Abbott</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
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</author>
<author><name sortKey="Abernathy, M" sort="Abernathy, M" uniqKey="Abernathy M" first="M." last="Abernathy">M. Abernathy</name>
<affiliation wicri:level="1"><inist:fA14 i1="02"><s1>University of Glasgow</s1>
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</author>
<author><name sortKey="Accadia, T" sort="Accadia, T" uniqKey="Accadia T" first="T." last="Accadia">T. Accadia</name>
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</author>
<author><name sortKey="Acernese, F" sort="Acernese, F" uniqKey="Acernese F" first="F." last="Acernese">F. Acernese</name>
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<author><name sortKey="Affeldt, C" sort="Affeldt, C" uniqKey="Affeldt C" first="C." last="Affeldt">C. Affeldt</name>
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<author><name sortKey="Allen, B" sort="Allen, B" uniqKey="Allen B" first="B." last="Allen">B. Allen</name>
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<s2>30167 Hannover</s2>
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</inist:fA14>
<country>Allemagne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Leibniz Universität Hannover</s1>
<s2>30167 Hannover</s2>
<s3>DEU</s3>
<sZ>9 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>25 aut.</sZ>
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<sZ>52 aut.</sZ>
</inist:fA14>
<country>Allemagne</country>
</affiliation>
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<s3>USA</s3>
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</affiliation>
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<author><name sortKey="Allen, G S" sort="Allen, G S" uniqKey="Allen G" first="G. S." last="Allen">G. S. Allen</name>
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<s3>USA</s3>
<sZ>11 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
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<s2>Milwaukee, WI 53201</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>16 aut.</sZ>
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<country>États-Unis</country>
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</author>
<author><name sortKey="Amariutei, D" sort="Amariutei, D" uniqKey="Amariutei D" first="D." last="Amariutei">D. Amariutei</name>
<affiliation wicri:level="1"><inist:fA14 i1="11"><s1>University of Florida</s1>
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<s3>USA</s3>
<sZ>13 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
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<affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Louisiana State University</s1>
<s2>Baton Rouge, LA 70803</s2>
<s3>USA</s3>
<sZ>14 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
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<author><name sortKey="Anderson, S B" sort="Anderson, S B" uniqKey="Anderson S" first="S. B." last="Anderson">S. B. Anderson</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
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<s3>USA</s3>
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<sZ>53 aut.</sZ>
<sZ>57 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Anderson, W G" sort="Anderson, W G" uniqKey="Anderson W" first="W. G." last="Anderson">W. G. Anderson</name>
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<s2>Milwaukee, WI 53201</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>16 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Antonucci, F" sort="Antonucci, F" uniqKey="Antonucci F" first="F." last="Antonucci">F. Antonucci</name>
<affiliation wicri:level="1"><inist:fA14 i1="13"><s1>INFN, Sezione di Roma</s1>
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<s3>ITA</s3>
<sZ>17 aut.</sZ>
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</inist:fA14>
<country>Italie</country>
</affiliation>
</author>
<author><name sortKey="Arai, K" sort="Arai, K" uniqKey="Arai K" first="K." last="Arai">K. Arai</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
<s2>Pasadena, CA 91125</s2>
<s3>USA</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
<sZ>3 aut.</sZ>
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</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Arain, M A" sort="Arain, M A" uniqKey="Arain M" first="M. A." last="Arain">M. A. Arain</name>
<affiliation wicri:level="1"><inist:fA14 i1="11"><s1>University of Florida</s1>
<s2>Gainesville, FL 32611</s2>
<s3>USA</s3>
<sZ>13 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
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<author><name sortKey="Araya, M C" sort="Araya, M C" uniqKey="Araya M" first="M. C." last="Araya">M. C. Araya</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
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<s3>USA</s3>
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<country>États-Unis</country>
</affiliation>
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<author><name sortKey="Aston, S M" sort="Aston, S M" uniqKey="Aston S" first="S. M." last="Aston">S. M. Aston</name>
<affiliation wicri:level="1"><inist:fA14 i1="14"><s1>University of Birmingham</s1>
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<sZ>21 aut.</sZ>
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</inist:fA14>
<country>Royaume-Uni</country>
</affiliation>
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<author><name sortKey="Astone, P" sort="Astone, P" uniqKey="Astone P" first="P." last="Astone">P. Astone</name>
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<country>Italie</country>
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<author><name sortKey="Atkinson, D" sort="Atkinson, D" uniqKey="Atkinson D" first="D." last="Atkinson">D. Atkinson</name>
<affiliation wicri:level="1"><inist:fA14 i1="15"><s1>LIGO-Hanford Observatory</s1>
<s2>Richland, WA 99352</s2>
<s3>USA</s3>
<sZ>23 aut.</sZ>
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<sZ>38 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Aufmuth, P" sort="Aufmuth, P" uniqKey="Aufmuth P" first="P." last="Aufmuth">P. Aufmuth</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
<s2>30167 Hannover</s2>
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</inist:fA14>
<country>Allemagne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Leibniz Universität Hannover</s1>
<s2>30167 Hannover</s2>
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<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>25 aut.</sZ>
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<country>Allemagne</country>
</affiliation>
</author>
<author><name sortKey="Aulbert, C" sort="Aulbert, C" uniqKey="Aulbert C" first="C." last="Aulbert">C. Aulbert</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
<s2>30167 Hannover</s2>
<s3>DEU</s3>
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<country>Allemagne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Leibniz Universität Hannover</s1>
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<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>25 aut.</sZ>
<sZ>43 aut.</sZ>
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<country>Allemagne</country>
</affiliation>
</author>
<author><name sortKey="Aylott, B E" sort="Aylott, B E" uniqKey="Aylott B" first="B. E." last="Aylott">B. E. Aylott</name>
<affiliation wicri:level="1"><inist:fA14 i1="14"><s1>University of Birmingham</s1>
<s2>Birmingham B15 2TT</s2>
<s3>GBR</s3>
<sZ>21 aut.</sZ>
<sZ>26 aut.</sZ>
</inist:fA14>
<country>Royaume-Uni</country>
</affiliation>
</author>
<author><name sortKey="Babak, S" sort="Babak, S" uniqKey="Babak S" first="S." last="Babak">S. Babak</name>
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<s2>14476 Golm</s2>
<s3>DEU</s3>
<sZ>27 aut.</sZ>
<sZ>45 aut.</sZ>
</inist:fA14>
<country>Allemagne</country>
</affiliation>
</author>
<author><name sortKey="Baker, P" sort="Baker, P" uniqKey="Baker P" first="P." last="Baker">P. Baker</name>
<affiliation wicri:level="1"><inist:fA14 i1="17"><s1>Montana State University</s1>
<s2>Bozeman, MT 59717</s2>
<s3>USA</s3>
<sZ>28 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Ballardin, G" sort="Ballardin, G" uniqKey="Ballardin G" first="G." last="Ballardin">G. Ballardin</name>
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<s3>ITA</s3>
<sZ>29 aut.</sZ>
</inist:fA14>
<country>Italie</country>
</affiliation>
</author>
<author><name sortKey="Ballmer, S" sort="Ballmer, S" uniqKey="Ballmer S" first="S." last="Ballmer">S. Ballmer</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>LIGO-California Institute of Technology</s1>
<s2>Pasadena, CA 91125</s2>
<s3>USA</s3>
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<sZ>3 aut.</sZ>
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<sZ>20 aut.</sZ>
<sZ>30 aut.</sZ>
<sZ>53 aut.</sZ>
<sZ>57 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Barker, D" sort="Barker, D" uniqKey="Barker D" first="D." last="Barker">D. Barker</name>
<affiliation wicri:level="1"><inist:fA14 i1="15"><s1>LIGO-Hanford Observatory</s1>
<s2>Richland, WA 99352</s2>
<s3>USA</s3>
<sZ>23 aut.</sZ>
<sZ>31 aut.</sZ>
<sZ>38 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
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<author><name sortKey="Barnum, S" sort="Barnum, S" uniqKey="Barnum S" first="S." last="Barnum">S. Barnum</name>
<affiliation wicri:level="1"><inist:fA14 i1="19"><s1>Carleton College</s1>
<s2>Northfield, MN 55057</s2>
<s3>USA</s3>
<sZ>32 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Barone, F" sort="Barone, F" uniqKey="Barone F" first="F." last="Barone">F. Barone</name>
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<s2>80126 Napoli</s2>
<s3>ITA</s3>
<sZ>6 aut.</sZ>
<sZ>33 aut.</sZ>
</inist:fA14>
<country>Italie</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="05"><s1>Università di Salerno, Fisciano</s1>
<s2>84084 Salerno</s2>
<s3>ITA</s3>
<sZ>6 aut.</sZ>
<sZ>33 aut.</sZ>
</inist:fA14>
<country>Italie</country>
</affiliation>
</author>
<author><name sortKey="Barr, B" sort="Barr, B" uniqKey="Barr B" first="B." last="Barr">B. Barr</name>
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<sZ>40 aut.</sZ>
<sZ>41 aut.</sZ>
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<country>Royaume-Uni</country>
</affiliation>
</author>
<author><name sortKey="Barriga, P" sort="Barriga, P" uniqKey="Barriga P" first="P." last="Barriga">P. Barriga</name>
<affiliation wicri:level="1"><inist:fA14 i1="20"><s1>University of Western Australia</s1>
<s2>Crawley, WA 6009</s2>
<s3>AUS</s3>
<sZ>35 aut.</sZ>
</inist:fA14>
<country>Australie</country>
</affiliation>
</author>
<author><name sortKey="Barsotti, L" sort="Barsotti, L" uniqKey="Barsotti L" first="L." last="Barsotti">L. Barsotti</name>
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<s3>USA</s3>
<sZ>36 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Barsuglia, M" sort="Barsuglia, M" uniqKey="Barsuglia M" first="M." last="Barsuglia">M. Barsuglia</name>
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<s2>75013 Paris</s2>
<s3>FRA</s3>
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</inist:fA14>
<country>France</country>
</affiliation>
</author>
<author><name sortKey="Barton, M A" sort="Barton, M A" uniqKey="Barton M" first="M. A." last="Barton">M. A. Barton</name>
<affiliation wicri:level="1"><inist:fA14 i1="15"><s1>LIGO-Hanford Observatory</s1>
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<s3>USA</s3>
<sZ>23 aut.</sZ>
<sZ>31 aut.</sZ>
<sZ>38 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Bartos, I" sort="Bartos, I" uniqKey="Bartos I" first="I." last="Bartos">I. Bartos</name>
<affiliation wicri:level="1"><inist:fA14 i1="23"><s1>Columbia University</s1>
<s2>New York, NY 10027</s2>
<s3>USA</s3>
<sZ>39 aut.</sZ>
<sZ>50 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
</affiliation>
</author>
<author><name sortKey="Bassiri, R" sort="Bassiri, R" uniqKey="Bassiri R" first="R." last="Bassiri">R. Bassiri</name>
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<sZ>34 aut.</sZ>
<sZ>40 aut.</sZ>
<sZ>41 aut.</sZ>
<sZ>48 aut.</sZ>
<sZ>54 aut.</sZ>
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</affiliation>
</author>
<author><name sortKey="Bastarrika, M" sort="Bastarrika, M" uniqKey="Bastarrika M" first="M." last="Bastarrika">M. Bastarrika</name>
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<sZ>4 aut.</sZ>
<sZ>34 aut.</sZ>
<sZ>40 aut.</sZ>
<sZ>41 aut.</sZ>
<sZ>48 aut.</sZ>
<sZ>54 aut.</sZ>
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<country>Royaume-Uni</country>
</affiliation>
</author>
<author><name sortKey="Basti, A" sort="Basti, A" uniqKey="Basti A" first="A." last="Basti">A. Basti</name>
<affiliation wicri:level="1"><inist:fA14 i1="24"><s1>INFN, Sezione di Pisa</s1>
<s2>56127 Pisa</s2>
<s3>ITA</s3>
<sZ>42 aut.</sZ>
</inist:fA14>
<country>Italie</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="25"><s1>Università di Pisa</s1>
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<s3>ITA</s3>
<sZ>42 aut.</sZ>
</inist:fA14>
<country>Italie</country>
</affiliation>
</author>
<author><name sortKey="Bauchrowitz, J" sort="Bauchrowitz, J" uniqKey="Bauchrowitz J" first="J." last="Bauchrowitz">J. Bauchrowitz</name>
<affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
<s2>30167 Hannover</s2>
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<sZ>9 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>25 aut.</sZ>
<sZ>43 aut.</sZ>
<sZ>52 aut.</sZ>
</inist:fA14>
<country>Allemagne</country>
</affiliation>
<affiliation wicri:level="1"><inist:fA14 i1="08"><s1>Leibniz Universität Hannover</s1>
<s2>30167 Hannover</s2>
<s3>DEU</s3>
<sZ>9 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>25 aut.</sZ>
<sZ>43 aut.</sZ>
<sZ>52 aut.</sZ>
</inist:fA14>
<country>Allemagne</country>
</affiliation>
</author>
<author><name sortKey="Bauer, Th S" sort="Bauer, Th S" uniqKey="Bauer T" first="Th. S." last="Bauer">Th. S. Bauer</name>
</author>
<author><name sortKey="Behnke, B" sort="Behnke, B" uniqKey="Behnke B" first="B." last="Behnke">B. Behnke</name>
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<s3>DEU</s3>
<sZ>27 aut.</sZ>
<sZ>45 aut.</sZ>
</inist:fA14>
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</affiliation>
</author>
<author><name sortKey="Bejger, M" sort="Bejger, M" uniqKey="Bejger M" first="M." last="Bejger">M. Bejger</name>
</author>
<author><name sortKey="Beker, M G" sort="Beker, M G" uniqKey="Beker M" first="M. G." last="Beker">M. G. Beker</name>
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<author><name sortKey="Bell, A S" sort="Bell, A S" uniqKey="Bell A" first="A. S." last="Bell">A. S. Bell</name>
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<s2>Glasgow G12 8QQ</s2>
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<author><name sortKey="Billingsley, G" sort="Billingsley, G" uniqKey="Billingsley G" first="G." last="Billingsley">G. Billingsley</name>
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<author><name sortKey="Birch, J" sort="Birch, J" uniqKey="Birch J" first="J." last="Birch">J. Birch</name>
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<author><name sortKey="Birindelli, S" sort="Birindelli, S" uniqKey="Birindelli S" first="S." last="Birindelli">S. Birindelli</name>
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<author><name sortKey="Biswas, R" sort="Biswas, R" uniqKey="Biswas R" first="R." last="Biswas">R. Biswas</name>
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</analytic>
<series><title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
<imprint><date when="2011">2011</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">The Astrophysical journal</title>
<title level="j" type="abbreviated">Astrophys. j.</title>
<idno type="ISSN">0004-637X</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Ellipticity</term>
<term>Energy losses</term>
<term>Gravitational waves</term>
<term>Loss rate</term>
<term>Neutron stars</term>
<term>Pulsars</term>
<term>S stars</term>
<term>Timing</term>
<term>Upper bound</term>
<term>Wave emission</term>
<term>Wave polarization</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Onde gravitationnelle</term>
<term>Emission onde</term>
<term>Pulsar</term>
<term>Borne supérieure</term>
<term>Timing</term>
<term>Etoile S</term>
<term>Polarisation onde</term>
<term>Perte énergie</term>
<term>Taux perte</term>
<term>Ellipticité</term>
<term>Etoile neutron</term>
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<front><div type="abstract" xml:lang="en">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 x 10<sup>-24</sup>
and 2.2 × 10<sup>-24</sup>
, with 95% confidence. The third method, under the same hypothesis, produces a Bayesian upper limit of 2.1 x 10<sup>-24</sup>
, with 95% degree of belief. These limits are below the indirect spin-down limit of 3.3 x 10<sup>-24</sup>
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<sup>-3</sup>
. 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.</div>
</front>
</TEI>
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<fA08 i1="01" i2="1" l="ENG"><s1>BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>ABADIE (J.)</s1>
</fA11>
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<sZ>33 aut.</sZ>
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<sZ>33 aut.</sZ>
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<s3>USA</s3>
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<sZ>58 aut.</sZ>
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<sZ>25 aut.</sZ>
<sZ>43 aut.</sZ>
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<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
<sZ>25 aut.</sZ>
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<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>16 aut.</sZ>
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<sZ>19 aut.</sZ>
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</fA14>
<fA14 i1="13"><s1>INFN, Sezione di Roma</s1>
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<sZ>22 aut.</sZ>
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<sZ>26 aut.</sZ>
</fA14>
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<s3>DEU</s3>
<sZ>27 aut.</sZ>
<sZ>45 aut.</sZ>
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<fA14 i1="17"><s1>Montana State University</s1>
<s2>Bozeman, MT 59717</s2>
<s3>USA</s3>
<sZ>28 aut.</sZ>
</fA14>
<fA14 i1="18"><s1>European Gravitational Observatory (EGO)</s1>
<s2>56021 Cascina (PI)</s2>
<s3>ITA</s3>
<sZ>29 aut.</sZ>
</fA14>
<fA14 i1="19"><s1>Carleton College</s1>
<s2>Northfield, MN 55057</s2>
<s3>USA</s3>
<sZ>32 aut.</sZ>
</fA14>
<fA14 i1="20"><s1>University of Western Australia</s1>
<s2>Crawley, WA 6009</s2>
<s3>AUS</s3>
<sZ>35 aut.</sZ>
</fA14>
<fA14 i1="21"><s1>LIGO-Massachusetts Institute of Technology</s1>
<s2>Cambridge, MA 02139</s2>
<s3>USA</s3>
<sZ>36 aut.</sZ>
</fA14>
<fA14 i1="22"><s1>Laboratoire AstroParticule et Cosmologie (APC) Université Paris Diderot, CNRS: IN2P3, CEA: DSM/IRFU, Observatoire de Paris. 10 rue A. Domon et L. Duquet</s1>
<s2>75013 Paris</s2>
<s3>FRA</s3>
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</fA14>
<fA14 i1="23"><s1>Columbia University</s1>
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<sZ>39 aut.</sZ>
<sZ>50 aut.</sZ>
</fA14>
<fA14 i1="24"><s1>INFN, Sezione di Pisa</s1>
<s2>56127 Pisa</s2>
<s3>ITA</s3>
<sZ>42 aut.</sZ>
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<fA14 i1="25"><s1>Università di Pisa</s1>
<s2>56127 Pisa</s2>
<s3>ITA</s3>
<sZ>42 aut.</sZ>
</fA14>
<fA20><s2>73793.1-73793.16</s2>
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<fA64 i1="01" i2="1"><s0>The Astrophysical journal</s0>
</fA64>
<fA66 i1="01"><s0>GBR</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>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 x 10<sup>-24</sup>
and 2.2 × 10<sup>-24</sup>
, with 95% confidence. The third method, under the same hypothesis, produces a Bayesian upper limit of 2.1 x 10<sup>-24</sup>
, with 95% degree of belief. These limits are below the indirect spin-down limit of 3.3 x 10<sup>-24</sup>
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<sup>-3</sup>
. 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.</s0>
</fC01>
<fC02 i1="01" i2="3"><s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="3" l="FRE"><s0>Onde gravitationnelle</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="3" l="ENG"><s0>Gravitational waves</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE"><s0>Emission onde</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG"><s0>Wave emission</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA"><s0>Emisión onda</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Pulsar</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Pulsars</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Borne supérieure</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Upper bound</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Cota superior</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="3" l="FRE"><s0>Timing</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="3" l="ENG"><s0>Timing</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Etoile S</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>S stars</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Polarisation onde</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Wave polarization</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Polarización onda</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Perte énergie</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Energy losses</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE"><s0>Taux perte</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG"><s0>Loss rate</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Porcentaje pérdida</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Ellipticité</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Ellipticity</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Elipticidad</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Etoile neutron</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Neutron stars</s0>
<s5>36</s5>
</fC03>
<fN21><s1>262</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
</record>
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