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BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR

Identifieur interne : 004519 ( PascalFrancis/Curation ); précédent : 004518; suivant : 004520

BEATING 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. Biswas

Source :

RBID : Pascal:11-0379596

Descripteurs français

English descriptors

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.
pA  
A01 01  1    @0 0004-637X
A02 01      @0 ASJOAB
A03   1    @0 Astrophys. j.
A05       @2 737
A06       @2 2 @3 p. 1
A08 01  1  ENG  @1 BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR
A11 01  1    @1 ABADIE (J.)
A11 02  1    @1 ABBOTT (B. P.)
A11 03  1    @1 ABBOTT (R.)
A11 04  1    @1 ABERNATHY (M.)
A11 05  1    @1 ACCADIA (T.)
A11 06  1    @1 ACERNESE (F.)
A11 07  1    @1 ADAMS (C.)
A11 08  1    @1 ADHIKARI (R.)
A11 09  1    @1 AFFELDT (C.)
A11 10  1    @1 ALLEN (B.)
A11 11  1    @1 ALLEN (G. S.)
A11 12  1    @1 AMADOR CERON (E.)
A11 13  1    @1 AMARIUTEI (D.)
A11 14  1    @1 AMIN (R. S.)
A11 15  1    @1 ANDERSON (S. B.)
A11 16  1    @1 ANDERSON (W. G.)
A11 17  1    @1 ANTONUCCI (F.)
A11 18  1    @1 ARAI (K.)
A11 19  1    @1 ARAIN (M. A.)
A11 20  1    @1 ARAYA (M. C.)
A11 21  1    @1 ASTON (S. M.)
A11 22  1    @1 ASTONE (P.)
A11 23  1    @1 ATKINSON (D.)
A11 24  1    @1 AUFMUTH (P.)
A11 25  1    @1 AULBERT (C.)
A11 26  1    @1 AYLOTT (B. E.)
A11 27  1    @1 BABAK (S.)
A11 28  1    @1 BAKER (P.)
A11 29  1    @1 BALLARDIN (G.)
A11 30  1    @1 BALLMER (S.)
A11 31  1    @1 BARKER (D.)
A11 32  1    @1 BARNUM (S.)
A11 33  1    @1 BARONE (F.)
A11 34  1    @1 BARR (B.)
A11 35  1    @1 BARRIGA (P.)
A11 36  1    @1 BARSOTTI (L.)
A11 37  1    @1 BARSUGLIA (M.)
A11 38  1    @1 BARTON (M. A.)
A11 39  1    @1 BARTOS (I.)
A11 40  1    @1 BASSIRI (R.)
A11 41  1    @1 BASTARRIKA (M.)
A11 42  1    @1 BASTI (A.)
A11 43  1    @1 BAUCHROWITZ (J.)
A11 44  1    @1 BAUER (TH. S.)
A11 45  1    @1 BEHNKE (B.)
A11 46  1    @1 BEJGER (M.)
A11 47  1    @1 BEKER (M. G.)
A11 48  1    @1 BELL (A. S.)
A11 49  1    @1 BELLETOILE (A.)
A11 50  1    @1 BELOPOLSKI (I.)
A11 51  1    @1 BENACQUISTA (M.)
A11 52  1    @1 BERTOLINI (A.)
A11 53  1    @1 BETZWIESER (J.)
A11 54  1    @1 BEVERIDGE (N.)
A11 55  1    @1 BEYERSDORF (P. T.)
A11 56  1    @1 BILENKO (I. A.)
A11 57  1    @1 BILLINGSLEY (G.)
A11 58  1    @1 BIRCH (J.)
A11 59  1    @1 BIRINDELLI (S.)
A11 60  1    @1 BISWAS (R.)
A14 01      @1 LIGO-California Institute of Technology @2 Pasadena, CA 91125 @3 USA @Z 1 aut. @Z 2 aut. @Z 3 aut. @Z 8 aut. @Z 15 aut. @Z 18 aut. @Z 20 aut. @Z 30 aut. @Z 53 aut. @Z 57 aut.
A14 02      @1 University of Glasgow @2 Glasgow G12 8QQ @3 GBR @Z 4 aut. @Z 34 aut. @Z 40 aut. @Z 41 aut. @Z 48 aut. @Z 54 aut.
A14 03      @1 Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3 @2 74941 Annecy-Le-Vieux @3 FRA @Z 5 aut. @Z 49 aut.
A14 04      @1 INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo @2 80126 Napoli @3 ITA @Z 6 aut. @Z 33 aut.
A14 05      @1 Università di Salerno, Fisciano @2 84084 Salerno @3 ITA @Z 6 aut. @Z 33 aut.
A14 06      @1 LIGO-Livingston Observatory @2 Livingston, LA 70754 @3 USA @Z 7 aut. @Z 58 aut.
A14 07      @1 Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik @2 30167 Hannover @3 DEU @Z 9 aut. @Z 10 aut. @Z 24 aut. @Z 25 aut. @Z 43 aut. @Z 52 aut.
A14 08      @1 Leibniz Universität Hannover @2 30167 Hannover @3 DEU @Z 9 aut. @Z 10 aut. @Z 24 aut. @Z 25 aut. @Z 43 aut. @Z 52 aut.
A14 09      @1 University of Wisconsin-Milwaukee @2 Milwaukee, WI 53201 @3 USA @Z 10 aut. @Z 12 aut. @Z 16 aut.
A14 10      @1 Stanford University @2 Stanford, CA 94305 @3 USA @Z 11 aut.
A14 11      @1 University of Florida @2 Gainesville, FL 32611 @3 USA @Z 13 aut. @Z 19 aut.
A14 12      @1 Louisiana State University @2 Baton Rouge, LA 70803 @3 USA @Z 14 aut.
A14 13      @1 INFN, Sezione di Roma @2 00185 Roma @3 ITA @Z 17 aut. @Z 22 aut.
A14 14      @1 University of Birmingham @2 Birmingham B15 2TT @3 GBR @Z 21 aut. @Z 26 aut.
A14 15      @1 LIGO-Hanford Observatory @2 Richland, WA 99352 @3 USA @Z 23 aut. @Z 31 aut. @Z 38 aut.
A14 16      @1 Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik @2 14476 Golm @3 DEU @Z 27 aut. @Z 45 aut.
A14 17      @1 Montana State University @2 Bozeman, MT 59717 @3 USA @Z 28 aut.
A14 18      @1 European Gravitational Observatory (EGO) @2 56021 Cascina (PI) @3 ITA @Z 29 aut.
A14 19      @1 Carleton College @2 Northfield, MN 55057 @3 USA @Z 32 aut.
A14 20      @1 University of Western Australia @2 Crawley, WA 6009 @3 AUS @Z 35 aut.
A14 21      @1 LIGO-Massachusetts Institute of Technology @2 Cambridge, MA 02139 @3 USA @Z 36 aut.
A14 22      @1 Laboratoire AstroParticule et Cosmologie (APC) Université Paris Diderot, CNRS: IN2P3, CEA: DSM/IRFU, Observatoire de Paris. 10 rue A. Domon et L. Duquet @2 75013 Paris @3 FRA @Z 37 aut.
A14 23      @1 Columbia University @2 New York, NY 10027 @3 USA @Z 39 aut. @Z 50 aut.
A14 24      @1 INFN, Sezione di Pisa @2 56127 Pisa @3 ITA @Z 42 aut.
A14 25      @1 Università di Pisa @2 56127 Pisa @3 ITA @Z 42 aut.
A20       @2 73793.1-73793.16
A21       @1 2011
A23 01      @0 ENG
A43 01      @1 INIST @2 512 @5 354000500132270470
A44       @0 0000 @1 © 2011 INIST-CNRS. All rights reserved.
A45       @0 1/2 p.
A47 01  1    @0 11-0379596
A60       @1 P
A61       @0 A
A64 01  1    @0 The Astrophysical journal
A66 01      @0 GBR
C01 01    ENG  @0 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.
C02 01  3    @0 001E03
C03 01  3  FRE  @0 Onde gravitationnelle @5 26
C03 01  3  ENG  @0 Gravitational waves @5 26
C03 02  X  FRE  @0 Emission onde @5 27
C03 02  X  ENG  @0 Wave emission @5 27
C03 02  X  SPA  @0 Emisión onda @5 27
C03 03  3  FRE  @0 Pulsar @5 28
C03 03  3  ENG  @0 Pulsars @5 28
C03 04  X  FRE  @0 Borne supérieure @5 29
C03 04  X  ENG  @0 Upper bound @5 29
C03 04  X  SPA  @0 Cota superior @5 29
C03 05  3  FRE  @0 Timing @5 30
C03 05  3  ENG  @0 Timing @5 30
C03 06  3  FRE  @0 Etoile S @5 31
C03 06  3  ENG  @0 S stars @5 31
C03 07  X  FRE  @0 Polarisation onde @5 32
C03 07  X  ENG  @0 Wave polarization @5 32
C03 07  X  SPA  @0 Polarización onda @5 32
C03 08  3  FRE  @0 Perte énergie @5 33
C03 08  3  ENG  @0 Energy losses @5 33
C03 09  X  FRE  @0 Taux perte @5 34
C03 09  X  ENG  @0 Loss rate @5 34
C03 09  X  SPA  @0 Porcentaje pérdida @5 34
C03 10  X  FRE  @0 Ellipticité @5 35
C03 10  X  ENG  @0 Ellipticity @5 35
C03 10  X  SPA  @0 Elipticidad @5 35
C03 11  3  FRE  @0 Etoile neutron @5 36
C03 11  3  ENG  @0 Neutron stars @5 36
N21       @1 262
N44 01      @1 OTO
N82       @1 OTO

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Pascal:11-0379596

Le document en format XML

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<s1>Louisiana State University</s1>
<s2>Baton Rouge, LA 70803</s2>
<s3>USA</s3>
<sZ>14 aut.</sZ>
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<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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<inist:fA14 i1="09">
<s1>University of Wisconsin-Milwaukee</s1>
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<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
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<name sortKey="Antonucci, F" sort="Antonucci, F" uniqKey="Antonucci F" first="F." last="Antonucci">F. Antonucci</name>
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<s1>INFN, Sezione di Roma</s1>
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<name sortKey="Arai, K" sort="Arai, K" uniqKey="Arai K" first="K." last="Arai">K. Arai</name>
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<s1>LIGO-California Institute of Technology</s1>
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<name sortKey="Arain, M A" sort="Arain, M A" uniqKey="Arain M" first="M. A." last="Arain">M. A. Arain</name>
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<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>
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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>
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<inist:fA14 i1="01">
<s1>LIGO-California Institute of Technology</s1>
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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>
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<inist:fA14 i1="14">
<s1>University of Birmingham</s1>
<s2>Birmingham B15 2TT</s2>
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<sZ>21 aut.</sZ>
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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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<inist:fA14 i1="13">
<s1>INFN, Sezione di Roma</s1>
<s2>00185 Roma</s2>
<s3>ITA</s3>
<sZ>17 aut.</sZ>
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<author>
<name sortKey="Atkinson, D" sort="Atkinson, D" uniqKey="Atkinson D" first="D." last="Atkinson">D. Atkinson</name>
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<inist:fA14 i1="15">
<s1>LIGO-Hanford Observatory</s1>
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<s3>USA</s3>
<sZ>23 aut.</sZ>
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<sZ>38 aut.</sZ>
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</affiliation>
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<author>
<name sortKey="Aufmuth, P" sort="Aufmuth, P" uniqKey="Aufmuth P" first="P." last="Aufmuth">P. Aufmuth</name>
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<inist:fA14 i1="07">
<s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
<s2>30167 Hannover</s2>
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<inist:fA14 i1="08">
<s1>Leibniz Universität Hannover</s1>
<s2>30167 Hannover</s2>
<s3>DEU</s3>
<sZ>9 aut.</sZ>
<sZ>10 aut.</sZ>
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</affiliation>
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<author>
<name sortKey="Aulbert, C" sort="Aulbert, C" uniqKey="Aulbert C" first="C." last="Aulbert">C. Aulbert</name>
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<inist:fA14 i1="07">
<s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
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<s3>DEU</s3>
<sZ>9 aut.</sZ>
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<inist:fA14 i1="08">
<s1>Leibniz Universität Hannover</s1>
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<s3>DEU</s3>
<sZ>9 aut.</sZ>
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<author>
<name sortKey="Aylott, B E" sort="Aylott, B E" uniqKey="Aylott B" first="B. E." last="Aylott">B. E. Aylott</name>
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<inist:fA14 i1="14">
<s1>University of Birmingham</s1>
<s2>Birmingham B15 2TT</s2>
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<sZ>21 aut.</sZ>
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<author>
<name sortKey="Babak, S" sort="Babak, S" uniqKey="Babak S" first="S." last="Babak">S. Babak</name>
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<inist:fA14 i1="16">
<s1>Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik</s1>
<s2>14476 Golm</s2>
<s3>DEU</s3>
<sZ>27 aut.</sZ>
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</affiliation>
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<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>
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<author>
<name sortKey="Ballardin, G" sort="Ballardin, G" uniqKey="Ballardin G" first="G." last="Ballardin">G. Ballardin</name>
<affiliation wicri:level="1">
<inist:fA14 i1="18">
<s1>European Gravitational Observatory (EGO)</s1>
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<sZ>29 aut.</sZ>
</inist:fA14>
<country>Italie</country>
</affiliation>
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<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>
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<author>
<name sortKey="Barker, D" sort="Barker, D" uniqKey="Barker D" first="D." last="Barker">D. Barker</name>
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<inist:fA14 i1="15">
<s1>LIGO-Hanford Observatory</s1>
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<sZ>23 aut.</sZ>
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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>
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<author>
<name sortKey="Barone, F" sort="Barone, F" uniqKey="Barone F" first="F." last="Barone">F. Barone</name>
<affiliation wicri:level="1">
<inist:fA14 i1="04">
<s1>INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo</s1>
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<sZ>6 aut.</sZ>
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</inist:fA14>
<country>Italie</country>
</affiliation>
<affiliation wicri:level="1">
<inist:fA14 i1="05">
<s1>Università di Salerno, Fisciano</s1>
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<sZ>6 aut.</sZ>
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<country>Italie</country>
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<author>
<name sortKey="Barr, B" sort="Barr, B" uniqKey="Barr B" first="B." last="Barr">B. Barr</name>
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<inist:fA14 i1="02">
<s1>University of Glasgow</s1>
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</affiliation>
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<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>
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<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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<inist:fA14 i1="21">
<s1>LIGO-Massachusetts Institute of Technology</s1>
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</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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<inist: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>
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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>
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<inist:fA14 i1="15">
<s1>LIGO-Hanford Observatory</s1>
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<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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<inist:fA14 i1="02">
<s1>University of Glasgow</s1>
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<sZ>4 aut.</sZ>
<sZ>34 aut.</sZ>
<sZ>40 aut.</sZ>
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<country>Royaume-Uni</country>
</affiliation>
</author>
<author>
<name sortKey="Bastarrika, M" sort="Bastarrika, M" uniqKey="Bastarrika M" first="M." last="Bastarrika">M. Bastarrika</name>
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<inist:fA14 i1="02">
<s1>University of Glasgow</s1>
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<sZ>4 aut.</sZ>
<sZ>34 aut.</sZ>
<sZ>40 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>
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<inist:fA14 i1="24">
<s1>INFN, Sezione di Pisa</s1>
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<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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<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>
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<inist:fA14 i1="07">
<s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
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<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>
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<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>
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</affiliation>
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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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<inist:fA14 i1="16">
<s1>Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik</s1>
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<sZ>27 aut.</sZ>
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</inist:fA14>
<country>Allemagne</country>
</affiliation>
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<author>
<name sortKey="Bejger, M" sort="Bejger, M" uniqKey="Bejger M" first="M." last="Bejger">M. Bejger</name>
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<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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<inist:fA14 i1="02">
<s1>University of Glasgow</s1>
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<sZ>34 aut.</sZ>
<sZ>40 aut.</sZ>
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<author>
<name sortKey="Belletoile, A" sort="Belletoile, A" uniqKey="Belletoile A" first="A." last="Belletoile">A. Belletoile</name>
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<inist:fA14 i1="03">
<s1>Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3</s1>
<s2>74941 Annecy-Le-Vieux</s2>
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<sZ>5 aut.</sZ>
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<country>France</country>
</affiliation>
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<author>
<name sortKey="Belopolski, I" sort="Belopolski, I" uniqKey="Belopolski I" first="I." last="Belopolski">I. Belopolski</name>
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<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>
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<author>
<name sortKey="Benacquista, M" sort="Benacquista, M" uniqKey="Benacquista M" first="M." last="Benacquista">M. Benacquista</name>
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<author>
<name sortKey="Bertolini, A" sort="Bertolini, A" uniqKey="Bertolini A" first="A." last="Bertolini">A. Bertolini</name>
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<inist:fA14 i1="07">
<s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
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<sZ>10 aut.</sZ>
<sZ>24 aut.</sZ>
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<title xml:lang="en" level="a">BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR</title>
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<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>
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<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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<s1>Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik</s1>
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<sZ>27 aut.</sZ>
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<author>
<name sortKey="Baker, P" sort="Baker, P" uniqKey="Baker P" first="P." last="Baker">P. Baker</name>
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<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>
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<author>
<name sortKey="Ballardin, G" sort="Ballardin, G" uniqKey="Ballardin G" first="G." last="Ballardin">G. Ballardin</name>
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<name sortKey="Ballmer, S" sort="Ballmer, S" uniqKey="Ballmer S" first="S." last="Ballmer">S. Ballmer</name>
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<name sortKey="Barker, D" sort="Barker, D" uniqKey="Barker D" first="D." last="Barker">D. Barker</name>
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<name sortKey="Barnum, S" sort="Barnum, S" uniqKey="Barnum S" first="S." last="Barnum">S. Barnum</name>
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<s1>Carleton College</s1>
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<country>États-Unis</country>
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<name sortKey="Barone, F" sort="Barone, F" uniqKey="Barone F" first="F." last="Barone">F. Barone</name>
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<s1>INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo</s1>
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<country>Italie</country>
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<s1>Università di Salerno, Fisciano</s1>
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<sZ>33 aut.</sZ>
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<name sortKey="Barr, B" sort="Barr, B" uniqKey="Barr B" first="B." last="Barr">B. Barr</name>
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<s1>University of Glasgow</s1>
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<name sortKey="Barriga, P" sort="Barriga, P" uniqKey="Barriga P" first="P." last="Barriga">P. Barriga</name>
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<inist:fA14 i1="20">
<s1>University of Western Australia</s1>
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</inist:fA14>
<country>Australie</country>
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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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<s1>LIGO-Massachusetts Institute of Technology</s1>
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<name sortKey="Barsuglia, M" sort="Barsuglia, M" uniqKey="Barsuglia M" first="M." last="Barsuglia">M. Barsuglia</name>
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<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>
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<country>France</country>
</affiliation>
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<author>
<name sortKey="Barton, M A" sort="Barton, M A" uniqKey="Barton M" first="M. A." last="Barton">M. A. Barton</name>
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<inist:fA14 i1="15">
<s1>LIGO-Hanford Observatory</s1>
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<author>
<name sortKey="Bartos, I" sort="Bartos, I" uniqKey="Bartos I" first="I." last="Bartos">I. Bartos</name>
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<inist:fA14 i1="23">
<s1>Columbia University</s1>
<s2>New York, NY 10027</s2>
<s3>USA</s3>
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<sZ>50 aut.</sZ>
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<country>États-Unis</country>
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<name sortKey="Bassiri, R" sort="Bassiri, R" uniqKey="Bassiri R" first="R." last="Bassiri">R. Bassiri</name>
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<s1>University of Glasgow</s1>
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<name sortKey="Bastarrika, M" sort="Bastarrika, M" uniqKey="Bastarrika M" first="M." last="Bastarrika">M. Bastarrika</name>
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<s1>University of Glasgow</s1>
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</author>
<author>
<name sortKey="Basti, A" sort="Basti, A" uniqKey="Basti A" first="A." last="Basti">A. Basti</name>
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<s1>INFN, Sezione di Pisa</s1>
<s2>56127 Pisa</s2>
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</inist:fA14>
<country>Italie</country>
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<affiliation wicri:level="1">
<inist:fA14 i1="25">
<s1>Università di Pisa</s1>
<s2>56127 Pisa</s2>
<s3>ITA</s3>
<sZ>42 aut.</sZ>
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<country>Italie</country>
</affiliation>
</author>
<author>
<name sortKey="Bauchrowitz, J" sort="Bauchrowitz, J" uniqKey="Bauchrowitz J" first="J." last="Bauchrowitz">J. Bauchrowitz</name>
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<inist:fA14 i1="07">
<s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</s1>
<s2>30167 Hannover</s2>
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<sZ>25 aut.</sZ>
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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>
<sZ>43 aut.</sZ>
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<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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<inist:fA14 i1="16">
<s1>Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik</s1>
<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="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>
</author>
<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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<inist:fA14 i1="02">
<s1>University of Glasgow</s1>
<s2>Glasgow G12 8QQ</s2>
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<sZ>40 aut.</sZ>
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<country>Royaume-Uni</country>
</affiliation>
</author>
<author>
<name sortKey="Belletoile, A" sort="Belletoile, A" uniqKey="Belletoile A" first="A." last="Belletoile">A. Belletoile</name>
<affiliation wicri:level="1">
<inist:fA14 i1="03">
<s1>Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3</s1>
<s2>74941 Annecy-Le-Vieux</s2>
<s3>FRA</s3>
<sZ>5 aut.</sZ>
<sZ>49 aut.</sZ>
</inist:fA14>
<country>France</country>
</affiliation>
</author>
<author>
<name sortKey="Belopolski, I" sort="Belopolski, I" uniqKey="Belopolski I" first="I." last="Belopolski">I. Belopolski</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="Benacquista, M" sort="Benacquista, M" uniqKey="Benacquista M" first="M." last="Benacquista">M. Benacquista</name>
</author>
<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>
<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>
<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>
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<country>Allemagne</country>
</affiliation>
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<author>
<name sortKey="Betzwieser, J" sort="Betzwieser, J" uniqKey="Betzwieser J" first="J." last="Betzwieser">J. Betzwieser</name>
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<inist:fA14 i1="01">
<s1>LIGO-California Institute of Technology</s1>
<s2>Pasadena, CA 91125</s2>
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<country>États-Unis</country>
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</author>
<author>
<name sortKey="Beveridge, N" sort="Beveridge, N" uniqKey="Beveridge N" first="N." last="Beveridge">N. Beveridge</name>
<affiliation wicri:level="1">
<inist:fA14 i1="02">
<s1>University of Glasgow</s1>
<s2>Glasgow G12 8QQ</s2>
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<sZ>40 aut.</sZ>
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<country>Royaume-Uni</country>
</affiliation>
</author>
<author>
<name sortKey="Beyersdorf, P T" sort="Beyersdorf, P T" uniqKey="Beyersdorf P" first="P. T." last="Beyersdorf">P. T. Beyersdorf</name>
</author>
<author>
<name sortKey="Bilenko, I A" sort="Bilenko, I A" uniqKey="Bilenko I" first="I. A." last="Bilenko">I. A. Bilenko</name>
</author>
<author>
<name sortKey="Billingsley, G" sort="Billingsley, G" uniqKey="Billingsley G" first="G." last="Billingsley">G. Billingsley</name>
<affiliation wicri:level="1">
<inist:fA14 i1="01">
<s1>LIGO-California Institute of Technology</s1>
<s2>Pasadena, CA 91125</s2>
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</affiliation>
</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>
<s2>Livingston, LA 70754</s2>
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<sZ>7 aut.</sZ>
<sZ>58 aut.</sZ>
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</author>
<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>
</author>
</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>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<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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<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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<s1>ABBOTT (B. P.)</s1>
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<s1>ABBOTT (R.)</s1>
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<s1>ABERNATHY (M.)</s1>
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<s1>ACCADIA (T.)</s1>
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<s1>ACERNESE (F.)</s1>
</fA11>
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<s1>ADAMS (C.)</s1>
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<s1>ADHIKARI (R.)</s1>
</fA11>
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<s1>AFFELDT (C.)</s1>
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<s1>ALLEN (B.)</s1>
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<s1>ALLEN (G. S.)</s1>
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<s1>AMADOR CERON (E.)</s1>
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<fA11 i1="13" i2="1">
<s1>AMARIUTEI (D.)</s1>
</fA11>
<fA11 i1="14" i2="1">
<s1>AMIN (R. S.)</s1>
</fA11>
<fA11 i1="15" i2="1">
<s1>ANDERSON (S. B.)</s1>
</fA11>
<fA11 i1="16" i2="1">
<s1>ANDERSON (W. G.)</s1>
</fA11>
<fA11 i1="17" i2="1">
<s1>ANTONUCCI (F.)</s1>
</fA11>
<fA11 i1="18" i2="1">
<s1>ARAI (K.)</s1>
</fA11>
<fA11 i1="19" i2="1">
<s1>ARAIN (M. A.)</s1>
</fA11>
<fA11 i1="20" i2="1">
<s1>ARAYA (M. C.)</s1>
</fA11>
<fA11 i1="21" i2="1">
<s1>ASTON (S. M.)</s1>
</fA11>
<fA11 i1="22" i2="1">
<s1>ASTONE (P.)</s1>
</fA11>
<fA11 i1="23" i2="1">
<s1>ATKINSON (D.)</s1>
</fA11>
<fA11 i1="24" i2="1">
<s1>AUFMUTH (P.)</s1>
</fA11>
<fA11 i1="25" i2="1">
<s1>AULBERT (C.)</s1>
</fA11>
<fA11 i1="26" i2="1">
<s1>AYLOTT (B. E.)</s1>
</fA11>
<fA11 i1="27" i2="1">
<s1>BABAK (S.)</s1>
</fA11>
<fA11 i1="28" i2="1">
<s1>BAKER (P.)</s1>
</fA11>
<fA11 i1="29" i2="1">
<s1>BALLARDIN (G.)</s1>
</fA11>
<fA11 i1="30" i2="1">
<s1>BALLMER (S.)</s1>
</fA11>
<fA11 i1="31" i2="1">
<s1>BARKER (D.)</s1>
</fA11>
<fA11 i1="32" i2="1">
<s1>BARNUM (S.)</s1>
</fA11>
<fA11 i1="33" i2="1">
<s1>BARONE (F.)</s1>
</fA11>
<fA11 i1="34" i2="1">
<s1>BARR (B.)</s1>
</fA11>
<fA11 i1="35" i2="1">
<s1>BARRIGA (P.)</s1>
</fA11>
<fA11 i1="36" i2="1">
<s1>BARSOTTI (L.)</s1>
</fA11>
<fA11 i1="37" i2="1">
<s1>BARSUGLIA (M.)</s1>
</fA11>
<fA11 i1="38" i2="1">
<s1>BARTON (M. A.)</s1>
</fA11>
<fA11 i1="39" i2="1">
<s1>BARTOS (I.)</s1>
</fA11>
<fA11 i1="40" i2="1">
<s1>BASSIRI (R.)</s1>
</fA11>
<fA11 i1="41" i2="1">
<s1>BASTARRIKA (M.)</s1>
</fA11>
<fA11 i1="42" i2="1">
<s1>BASTI (A.)</s1>
</fA11>
<fA11 i1="43" i2="1">
<s1>BAUCHROWITZ (J.)</s1>
</fA11>
<fA11 i1="44" i2="1">
<s1>BAUER (TH. S.)</s1>
</fA11>
<fA11 i1="45" i2="1">
<s1>BEHNKE (B.)</s1>
</fA11>
<fA11 i1="46" i2="1">
<s1>BEJGER (M.)</s1>
</fA11>
<fA11 i1="47" i2="1">
<s1>BEKER (M. G.)</s1>
</fA11>
<fA11 i1="48" i2="1">
<s1>BELL (A. S.)</s1>
</fA11>
<fA11 i1="49" i2="1">
<s1>BELLETOILE (A.)</s1>
</fA11>
<fA11 i1="50" i2="1">
<s1>BELOPOLSKI (I.)</s1>
</fA11>
<fA11 i1="51" i2="1">
<s1>BENACQUISTA (M.)</s1>
</fA11>
<fA11 i1="52" i2="1">
<s1>BERTOLINI (A.)</s1>
</fA11>
<fA11 i1="53" i2="1">
<s1>BETZWIESER (J.)</s1>
</fA11>
<fA11 i1="54" i2="1">
<s1>BEVERIDGE (N.)</s1>
</fA11>
<fA11 i1="55" i2="1">
<s1>BEYERSDORF (P. T.)</s1>
</fA11>
<fA11 i1="56" i2="1">
<s1>BILENKO (I. A.)</s1>
</fA11>
<fA11 i1="57" i2="1">
<s1>BILLINGSLEY (G.)</s1>
</fA11>
<fA11 i1="58" i2="1">
<s1>BIRCH (J.)</s1>
</fA11>
<fA11 i1="59" i2="1">
<s1>BIRINDELLI (S.)</s1>
</fA11>
<fA11 i1="60" i2="1">
<s1>BISWAS (R.)</s1>
</fA11>
<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>
<sZ>8 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>20 aut.</sZ>
<sZ>30 aut.</sZ>
<sZ>53 aut.</sZ>
<sZ>57 aut.</sZ>
</fA14>
<fA14 i1="02">
<s1>University of Glasgow</s1>
<s2>Glasgow G12 8QQ</s2>
<s3>GBR</s3>
<sZ>4 aut.</sZ>
<sZ>34 aut.</sZ>
<sZ>40 aut.</sZ>
<sZ>41 aut.</sZ>
<sZ>48 aut.</sZ>
<sZ>54 aut.</sZ>
</fA14>
<fA14 i1="03">
<s1>Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), Université de Savoie, CNRS/IN2P3</s1>
<s2>74941 Annecy-Le-Vieux</s2>
<s3>FRA</s3>
<sZ>5 aut.</sZ>
<sZ>49 aut.</sZ>
</fA14>
<fA14 i1="04">
<s1>INFN, Sezione di Napoli, Complesso Universitario di Monte S. Angelo</s1>
<s2>80126 Napoli</s2>
<s3>ITA</s3>
<sZ>6 aut.</sZ>
<sZ>33 aut.</sZ>
</fA14>
<fA14 i1="05">
<s1>Università di Salerno, Fisciano</s1>
<s2>84084 Salerno</s2>
<s3>ITA</s3>
<sZ>6 aut.</sZ>
<sZ>33 aut.</sZ>
</fA14>
<fA14 i1="06">
<s1>LIGO-Livingston Observatory</s1>
<s2>Livingston, LA 70754</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
<sZ>58 aut.</sZ>
</fA14>
<fA14 i1="07">
<s1>Albert-Einstein-Institut, Max-Planck-Institut fur Gravitationsphysik</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>
</fA14>
<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>
</fA14>
<fA14 i1="09">
<s1>University of Wisconsin-Milwaukee</s1>
<s2>Milwaukee, WI 53201</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>16 aut.</sZ>
</fA14>
<fA14 i1="10">
<s1>Stanford University</s1>
<s2>Stanford, CA 94305</s2>
<s3>USA</s3>
<sZ>11 aut.</sZ>
</fA14>
<fA14 i1="11">
<s1>University of Florida</s1>
<s2>Gainesville, FL 32611</s2>
<s3>USA</s3>
<sZ>13 aut.</sZ>
<sZ>19 aut.</sZ>
</fA14>
<fA14 i1="12">
<s1>Louisiana State University</s1>
<s2>Baton Rouge, LA 70803</s2>
<s3>USA</s3>
<sZ>14 aut.</sZ>
</fA14>
<fA14 i1="13">
<s1>INFN, Sezione di Roma</s1>
<s2>00185 Roma</s2>
<s3>ITA</s3>
<sZ>17 aut.</sZ>
<sZ>22 aut.</sZ>
</fA14>
<fA14 i1="14">
<s1>University of Birmingham</s1>
<s2>Birmingham B15 2TT</s2>
<s3>GBR</s3>
<sZ>21 aut.</sZ>
<sZ>26 aut.</sZ>
</fA14>
<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>
</fA14>
<fA14 i1="16">
<s1>Albert-Einstein-Institut, Max-Planck-Institut für Gravitationsphysik</s1>
<s2>14476 Golm</s2>
<s3>DEU</s3>
<sZ>27 aut.</sZ>
<sZ>45 aut.</sZ>
</fA14>
<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>
<sZ>37 aut.</sZ>
</fA14>
<fA14 i1="23">
<s1>Columbia University</s1>
<s2>New York, NY 10027</s2>
<s3>USA</s3>
<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>
</fA14>
<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>
</fA20>
<fA21>
<s1>2011</s1>
</fA21>
<fA23 i1="01">
<s0>ENG</s0>
</fA23>
<fA43 i1="01">
<s1>INIST</s1>
<s2>512</s2>
<s5>354000500132270470</s5>
</fA43>
<fA44>
<s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45>
<s0>1/2 p.</s0>
</fA45>
<fA47 i1="01" i2="1">
<s0>11-0379596</s0>
</fA47>
<fA60>
<s1>P</s1>
</fA60>
<fA61>
<s0>A</s0>
</fA61>
<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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   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
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   |texte=   BEATING THE SPIN-DOWN LIMIT ON GRAVITATIONAL WAVE EMISSION FROM THE VELA PULSAR
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