AustralieFrV1, PascalFrancis, Corpus, bibRecord, 001B07

Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data

Identifieur interne : 001B07 ( PascalFrancis/Corpus ); précédent : 001B06; suivant : 001B08

Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data

Auteurs : R. Van Haasteren ; Y. Levin ; G. H. Janssen ; K. Lazaridis ; M. Kramer ; B. W. Stappers ; G. Desvignes ; M. B. Purver ; A. G. Lyne ; R. D. Ferdman ; A. Jessner ; I. Cognard ; G. Theureau ; N. D'Amico ; A. Possenti ; M. Burgay ; A. Corongiu ; J. W. T. Hessels ; R. Smits ; J. P. W. Verbiest

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.

RBID : Pascal:11-0320593

Descripteurs français

Pascal (Inist)
- Onde gravitationnelle, Pulsar, Timing, Loi puissance, Borne supérieure, Algorithme, Processus stochastique, Processus gaussien, Trou noir supermassif, Limite confiance, Analyse donnée, Cosmologie.

English descriptors

KwdEn :
- Algorithms, Confidence limit, Cosmology, Data analysis, Gaussian processes, Gravitational waves, Power law, Pulsars, Stochastic processes, Supermassive black hole, Timing, Upper bound.

Abstract

Direct detection of low-frequency gravitational waves (GWs, 10^-9 to 10^-g Hz) is the main goal of pulsar timing array (PTA) projects. One of the main targets for the PTAs is to measure the stochastic background of gravitational waves (GWB) whose characteristic strain is expected to approximately follow a power-law of the form h_c(f) = A(f /yr^-1)α, where f is the GW frequency. In this paper we use the current data from the European PTA to determine an upper limit on the GWB amplitude A as a function of the unknown spectral slope α with a Bayesian algorithm, by modelling the GWB as a random Gaussian process. For the case α = -2/3, which is expected if the GWB is produced by supermassive black hole binaries, we obtain a 95 per cent confidence upper limit on A of 6 x 10^-15, which is 1.8 times lower than the 95 per cent confidence GWB limit obtained by the Parkes PTA in 2006. Our approach to the data analysis incorporates the multitelescope nature of the European PTA and thus can serve as a useful template for future intercontinental PTA collaborations.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

A01	`01`	`1`		`@0 0035-8711`
A02	`01`			`@0 MNRAA4`
A03		`1`		`@0 Mon. Not. R. Astron. Soc.`
A05				`@2 414`
A06				`@2 4`
A08	`01`	`1`	`ENG`	`@1 Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data`
A11	`01`	`1`		`@1 VAN HAASTEREN (R.)`
A11	`02`	`1`		`@1 LEVIN (Y.)`
A11	`03`	`1`		`@1 JANSSEN (G. H.)`
A11	`04`	`1`		`@1 LAZARIDIS (K.)`
A11	`05`	`1`		`@1 KRAMER (M.)`
A11	`06`	`1`		`@1 STAPPERS (B. W.)`
A11	`07`	`1`		`@1 DESVIGNES (G.)`
A11	`08`	`1`		`@1 PURVER (M. B.)`
A11	`09`	`1`		`@1 LYNE (A. G.)`
A11	`10`	`1`		`@1 FERDMAN (R. D.)`
A11	`11`	`1`		`@1 JESSNER (A.)`
A11	`12`	`1`		`@1 COGNARD (I.)`
A11	`13`	`1`		`@1 THEUREAU (G.)`
A11	`14`	`1`		`@1 D'AMICO (N.)`
A11	`15`	`1`		`@1 POSSENTI (A.)`
A11	`16`	`1`		`@1 BURGAY (M.)`
A11	`17`	`1`		`@1 CORONGIU (A.)`
A11	`18`	`1`		`@1 HESSELS (J. W. T.)`
A11	`19`	`1`		`@1 SMITS (R.)`
A11	`20`	`1`		`@1 VERBIEST (J. P. W.)`
A14	`01`			`@1 Leiden Observatory, Leiden University, PO Box 9513 @2 2300 RA Leiden @3 NLD @Z 1 aut. @Z 2 aut.`
A14	`02`			`@1 School of Physics, Monash University, PO Box 27 @2 VIC 3800 @3 AUS @Z 2 aut.`
A14	`03`			`@1 University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building @2 Manchester M13 9PL @3 GBR @Z 3 aut. @Z 5 aut. @Z 6 aut. @Z 8 aut. @Z 19 aut.`
A14	`04`			`@1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69 @2 53121 Bonn @3 DEU @Z 4 aut. @Z 5 aut. @Z 11 aut. @Z 20 aut.`
A14	`05`			`@1 Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2 @2 7990 AA Dwingeloo @3 NLD @Z 6 aut. @Z 18 aut. @Z 19 aut.`
A14	`06`			`@1 LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique @2 45071 Orléans @3 FRA @Z 7 aut. @Z 10 aut. @Z 12 aut. @Z 13 aut.`
A14	`07`			`@1 Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU @2 18330 Nançay @3 FRA @Z 7 aut. @Z 10 aut. @Z 12 aut. @Z 13 aut.`
A14	`08`			`@1 Department of Astronomy and Radio Astronomy Laboratory, University of California @2 Berkeley, CA 94720 @3 USA @Z 7 aut.`
A14	`09`			`@1 University ofmanchester, Jodrell Bank Observatory @2 Macclesfield, Cheshire, SK11 9DL @3 GBR @Z 9 aut.`
A14	`10`			`@1 Dipartimento di Fisica, Universit========Atilde; Degli Studi di Cagliari, SP Monserrato-Sestu km 0.7 @2 90042 Monserrato (CA) @3 ITA @Z 14 aut.`
A14	`11`			`@1 INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54 @2 09012 Capoterra (CA) @3 ITA @Z 14 aut. @Z 15 aut. @Z 16 aut. @Z 17 aut.`
A14	`12`			`@1 Astronomical Institute 'Anton Pannekoek', University of Amsterdam @2 1098 SJ Amsterdam @3 NLD @Z 18 aut.`
A20				`@1 3117-3128`
A21				`@1 2011`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000190477460250`
A44				`@0 0000 @1 © 2011 INIST-CNRS. All rights reserved.`
A45				`@0 1/4 p.`
A47	`01`	`1`		`@0 11-0320593`
A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 Monthly Notices of the Royal Astronomical Society`
A66	`01`			`@0 USA`
C01	`01`		`ENG`	@0 Direct detection of low-frequency gravitational waves (GWs, 10^-9 to 10^-g Hz) is the main goal of pulsar timing array (PTA) projects. One of the main targets for the PTAs is to measure the stochastic background of gravitational waves (GWB) whose characteristic strain is expected to approximately follow a power-law of the form h_c(f) = A(f /yr^-1)α, where f is the GW frequency. In this paper we use the current data from the European PTA to determine an upper limit on the GWB amplitude A as a function of the unknown spectral slope α with a Bayesian algorithm, by modelling the GWB as a random Gaussian process. For the case α = -2/3, which is expected if the GWB is produced by supermassive black hole binaries, we obtain a 95 per cent confidence upper limit on A of 6 x 10^-15, which is 1.8 times lower than the 95 per cent confidence GWB limit obtained by the Parkes PTA in 2006. Our approach to the data analysis incorporates the multitelescope nature of the European PTA and thus can serve as a useful template for future intercontinental PTA collaborations.
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`	`3`	`FRE`	`@0 Pulsar @5 27`
C03	`02`	`3`	`ENG`	`@0 Pulsars @5 27`
C03	`03`	`3`	`FRE`	`@0 Timing @5 28`
C03	`03`	`3`	`ENG`	`@0 Timing @5 28`
C03	`04`	`X`	`FRE`	`@0 Loi puissance @5 29`
C03	`04`	`X`	`ENG`	`@0 Power law @5 29`
C03	`04`	`X`	`SPA`	`@0 Ley poder @5 29`
C03	`05`	`X`	`FRE`	`@0 Borne supérieure @5 30`
C03	`05`	`X`	`ENG`	`@0 Upper bound @5 30`
C03	`05`	`X`	`SPA`	`@0 Cota superior @5 30`
C03	`06`	`3`	`FRE`	`@0 Algorithme @5 31`
C03	`06`	`3`	`ENG`	`@0 Algorithms @5 31`
C03	`07`	`3`	`FRE`	`@0 Processus stochastique @5 32`
C03	`07`	`3`	`ENG`	`@0 Stochastic processes @5 32`
C03	`08`	`3`	`FRE`	`@0 Processus gaussien @5 33`
C03	`08`	`3`	`ENG`	`@0 Gaussian processes @5 33`
C03	`09`	`X`	`FRE`	`@0 Trou noir supermassif @5 34`
C03	`09`	`X`	`ENG`	`@0 Supermassive black hole @5 34`
C03	`09`	`X`	`SPA`	`@0 Agujero negro supermasivo @5 34`
C03	`10`	`X`	`FRE`	`@0 Limite confiance @5 35`
C03	`10`	`X`	`ENG`	`@0 Confidence limit @5 35`
C03	`10`	`X`	`SPA`	`@0 Límite confianza @5 35`
C03	`11`	`3`	`FRE`	`@0 Analyse donnée @5 36`
C03	`11`	`3`	`ENG`	`@0 Data analysis @5 36`
C03	`12`	`3`	`FRE`	`@0 Cosmologie @5 37`
C03	`12`	`3`	`ENG`	`@0 Cosmology @5 37`
N21				`@1 220`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 11-0320593 INIST
ET :	Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data
AU :	VAN HAASTEREN (R.); LEVIN (Y.); JANSSEN (G. H.); LAZARIDIS (K.); KRAMER (M.); STAPPERS (B. W.); DESVIGNES (G.); PURVER (M. B.); LYNE (A. G.); FERDMAN (R. D.); JESSNER (A.); COGNARD (I.); THEUREAU (G.); D'AMICO (N.); POSSENTI (A.); BURGAY (M.); CORONGIU (A.); HESSELS (J. W. T.); SMITS (R.); VERBIEST (J. P. W.)
AF :	Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (1 aut., 2 aut.); School of Physics, Monash University, PO Box 27/VIC 3800/Australie (2 aut.); University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building/Manchester M13 9PL/Royaume-Uni (3 aut., 5 aut., 6 aut., 8 aut., 19 aut.); Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69/53121 Bonn/Allemagne (4 aut., 5 aut., 11 aut., 20 aut.); Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2/7990 AA Dwingeloo/Pays-Bas (6 aut., 18 aut., 19 aut.); LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique/45071 Orléans/France (7 aut., 10 aut., 12 aut., 13 aut.); Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU/18330 Nançay/France (7 aut., 10 aut., 12 aut., 13 aut.); Department of Astronomy and Radio Astronomy Laboratory, University of California/Berkeley, CA 94720/Etats-Unis (7 aut.); University ofmanchester, Jodrell Bank Observatory/Macclesfield, Cheshire, SK11 9DL/Royaume-Uni (9 aut.); Dipartimento di Fisica, Universit========Atilde; Degli Studi di Cagliari, SP Monserrato-Sestu km 0.7/90042 Monserrato (CA)/Italie (14 aut.); INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54/09012 Capoterra (CA)/Italie (14 aut., 15 aut., 16 aut., 17 aut.); Astronomical Institute 'Anton Pannekoek', University of Amsterdam/1098 SJ Amsterdam/Pays-Bas (18 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 4; Pp. 3117-3128; Bibl. 1/4 p.
LA :	Anglais
EA :	Direct detection of low-frequency gravitational waves (GWs, 10^-9 to 10^-g Hz) is the main goal of pulsar timing array (PTA) projects. One of the main targets for the PTAs is to measure the stochastic background of gravitational waves (GWB) whose characteristic strain is expected to approximately follow a power-law of the form h_c(f) = A(f /yr^-1)α, where f is the GW frequency. In this paper we use the current data from the European PTA to determine an upper limit on the GWB amplitude A as a function of the unknown spectral slope α with a Bayesian algorithm, by modelling the GWB as a random Gaussian process. For the case α = -2/3, which is expected if the GWB is produced by supermassive black hole binaries, we obtain a 95 per cent confidence upper limit on A of 6 x 10^-15, which is 1.8 times lower than the 95 per cent confidence GWB limit obtained by the Parkes PTA in 2006. Our approach to the data analysis incorporates the multitelescope nature of the European PTA and thus can serve as a useful template for future intercontinental PTA collaborations.
CC :	001E03
FD :	Onde gravitationnelle; Pulsar; Timing; Loi puissance; Borne supérieure; Algorithme; Processus stochastique; Processus gaussien; Trou noir supermassif; Limite confiance; Analyse donnée; Cosmologie
ED :	Gravitational waves; Pulsars; Timing; Power law; Upper bound; Algorithms; Stochastic processes; Gaussian processes; Supermassive black hole; Confidence limit; Data analysis; Cosmology
SD :	Ley poder; Cota superior; Agujero negro supermasivo; Límite confianza
LO :	INIST-2067.354000190477460250
ID :	11-0320593

Links to Exploration step

Pascal:11-0320593

Le document en format XML

<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data</title>
<author><name sortKey="Van Haasteren, R" sort="Van Haasteren, R" uniqKey="Van Haasteren R" first="R." last="Van Haasteren">R. Van Haasteren</name>
<affiliation><inist:fA14 i1="01"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Levin, Y" sort="Levin, Y" uniqKey="Levin Y" first="Y." last="Levin">Y. Levin</name>
<affiliation><inist:fA14 i1="01"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>School of Physics, Monash University, PO Box 27</s1>
<s2>VIC 3800</s2>
<s3>AUS</s3>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Janssen, G H" sort="Janssen, G H" uniqKey="Janssen G" first="G. H." last="Janssen">G. H. Janssen</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Lazaridis, K" sort="Lazaridis, K" uniqKey="Lazaridis K" first="K." last="Lazaridis">K. Lazaridis</name>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Stappers, B W" sort="Stappers, B W" uniqKey="Stappers B" first="B. W." last="Stappers">B. W. Stappers</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Desvignes, G" sort="Desvignes, G" uniqKey="Desvignes G" first="G." last="Desvignes">G. Desvignes</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="08"><s1>Department of Astronomy and Radio Astronomy Laboratory, University of California</s1>
<s2>Berkeley, CA 94720</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Purver, M B" sort="Purver, M B" uniqKey="Purver M" first="M. B." last="Purver">M. B. Purver</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Lyne, A G" sort="Lyne, A G" uniqKey="Lyne A" first="A. G." last="Lyne">A. G. Lyne</name>
<affiliation><inist:fA14 i1="09"><s1>University ofmanchester, Jodrell Bank Observatory</s1>
<s2>Macclesfield, Cheshire, SK11 9DL</s2>
<s3>GBR</s3>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ferdman, R D" sort="Ferdman, R D" uniqKey="Ferdman R" first="R. D." last="Ferdman">R. D. Ferdman</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Jessner, A" sort="Jessner, A" uniqKey="Jessner A" first="A." last="Jessner">A. Jessner</name>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Cognard, I" sort="Cognard, I" uniqKey="Cognard I" first="I." last="Cognard">I. Cognard</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Theureau, G" sort="Theureau, G" uniqKey="Theureau G" first="G." last="Theureau">G. Theureau</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="D Amico, N" sort="D Amico, N" uniqKey="D Amico N" first="N." last="D'Amico">N. D'Amico</name>
<affiliation><inist:fA14 i1="10"><s1>Dipartimento di Fisica, Universit========Atilde; Degli Studi di Cagliari, SP Monserrato-Sestu km 0.7</s1>
<s2>90042 Monserrato (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Possenti, A" sort="Possenti, A" uniqKey="Possenti A" first="A." last="Possenti">A. Possenti</name>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Burgay, M" sort="Burgay, M" uniqKey="Burgay M" first="M." last="Burgay">M. Burgay</name>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Corongiu, A" sort="Corongiu, A" uniqKey="Corongiu A" first="A." last="Corongiu">A. Corongiu</name>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Hessels, J W T" sort="Hessels, J W T" uniqKey="Hessels J" first="J. W. T." last="Hessels">J. W. T. Hessels</name>
<affiliation><inist:fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="12"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam</s1>
<s2>1098 SJ Amsterdam</s2>
<s3>NLD</s3>
<sZ>18 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smits, R" sort="Smits, R" uniqKey="Smits R" first="R." last="Smits">R. Smits</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Verbiest, J P W" sort="Verbiest, J P W" uniqKey="Verbiest J" first="J. P. W." last="Verbiest">J. P. W. Verbiest</name>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">11-0320593</idno>
<date when="2011">2011</date>
<idno type="stanalyst">PASCAL 11-0320593 INIST</idno>
<idno type="RBID">Pascal:11-0320593</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">001B07</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data</title>
<author><name sortKey="Van Haasteren, R" sort="Van Haasteren, R" uniqKey="Van Haasteren R" first="R." last="Van Haasteren">R. Van Haasteren</name>
<affiliation><inist:fA14 i1="01"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Levin, Y" sort="Levin, Y" uniqKey="Levin Y" first="Y." last="Levin">Y. Levin</name>
<affiliation><inist:fA14 i1="01"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="02"><s1>School of Physics, Monash University, PO Box 27</s1>
<s2>VIC 3800</s2>
<s3>AUS</s3>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Janssen, G H" sort="Janssen, G H" uniqKey="Janssen G" first="G. H." last="Janssen">G. H. Janssen</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Lazaridis, K" sort="Lazaridis, K" uniqKey="Lazaridis K" first="K." last="Lazaridis">K. Lazaridis</name>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Stappers, B W" sort="Stappers, B W" uniqKey="Stappers B" first="B. W." last="Stappers">B. W. Stappers</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Desvignes, G" sort="Desvignes, G" uniqKey="Desvignes G" first="G." last="Desvignes">G. Desvignes</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="08"><s1>Department of Astronomy and Radio Astronomy Laboratory, University of California</s1>
<s2>Berkeley, CA 94720</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Purver, M B" sort="Purver, M B" uniqKey="Purver M" first="M. B." last="Purver">M. B. Purver</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Lyne, A G" sort="Lyne, A G" uniqKey="Lyne A" first="A. G." last="Lyne">A. G. Lyne</name>
<affiliation><inist:fA14 i1="09"><s1>University ofmanchester, Jodrell Bank Observatory</s1>
<s2>Macclesfield, Cheshire, SK11 9DL</s2>
<s3>GBR</s3>
<sZ>9 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ferdman, R D" sort="Ferdman, R D" uniqKey="Ferdman R" first="R. D." last="Ferdman">R. D. Ferdman</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Jessner, A" sort="Jessner, A" uniqKey="Jessner A" first="A." last="Jessner">A. Jessner</name>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Cognard, I" sort="Cognard, I" uniqKey="Cognard I" first="I." last="Cognard">I. Cognard</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Theureau, G" sort="Theureau, G" uniqKey="Theureau G" first="G." last="Theureau">G. Theureau</name>
<affiliation><inist:fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="D Amico, N" sort="D Amico, N" uniqKey="D Amico N" first="N." last="D'Amico">N. D'Amico</name>
<affiliation><inist:fA14 i1="10"><s1>Dipartimento di Fisica, Universit========Atilde; Degli Studi di Cagliari, SP Monserrato-Sestu km 0.7</s1>
<s2>90042 Monserrato (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Possenti, A" sort="Possenti, A" uniqKey="Possenti A" first="A." last="Possenti">A. Possenti</name>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Burgay, M" sort="Burgay, M" uniqKey="Burgay M" first="M." last="Burgay">M. Burgay</name>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Corongiu, A" sort="Corongiu, A" uniqKey="Corongiu A" first="A." last="Corongiu">A. Corongiu</name>
<affiliation><inist:fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Hessels, J W T" sort="Hessels, J W T" uniqKey="Hessels J" first="J. W. T." last="Hessels">J. W. T. Hessels</name>
<affiliation><inist:fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="12"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam</s1>
<s2>1098 SJ Amsterdam</s2>
<s3>NLD</s3>
<sZ>18 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smits, R" sort="Smits, R" uniqKey="Smits R" first="R." last="Smits">R. Smits</name>
<affiliation><inist:fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Verbiest, J P W" sort="Verbiest, J P W" uniqKey="Verbiest J" first="J. P. W." last="Verbiest">J. P. W. Verbiest</name>
<affiliation><inist:fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</analytic>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
<imprint><date when="2011">2011</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Algorithms</term>
<term>Confidence limit</term>
<term>Cosmology</term>
<term>Data analysis</term>
<term>Gaussian processes</term>
<term>Gravitational waves</term>
<term>Power law</term>
<term>Pulsars</term>
<term>Stochastic processes</term>
<term>Supermassive black hole</term>
<term>Timing</term>
<term>Upper bound</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Onde gravitationnelle</term>
<term>Pulsar</term>
<term>Timing</term>
<term>Loi puissance</term>
<term>Borne supérieure</term>
<term>Algorithme</term>
<term>Processus stochastique</term>
<term>Processus gaussien</term>
<term>Trou noir supermassif</term>
<term>Limite confiance</term>
<term>Analyse donnée</term>
<term>Cosmologie</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">Direct detection of low-frequency gravitational waves (GWs, 10<sup>-9</sup>
 to 10<sup>-g</sup>
 Hz) is the main goal of pulsar timing array (PTA) projects. One of the main targets for the PTAs is to measure the stochastic background of gravitational waves (GWB) whose characteristic strain is expected to approximately follow a power-law of the form h<sub>c</sub>
(f) = A(f /yr<sup>-1</sup>
)α, where f is the GW frequency. In this paper we use the current data from the European PTA to determine an upper limit on the GWB amplitude A as a function of the unknown spectral slope α with a Bayesian algorithm, by modelling the GWB as a random Gaussian process. For the case α = -2/3, which is expected if the GWB is produced by supermassive black hole binaries, we obtain a 95 per cent confidence upper limit on A of 6 x 10<sup>-15</sup>
, which is 1.8 times lower than the 95 per cent confidence GWB limit obtained by the Parkes PTA in 2006. Our approach to the data analysis incorporates the multitelescope nature of the European PTA and thus can serve as a useful template for future intercontinental PTA collaborations.</div>
</front>
</TEI>
<inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0>
</fA01>
<fA02 i1="01"><s0>MNRAA4</s0>
</fA02>
<fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0>
</fA03>
<fA05><s2>414</s2>
</fA05>
<fA06><s2>4</s2>
</fA06>
<fA08 i1="01" i2="1" l="ENG"><s1>Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>VAN HAASTEREN (R.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>LEVIN (Y.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>JANSSEN (G. H.)</s1>
</fA11>
<fA11 i1="04" i2="1"><s1>LAZARIDIS (K.)</s1>
</fA11>
<fA11 i1="05" i2="1"><s1>KRAMER (M.)</s1>
</fA11>
<fA11 i1="06" i2="1"><s1>STAPPERS (B. W.)</s1>
</fA11>
<fA11 i1="07" i2="1"><s1>DESVIGNES (G.)</s1>
</fA11>
<fA11 i1="08" i2="1"><s1>PURVER (M. B.)</s1>
</fA11>
<fA11 i1="09" i2="1"><s1>LYNE (A. G.)</s1>
</fA11>
<fA11 i1="10" i2="1"><s1>FERDMAN (R. D.)</s1>
</fA11>
<fA11 i1="11" i2="1"><s1>JESSNER (A.)</s1>
</fA11>
<fA11 i1="12" i2="1"><s1>COGNARD (I.)</s1>
</fA11>
<fA11 i1="13" i2="1"><s1>THEUREAU (G.)</s1>
</fA11>
<fA11 i1="14" i2="1"><s1>D'AMICO (N.)</s1>
</fA11>
<fA11 i1="15" i2="1"><s1>POSSENTI (A.)</s1>
</fA11>
<fA11 i1="16" i2="1"><s1>BURGAY (M.)</s1>
</fA11>
<fA11 i1="17" i2="1"><s1>CORONGIU (A.)</s1>
</fA11>
<fA11 i1="18" i2="1"><s1>HESSELS (J. W. T.)</s1>
</fA11>
<fA11 i1="19" i2="1"><s1>SMITS (R.)</s1>
</fA11>
<fA11 i1="20" i2="1"><s1>VERBIEST (J. P. W.)</s1>
</fA11>
<fA14 i1="01"><s1>Leiden Observatory, Leiden University, PO Box 9513</s1>
<s2>2300 RA Leiden</s2>
<s3>NLD</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>School of Physics, Monash University, PO Box 27</s1>
<s2>VIC 3800</s2>
<s3>AUS</s3>
<sZ>2 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>3 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
<sZ>19 aut.</sZ>
</fA14>
<fA14 i1="04"><s1>Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>4 aut.</sZ>
<sZ>5 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>20 aut.</sZ>
</fA14>
<fA14 i1="05"><s1>Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2</s1>
<s2>7990 AA Dwingeloo</s2>
<s3>NLD</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
<sZ>19 aut.</sZ>
</fA14>
<fA14 i1="06"><s1>LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique</s1>
<s2>45071 Orléans</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</fA14>
<fA14 i1="07"><s1>Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU</s1>
<s2>18330 Nançay</s2>
<s3>FRA</s3>
<sZ>7 aut.</sZ>
<sZ>10 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
</fA14>
<fA14 i1="08"><s1>Department of Astronomy and Radio Astronomy Laboratory, University of California</s1>
<s2>Berkeley, CA 94720</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
</fA14>
<fA14 i1="09"><s1>University ofmanchester, Jodrell Bank Observatory</s1>
<s2>Macclesfield, Cheshire, SK11 9DL</s2>
<s3>GBR</s3>
<sZ>9 aut.</sZ>
</fA14>
<fA14 i1="10"><s1>Dipartimento di Fisica, Universit========Atilde; Degli Studi di Cagliari, SP Monserrato-Sestu km 0.7</s1>
<s2>90042 Monserrato (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
</fA14>
<fA14 i1="11"><s1>INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54</s1>
<s2>09012 Capoterra (CA)</s2>
<s3>ITA</s3>
<sZ>14 aut.</sZ>
<sZ>15 aut.</sZ>
<sZ>16 aut.</sZ>
<sZ>17 aut.</sZ>
</fA14>
<fA14 i1="12"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam</s1>
<s2>1098 SJ Amsterdam</s2>
<s3>NLD</s3>
<sZ>18 aut.</sZ>
</fA14>
<fA20><s1>3117-3128</s1>
</fA20>
<fA21><s1>2011</s1>
</fA21>
<fA23 i1="01"><s0>ENG</s0>
</fA23>
<fA43 i1="01"><s1>INIST</s1>
<s2>2067</s2>
<s5>354000190477460250</s5>
</fA43>
<fA44><s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45><s0>1/4 p.</s0>
</fA45>
<fA47 i1="01" i2="1"><s0>11-0320593</s0>
</fA47>
<fA60><s1>P</s1>
</fA60>
<fA61><s0>A</s0>
</fA61>
<fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0>
</fA64>
<fA66 i1="01"><s0>USA</s0>
</fA66>
<fC01 i1="01" l="ENG"><s0>Direct detection of low-frequency gravitational waves (GWs, 10<sup>-9</sup>
 to 10<sup>-g</sup>
 Hz) is the main goal of pulsar timing array (PTA) projects. One of the main targets for the PTAs is to measure the stochastic background of gravitational waves (GWB) whose characteristic strain is expected to approximately follow a power-law of the form h<sub>c</sub>
(f) = A(f /yr<sup>-1</sup>
)α, where f is the GW frequency. In this paper we use the current data from the European PTA to determine an upper limit on the GWB amplitude A as a function of the unknown spectral slope α with a Bayesian algorithm, by modelling the GWB as a random Gaussian process. For the case α = -2/3, which is expected if the GWB is produced by supermassive black hole binaries, we obtain a 95 per cent confidence upper limit on A of 6 x 10<sup>-15</sup>
, which is 1.8 times lower than the 95 per cent confidence GWB limit obtained by the Parkes PTA in 2006. Our approach to the data analysis incorporates the multitelescope nature of the European PTA and thus can serve as a useful template for future intercontinental PTA collaborations.</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="3" l="FRE"><s0>Pulsar</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="3" l="ENG"><s0>Pulsars</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="3" l="FRE"><s0>Timing</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="3" l="ENG"><s0>Timing</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE"><s0>Loi puissance</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG"><s0>Power law</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA"><s0>Ley poder</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="X" l="FRE"><s0>Borne supérieure</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG"><s0>Upper bound</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Cota superior</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE"><s0>Algorithme</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG"><s0>Algorithms</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE"><s0>Processus stochastique</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG"><s0>Stochastic processes</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE"><s0>Processus gaussien</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG"><s0>Gaussian processes</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE"><s0>Trou noir supermassif</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG"><s0>Supermassive black hole</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA"><s0>Agujero negro supermasivo</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Limite confiance</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="ENG"><s0>Confidence limit</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="X" l="SPA"><s0>Límite confianza</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE"><s0>Analyse donnée</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG"><s0>Data analysis</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="3" l="FRE"><s0>Cosmologie</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="3" l="ENG"><s0>Cosmology</s0>
<s5>37</s5>
</fC03>
<fN21><s1>220</s1>
</fN21>
<fN44 i1="01"><s1>OTO</s1>
</fN44>
<fN82><s1>OTO</s1>
</fN82>
</pA>
</standard>
<server><NO>PASCAL 11-0320593 INIST</NO>
<ET>Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data</ET>
<AU>VAN HAASTEREN (R.); LEVIN (Y.); JANSSEN (G. H.); LAZARIDIS (K.); KRAMER (M.); STAPPERS (B. W.); DESVIGNES (G.); PURVER (M. B.); LYNE (A. G.); FERDMAN (R. D.); JESSNER (A.); COGNARD (I.); THEUREAU (G.); D'AMICO (N.); POSSENTI (A.); BURGAY (M.); CORONGIU (A.); HESSELS (J. W. T.); SMITS (R.); VERBIEST (J. P. W.)</AU>
<AF>Leiden Observatory, Leiden University, PO Box 9513/2300 RA Leiden/Pays-Bas (1 aut., 2 aut.); School of Physics, Monash University, PO Box 27/VIC 3800/Australie (2 aut.); University of Manchester, Jodrell Bank Centre for Astrophysics, Alan Turing Building/Manchester M13 9PL/Royaume-Uni (3 aut., 5 aut., 6 aut., 8 aut., 19 aut.); Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69/53121 Bonn/Allemagne (4 aut., 5 aut., 11 aut., 20 aut.); Netherlands Institute for Radio Astronomy (ASTRON), Postbus 2/7990 AA Dwingeloo/Pays-Bas (6 aut., 18 aut., 19 aut.); LPC2E, Université d'Orléans - CNRS, 3A Av de la Recherche Scientifique/45071 Orléans/France (7 aut., 10 aut., 12 aut., 13 aut.); Station de Radioastronomie de Nançay, Observatoire de Paris, CNRS/INSU/18330 Nançay/France (7 aut., 10 aut., 12 aut., 13 aut.); Department of Astronomy and Radio Astronomy Laboratory, University of California/Berkeley, CA 94720/Etats-Unis (7 aut.); University ofmanchester, Jodrell Bank Observatory/Macclesfield, Cheshire, SK11 9DL/Royaume-Uni (9 aut.); Dipartimento di Fisica, Universit========Atilde; Degli Studi di Cagliari, SP Monserrato-Sestu km 0.7/90042 Monserrato (CA)/Italie (14 aut.); INAF Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Strada 54/09012 Capoterra (CA)/Italie (14 aut., 15 aut., 16 aut., 17 aut.); Astronomical Institute 'Anton Pannekoek', University of Amsterdam/1098 SJ Amsterdam/Pays-Bas (18 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 4; Pp. 3117-3128; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>Direct detection of low-frequency gravitational waves (GWs, 10<sup>-9</sup>
 to 10<sup>-g</sup>
 Hz) is the main goal of pulsar timing array (PTA) projects. One of the main targets for the PTAs is to measure the stochastic background of gravitational waves (GWB) whose characteristic strain is expected to approximately follow a power-law of the form h<sub>c</sub>
(f) = A(f /yr<sup>-1</sup>
)α, where f is the GW frequency. In this paper we use the current data from the European PTA to determine an upper limit on the GWB amplitude A as a function of the unknown spectral slope α with a Bayesian algorithm, by modelling the GWB as a random Gaussian process. For the case α = -2/3, which is expected if the GWB is produced by supermassive black hole binaries, we obtain a 95 per cent confidence upper limit on A of 6 x 10<sup>-15</sup>
, which is 1.8 times lower than the 95 per cent confidence GWB limit obtained by the Parkes PTA in 2006. Our approach to the data analysis incorporates the multitelescope nature of the European PTA and thus can serve as a useful template for future intercontinental PTA collaborations.</EA>
<CC>001E03</CC>
<FD>Onde gravitationnelle; Pulsar; Timing; Loi puissance; Borne supérieure; Algorithme; Processus stochastique; Processus gaussien; Trou noir supermassif; Limite confiance; Analyse donnée; Cosmologie</FD>
<ED>Gravitational waves; Pulsars; Timing; Power law; Upper bound; Algorithms; Stochastic processes; Gaussian processes; Supermassive black hole; Confidence limit; Data analysis; Cosmology</ED>
<SD>Ley poder; Cota superior; Agujero negro supermasivo; Límite confianza</SD>
<LO>INIST-2067.354000190477460250</LO>
<ID>11-0320593</ID>
</server>
</inist>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Corpus

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 001B07 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Corpus/biblio.hfd -nk 001B07 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    PascalFrancis
   |étape=   Corpus
   |type=    RBID
   |clé=     Pascal:11-0320593
   |texte=   Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data

Placing limits on the stochastic gravitational-wave background using European Pulsar Timing Array data

Source :

Descripteurs français

English descriptors

Abstract

Notice en format standard (ISO 2709)

Format Inist (serveur)

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri