Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357-6429 with Fermi and XMM-Newton
Identifieur interne : 006B88 ( Main/Curation ); précédent : 006B87; suivant : 006B89Discovery of gamma- and X-ray pulsations from the young and energetic PSR J1357-6429 with Fermi and XMM-Newton
Auteurs : M. Lemoine-Goumard [France] ; V. E. Zavlin [États-Unis] ; M.-H. Grondin [Allemagne] ; R. Shannon [Australie] ; D. A. Smith [France] ; M. Burgay [Italie] ; F. Camilo [États-Unis] ; J. Cohen- Tanugi [France] ; P. C. C. Freire [Allemagne] ; J. E. Grove [États-Unis] ; L. Guillemot [Allemagne] ; S. Johnston [Australie] ; M. Keith [Australie] ; M. Kramer [Allemagne, Royaume-Uni] ; R. N. Manchester [Australie] ; P. F. Michelson [États-Unis] ; D. Parent [États-Unis] ; A. Possenti [Italie] ; P. S. Ray [États-Unis] ; M. Renaud [France] ; S. E. Thorsett [États-Unis] ; P. Weltevrede [Royaume-Uni] ; M. T. Wolff [États-Unis]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2011.
Descripteurs français
- Pascal (Inist)
- Rayonnement gamma, Pulsation RX, Energétique, Pulsar, Plan galactique, Timing, Très haute énergie, Source étendue, Etoile neutron, Emission neutron, Modélisation, Courbe lumière, Analyse spectrale, Loi puissance, Spectre RX, Borne supérieure, Emission gamma, Niveau Fermi, Transfert énergie, Luminosité, Domaine énergie TeV.
English descriptors
- KwdEn :
Abstract
Context. Since the launch of the Fermi satellite, the number of known gamma-ray pulsars has increased tenfold. Most gamma-ray detected pulsars are young and energetic, and many are associated with TeV sources. PSR J 1357-6429 is a high spin-down power pulsar (E = 3.1 × 1036 erg s-1), discovered during the Parkes multibeam survey of the Galactic plane, with significant timing noise typical of very young pulsars. In the very-high-energy domain (E > 100 GeV), H.E.S.S. has reported the detection of the extended source HESS J 1356-645 (intrinsic Gaussian width of 12') whose centroid lies 7' from PSR J 1357-6429. Aims. We search for gamma- and X-ray pulsations from this pulsar, characterize the neutron star emission and explore the environment of PSR J 1357-6429. Methods. Using a rotational ephemeris obtained with 74 observations made with the Parkes telescope at 1.4 GHz, we phase-fold more than two years of gamma-ray data acquired by the Large Area Telescope on-board Fermi as well as those collected with XMM-Newton, and perform gamma-ray spectral modeling. Results. Significant gamma- and X-ray pulsations are detected from PSR J1357-6429. The light curve in both bands shows one broad peak. Gamma-ray spectral analysis of the pulsed emission suggests that it is well described by a simple power-law of index 1.5 ± 0.3stat ± 0.3syst with an exponential cut-off at 0.8 ± 0.3stat ± 0.3syst GeV and an integral photon flux above 100 MeV of (6.5 ± 1.6stat ± 2.3sysc) x 10-8 cm-2 s-1. The X-ray spectra obtained from the new data provide results consistent with previous work. Upper limits on the gamma-ray emission from its potential pulsar wind nebula (PWN) are also reported. Conclusions. Assuming a distance of 2.4 kpc, the Fermi LAT energy flux yields a gamma-ray luminosity for PSR J1357-6429 of Lγ = (2.13 ± 0.25stat ± 0.83syst) x 1034 erg s-1, consistent with an Lγ √E========dot; relationship. The Fermi non-detection of the pulsar wind nebula associated with HESS J 1356-645 provides new constraints on the electron population responsible for the extended TeV emission.
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Pascal:12-0012757Le document en format XML
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<author><name sortKey="Smith, D A" sort="Smith, D A" uniqKey="Smith D" first="D. A." last="Smith">D. A. Smith</name>
<affiliation wicri:level="1"><inist:fA14 i1="01"><s1>Université Bordeaux 1, CNRS/IN2P3, Centre d'Études Nucléaires de Bordeaux Gradignan</s1>
<s2>33175 Gradignan</s2>
<s3>FRA</s3>
<sZ>1 aut.</sZ>
<sZ>5 aut.</sZ>
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<country>France</country>
<wicri:noRegion>33175 Gradignan</wicri:noRegion>
<wicri:noRegion>Centre d'Études Nucléaires de Bordeaux Gradignan</wicri:noRegion>
<wicri:noRegion>33175 Gradignan</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Burgay, M" sort="Burgay, M" uniqKey="Burgay M" first="M." last="Burgay">M. Burgay</name>
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<s2>New York, NY 10027</s2>
<s3>USA</s3>
<sZ>7 aut.</sZ>
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<author><name sortKey="Cohen Tanugi, J" sort="Cohen Tanugi, J" uniqKey="Cohen Tanugi J" first="J." last="Cohen- Tanugi">J. Cohen- Tanugi</name>
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<author><name sortKey="Freire, P C C" sort="Freire, P C C" uniqKey="Freire P" first="P. C. C." last="Freire">P. C. C. Freire</name>
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<author><name sortKey="Grove, J E" sort="Grove, J E" uniqKey="Grove J" first="J. E." last="Grove">J. E. Grove</name>
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<s2>Washington, DC 20375</s2>
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<author><name sortKey="Guillemot, L" sort="Guillemot, L" uniqKey="Guillemot L" first="L." last="Guillemot">L. Guillemot</name>
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<s2>53121 Bonn</s2>
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<settlement type="city">Bonn</settlement>
</placeName>
</affiliation>
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<author><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>CSIRO Astronomy and Space Science, Australia Telescope National Facility</s1>
<s2>Epping NSW 1710</s2>
<s3>AUS</s3>
<sZ>4 aut.</sZ>
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<country>Australie</country>
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<author><name sortKey="Keith, M" sort="Keith, M" uniqKey="Keith M" first="M." last="Keith">M. Keith</name>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>CSIRO Astronomy and Space Science, Australia Telescope National Facility</s1>
<s2>Epping NSW 1710</s2>
<s3>AUS</s3>
<sZ>4 aut.</sZ>
<sZ>12 aut.</sZ>
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<country>Australie</country>
<wicri:noRegion>Epping NSW 1710</wicri:noRegion>
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<author><name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
<affiliation wicri:level="3"><inist:fA14 i1="08"><s1>Max-Planck-Institut fur Radioastronomie, Auf dem Hügel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>9 aut.</sZ>
<sZ>11 aut.</sZ>
<sZ>14 aut.</sZ>
</inist:fA14>
<country>Allemagne</country>
<placeName><region type="land" nuts="1">Rhénanie-du-Nord-Westphalie</region>
<region type="district" nuts="2">District de Cologne</region>
<settlement type="city">Bonn</settlement>
</placeName>
</affiliation>
<affiliation wicri:level="4"><inist:fA14 i1="10"><s1>Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester</s1>
<s2>M13 9PL</s2>
<s3>GBR</s3>
<sZ>14 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
<country>Royaume-Uni</country>
<placeName><settlement type="city">Manchester</settlement>
<region type="nation">Angleterre</region>
<region nuts="2" type="region">Grand Manchester</region>
</placeName>
<orgName type="university">Université de Manchester</orgName>
</affiliation>
</author>
<author><name sortKey="Manchester, R N" sort="Manchester, R N" uniqKey="Manchester R" first="R. N." last="Manchester">R. N. Manchester</name>
<affiliation wicri:level="1"><inist:fA14 i1="04"><s1>CSIRO Astronomy and Space Science, Australia Telescope National Facility</s1>
<s2>Epping NSW 1710</s2>
<s3>AUS</s3>
<sZ>4 aut.</sZ>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>15 aut.</sZ>
</inist:fA14>
<country>Australie</country>
<wicri:noRegion>Epping NSW 1710</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Michelson, P F" sort="Michelson, P F" uniqKey="Michelson P" first="P. F." last="Michelson">P. F. Michelson</name>
<affiliation wicri:level="1"><inist:fA14 i1="11"><s1>W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University</s1>
<s2>Stanford, CA 94305</s2>
<s3>USA</s3>
<sZ>16 aut.</sZ>
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<country>États-Unis</country>
<wicri:noRegion>Stanford, CA 94305</wicri:noRegion>
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<author><name sortKey="Parent, D" sort="Parent, D" uniqKey="Parent D" first="D." last="Parent">D. Parent</name>
<affiliation wicri:level="1"><inist:fA14 i1="12"><s1>Center for Earth Observing and Space Research, College of Science, George Mason University, Fairfax, VA 22030, resident at Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>17 aut.</sZ>
</inist:fA14>
<country>États-Unis</country>
<wicri:noRegion>Washington, DC 20375</wicri:noRegion>
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<author><name sortKey="Possenti, A" sort="Possenti, A" uniqKey="Possenti A" first="A." last="Possenti">A. Possenti</name>
<affiliation wicri:level="1"><inist:fA14 i1="05"><s1>INAF - Cagliari Astronomical Observatory</s1>
<s2>09012 Capoterra (CA</s2>
<s3>ITA</s3>
<sZ>6 aut.</sZ>
<sZ>18 aut.</sZ>
</inist:fA14>
<country>Italie</country>
<wicri:noRegion>INAF - Cagliari Astronomical Observatory</wicri:noRegion>
</affiliation>
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<author><name sortKey="Ray, P S" sort="Ray, P S" uniqKey="Ray P" first="P. S." last="Ray">P. S. Ray</name>
<affiliation wicri:level="1"><inist:fA14 i1="09"><s1>High Energy Space Environment Branch, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>23 aut.</sZ>
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<country>États-Unis</country>
<wicri:noRegion>Washington, DC 20375</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Renaud, M" sort="Renaud, M" uniqKey="Renaud M" first="M." last="Renaud">M. Renaud</name>
<affiliation wicri:level="3"><inist:fA14 i1="07"><s1>Laboratoire Univers et Particules de Montpellier, Université Montpellier 2, CNRS/IN2P3</s1>
<s2>Montpellier</s2>
<s3>FRA</s3>
<sZ>8 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
<country>France</country>
<placeName><region type="region">Occitanie (région administrative)</region>
<region type="old region">Languedoc-Roussillon</region>
<settlement type="city">Montpellier</settlement>
</placeName>
</affiliation>
</author>
<author><name sortKey="Thorsett, S E" sort="Thorsett, S E" uniqKey="Thorsett S" first="S. E." last="Thorsett">S. E. Thorsett</name>
<affiliation wicri:level="1"><inist:fA14 i1="13"><s1>Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz</s1>
<s2>Santa Cruz, CA 95064</s2>
<s3>USA</s3>
<sZ>21 aut.</sZ>
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<country>États-Unis</country>
<wicri:noRegion>Santa Cruz, CA 95064</wicri:noRegion>
</affiliation>
</author>
<author><name sortKey="Weltevrede, P" sort="Weltevrede, P" uniqKey="Weltevrede P" first="P." last="Weltevrede">P. Weltevrede</name>
<affiliation wicri:level="4"><inist:fA14 i1="10"><s1>Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester</s1>
<s2>M13 9PL</s2>
<s3>GBR</s3>
<sZ>14 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
<country>Royaume-Uni</country>
<placeName><settlement type="city">Manchester</settlement>
<region type="nation">Angleterre</region>
<region nuts="2" type="region">Grand Manchester</region>
</placeName>
<orgName type="university">Université de Manchester</orgName>
</affiliation>
</author>
<author><name sortKey="Wolff, M T" sort="Wolff, M T" uniqKey="Wolff M" first="M. T." last="Wolff">M. T. Wolff</name>
<affiliation wicri:level="1"><inist:fA14 i1="09"><s1>High Energy Space Environment Branch, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>10 aut.</sZ>
<sZ>19 aut.</sZ>
<sZ>23 aut.</sZ>
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<country>États-Unis</country>
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<series><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title>
<title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title>
<idno type="ISSN">0004-6361</idno>
<imprint><date when="2011">2011</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><title level="j" type="main">Astronomy and astrophysics : (Berlin. Print)</title>
<title level="j" type="abbreviated">Astron. astrophys. : (Berl., Print)</title>
<idno type="ISSN">0004-6361</idno>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Energetics</term>
<term>Energy transfer</term>
<term>Extended source</term>
<term>Fermi level</term>
<term>Galactic planes</term>
<term>Gamma emission</term>
<term>Gamma radiation</term>
<term>Light curves</term>
<term>Luminosity</term>
<term>Modelling</term>
<term>Neutron emission</term>
<term>Neutron stars</term>
<term>Power law</term>
<term>Pulsars</term>
<term>Spectral analysis</term>
<term>TeV range</term>
<term>Timing</term>
<term>Upper bound</term>
<term>Very high energy</term>
<term>X ray pulsation</term>
<term>X-ray spectra</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr"><term>Rayonnement gamma</term>
<term>Pulsation RX</term>
<term>Energétique</term>
<term>Pulsar</term>
<term>Plan galactique</term>
<term>Timing</term>
<term>Très haute énergie</term>
<term>Source étendue</term>
<term>Etoile neutron</term>
<term>Emission neutron</term>
<term>Modélisation</term>
<term>Courbe lumière</term>
<term>Analyse spectrale</term>
<term>Loi puissance</term>
<term>Spectre RX</term>
<term>Borne supérieure</term>
<term>Emission gamma</term>
<term>Niveau Fermi</term>
<term>Transfert énergie</term>
<term>Luminosité</term>
<term>Domaine énergie TeV</term>
</keywords>
</textClass>
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</teiHeader>
<front><div type="abstract" xml:lang="en">Context. Since the launch of the Fermi satellite, the number of known gamma-ray pulsars has increased tenfold. Most gamma-ray detected pulsars are young and energetic, and many are associated with TeV sources. PSR J 1357-6429 is a high spin-down power pulsar (E = 3.1 × 10<sup>36</sup>
erg s<sup>-1</sup>
), discovered during the Parkes multibeam survey of the Galactic plane, with significant timing noise typical of very young pulsars. In the very-high-energy domain (E > 100 GeV), H.E.S.S. has reported the detection of the extended source HESS J 1356-645 (intrinsic Gaussian width of 12') whose centroid lies 7' from PSR J 1357-6429. Aims. We search for gamma- and X-ray pulsations from this pulsar, characterize the neutron star emission and explore the environment of PSR J 1357-6429. Methods. Using a rotational ephemeris obtained with 74 observations made with the Parkes telescope at 1.4 GHz, we phase-fold more than two years of gamma-ray data acquired by the Large Area Telescope on-board Fermi as well as those collected with XMM-Newton, and perform gamma-ray spectral modeling. Results. Significant gamma- and X-ray pulsations are detected from PSR J1357-6429. The light curve in both bands shows one broad peak. Gamma-ray spectral analysis of the pulsed emission suggests that it is well described by a simple power-law of index 1.5 ± 0.3<sub>stat</sub>
± 0.3<sub>syst</sub>
with an exponential cut-off at 0.8 ± 0.3<sub>stat</sub>
± 0.3<sub>syst</sub>
GeV and an integral photon flux above 100 MeV of (6.5 ± 1.6<sub>stat</sub>
± 2.3<sub>sysc</sub>
) x 10<sup>-8</sup>
cm<sup>-</sup>
2 s<sup>-1</sup>
. The X-ray spectra obtained from the new data provide results consistent with previous work. Upper limits on the gamma-ray emission from its potential pulsar wind nebula (PWN) are also reported. Conclusions. Assuming a distance of 2.4 kpc, the Fermi LAT energy flux yields a gamma-ray luminosity for PSR J1357-6429 of L<sub>γ</sub>
= (2.13 ± 0.25<sub>stat</sub>
± 0.83<sub>syst</sub>
) x 10<sup>34</sup>
erg s<sup>-1</sup>
, consistent with an Lγ √E========dot; relationship. The Fermi non-detection of the pulsar wind nebula associated with HESS J 1356-645 provides new constraints on the electron population responsible for the extended TeV emission.</div>
</front>
</TEI>
</record>
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