Discovery of two millisecond pulsars in Fermi sources with the Nancay Radio Telescope
Identifieur interne : 000567 ( Hal/Checkpoint ); précédent : 000566; suivant : 000568Discovery of two millisecond pulsars in Fermi sources with the Nancay Radio Telescope
Auteurs : Ismaël Cognard [France] ; L. Guillemot ; T. J. Johnson ; D. A. Smith [France] ; C. Venter ; A. K. Harding ; M. T. Wolff ; C. C. Cheung ; D. Donato ; A. A. Abdo ; J. Ballet [France] ; F. Camilo ; G. Desvignes ; D. Dumora [France] ; E. C. Ferrara ; P. C. C. Freire ; J. E. Grove ; S. Johnston ; M. Keith ; M. Kramer ; A. G. Lyne ; P. F. Michelson ; D. Parent ; S. M. Ransom ; P. S. Ray ; R. W. Romani ; P. M. Saz Parkinson ; B. W. Stappers ; Gilles Theureau [France] ; D. J. Thompson ; P. Weltevrede ; K. S. WoodSource :
- Astrophysical Journal [ 0004-637X ] ; 2011-05-01.
Abstract
We report the discovery of two millisecond pulsars in a search for radio pulsations at the positions of \emph{Fermi Large Area Telescope} sources with no previously known counterparts, using the Nançay radio telescope. The two millisecond pulsars, PSRs J2017+0603 and J2302+4442, have rotational periods of 2.896 and 5.192 ms and are both in binary systems with low-eccentricity orbits and orbital periods of 2.2 and 125.9 days respectively, suggesting long recycling processes. Gamma-ray pulsations were subsequently detected for both objects, indicating that they power the associated \emph{Fermi} sources in which they were found. The gamma-ray light curves and spectral properties are similar to those of previously-detected gamma-ray millisecond pulsars. Detailed modeling of the observed radio and gamma-ray light curves shows that the gamma-ray emission seems to originate at high altitudes in their magnetospheres. Additionally, X-ray observations revealed the presence of an X-ray source at the position of PSR J2302+4442, consistent with thermal emission from a neutron star. These discoveries along with the numerous detections of radio-loud millisecond pulsars in gamma rays suggest that many \emph{Fermi} sources with no known counterpart could be unknown millisecond pulsars.
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DOI: 10.1088/0004-637X/732/1/47
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Hal:in2p3-00605514Le document en format XML
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<author><name sortKey="Thompson, D J" sort="Thompson, D J" uniqKey="Thompson D" first="D. J." last="Thompson">D. J. Thompson</name>
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<idno type="DOI">10.1088/0004-637X/732/1/47</idno>
<series><title level="j">Astrophysical Journal</title>
<idno type="ISSN">0004-637X</idno>
<imprint><date type="datePub">2011-05-01</date>
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<profileDesc><textClass><keywords scheme="mix" xml:lang="id"><term>J2302+4442)</term>
<term>gamma rays: general</term>
<term>pulsars: general</term>
<term>pulsars: individual (J2017+0603</term>
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<front><div type="abstract" xml:lang="en">We report the discovery of two millisecond pulsars in a search for radio pulsations at the positions of \emph{Fermi Large Area Telescope} sources with no previously known counterparts, using the Nançay radio telescope. The two millisecond pulsars, PSRs J2017+0603 and J2302+4442, have rotational periods of 2.896 and 5.192 ms and are both in binary systems with low-eccentricity orbits and orbital periods of 2.2 and 125.9 days respectively, suggesting long recycling processes. Gamma-ray pulsations were subsequently detected for both objects, indicating that they power the associated \emph{Fermi} sources in which they were found. The gamma-ray light curves and spectral properties are similar to those of previously-detected gamma-ray millisecond pulsars. Detailed modeling of the observed radio and gamma-ray light curves shows that the gamma-ray emission seems to originate at high altitudes in their magnetospheres. Additionally, X-ray observations revealed the presence of an X-ray source at the position of PSR J2302+4442, consistent with thermal emission from a neutron star. These discoveries along with the numerous detections of radio-loud millisecond pulsars in gamma rays suggest that many \emph{Fermi} sources with no known counterpart could be unknown millisecond pulsars.</div>
</front>
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<hal api="V3"> <titleStmt> <title xml:lang="en">Discovery of two millisecond pulsars in Fermi sources with the Nancay Radio Telescope</title>
<author role="aut"> <persName> <forename type="first">Ismaël</forename>
<surname>Cognard</surname>
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<author role="aut"> <persName> <forename type="first">L.</forename>
<surname>Guillemot</surname>
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<idno type="halauthorid">38579</idno>
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<author role="aut"> <persName> <forename type="first">T. J.</forename>
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<author role="aut"> <persName> <forename type="first">D. A.</forename>
<surname>Smith</surname>
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<author role="aut"> <persName> <forename type="first">C.</forename>
<surname>Venter</surname>
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<author role="aut"> <persName> <forename type="first">A. K.</forename>
<surname>Harding</surname>
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<author role="aut"> <persName> <forename type="first">M. T.</forename>
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<author role="aut"> <persName> <forename type="first">C. C.</forename>
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<author role="aut"> <persName> <forename type="first">D.</forename>
<surname>Donato</surname>
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<author role="aut"> <persName> <forename type="first">A.A.</forename>
<surname>Abdo</surname>
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<idno type="halauthorid">398530</idno>
</author>
<author role="aut"> <persName> <forename type="first">J.</forename>
<surname>Ballet</surname>
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<idno type="halauthorid">3286</idno>
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</author>
<author role="aut"> <persName> <forename type="first">F.</forename>
<surname>Camilo</surname>
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<idno type="halauthorid">367619</idno>
</author>
<author role="aut"> <persName> <forename type="first">G.</forename>
<surname>Desvignes</surname>
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<author role="aut"> <persName> <forename type="first">D.</forename>
<surname>Dumora</surname>
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<idno type="halauthorid">9055</idno>
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</author>
<author role="aut"> <persName> <forename type="first">E. C.</forename>
<surname>Ferrara</surname>
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<idno type="halauthorid">599612</idno>
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<author role="aut"> <persName> <forename type="first">P. C. C.</forename>
<surname>Freire</surname>
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<idno type="halauthorid">367621</idno>
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<author role="aut"> <persName> <forename type="first">J. E.</forename>
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<author role="aut"> <persName> <forename type="first">M.</forename>
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<author role="aut"> <persName> <forename type="first">A. G.</forename>
<surname>Lyne</surname>
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<idno type="halauthorid">367627</idno>
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<author role="aut"> <persName> <forename type="first">P. F.</forename>
<surname>Michelson</surname>
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<idno type="halauthorid">398988</idno>
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<author role="aut"> <persName> <forename type="first">D.</forename>
<surname>Parent</surname>
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<author role="aut"> <persName> <forename type="first">S. M.</forename>
<surname>Ransom</surname>
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<author role="aut"> <persName> <forename type="first">P. S.</forename>
<surname>Ray</surname>
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<author role="aut"> <persName> <forename type="first">R. W.</forename>
<surname>Romani</surname>
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<author role="aut"> <persName> <forename type="first">P. M. Saz</forename>
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<author role="aut"> <persName> <forename type="first">B. W.</forename>
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<author role="aut"> <persName> <forename type="first">Gilles</forename>
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<author role="aut"> <persName> <forename type="first">D. J.</forename>
<surname>Thompson</surname>
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<author role="aut"> <persName> <forename type="first">P.</forename>
<surname>Weltevrede</surname>
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<author role="aut"> <persName> <forename type="first">K. S.</forename>
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<editor role="depositor"> <persName> <forename>Virginie</forename>
<surname>Mas</surname>
</persName>
<email type="md5">fb11fe81890fd082ebcff2349d972171</email>
<email type="domain">cenbg.in2p3.fr</email>
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<date type="whenReleased">2011-07-04 06:46:04</date>
<date type="whenProduced">2011-05-01</date>
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<respStmt> <resp>contributor</resp>
<name key="136365"> <persName> <forename>Virginie</forename>
<surname>Mas</surname>
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<email type="domain">cenbg.in2p3.fr</email>
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<idno type="halRefHtml">Astrophysical Journal, American Astronomical Society, 2011, 732, pp.47. <10.1088/0004-637X/732/1/47></idno>
<idno type="halRef">Astrophysical Journal, American Astronomical Society, 2011, 732, pp.47. <10.1088/0004-637X/732/1/47></idno>
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<seriesStmt> <idno type="stamp" n="IN2P3">Institut National de Physique Nucléaire et de Physique des Particules</idno>
<idno type="stamp" n="CEA">CEA - Commissariat à l'énergie atomique</idno>
<idno type="stamp" n="INSU">INSU - Institut National des Sciences de l'Univers</idno>
<idno type="stamp" n="CENBG">Centre d'Etudes Nucléaires de Bordeaux Gradignan</idno>
<idno type="stamp" n="CNRS">CNRS - Centre national de la recherche scientifique</idno>
<idno type="stamp" n="UNIV-ORLEANS">Université d'Orléans</idno>
<idno type="stamp" n="OSUC" p="INSU">Observatoire des Sciences de l'Univers en région Centre</idno>
<idno type="stamp" n="UNIV-PARIS7">Université Denis Diderot - Paris VII</idno>
<idno type="stamp" n="LPC2E" p="INSU">Laboratoire de Physique et Chimie de l'Environnement et de l'Espace</idno>
<idno type="stamp" n="USPC">Université Sorbonne Paris Cité</idno>
</seriesStmt>
<notesStmt> <note type="commentary">26 pages, 7 figures, accepted for publication in ApJ</note>
<note type="audience" n="1">Not set</note>
<note type="popular" n="0">No</note>
<note type="peer" n="1">Yes</note>
</notesStmt>
<sourceDesc> <biblStruct> <analytic> <title xml:lang="en">Discovery of two millisecond pulsars in Fermi sources with the Nancay Radio Telescope</title>
<author role="aut"> <persName> <forename type="first">Ismaël</forename>
<surname>Cognard</surname>
</persName>
<email type="md5">f1a09cf21128b4f297fd54ff5611b719</email>
<email type="domain">cnrs-orleans.fr</email>
<idno type="halauthorid">1144034</idno>
<affiliation ref="#struct-833"></affiliation>
</author>
<author role="aut"> <persName> <forename type="first">L.</forename>
<surname>Guillemot</surname>
</persName>
<idno type="halauthorid">38579</idno>
</author>
<author role="aut"> <persName> <forename type="first">T. J.</forename>
<surname>Johnson</surname>
</persName>
<idno type="halauthorid">327493</idno>
</author>
<author role="aut"> <persName> <forename type="first">D. A.</forename>
<surname>Smith</surname>
</persName>
<idno type="halauthorid">348219</idno>
<affiliation ref="#struct-121"></affiliation>
</author>
<author role="aut"> <persName> <forename type="first">C.</forename>
<surname>Venter</surname>
</persName>
<idno type="halauthorid">49474</idno>
</author>
<author role="aut"> <persName> <forename type="first">A. K.</forename>
<surname>Harding</surname>
</persName>
<idno type="halauthorid">367623</idno>
</author>
<author role="aut"> <persName> <forename type="first">M. T.</forename>
<surname>Wolff</surname>
</persName>
<idno type="halauthorid">599613</idno>
</author>
<author role="aut"> <persName> <forename type="first">C. C.</forename>
<surname>Cheung</surname>
</persName>
<idno type="halauthorid">398960</idno>
</author>
<author role="aut"> <persName> <forename type="first">D.</forename>
<surname>Donato</surname>
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<idno type="halauthorid">398531</idno>
</author>
<author role="aut"> <persName> <forename type="first">A.A.</forename>
<surname>Abdo</surname>
</persName>
<idno type="halauthorid">398530</idno>
</author>
<author role="aut"> <persName> <forename type="first">J.</forename>
<surname>Ballet</surname>
</persName>
<idno type="halauthorid">3286</idno>
<affiliation ref="#struct-2068"></affiliation>
</author>
<author role="aut"> <persName> <forename type="first">F.</forename>
<surname>Camilo</surname>
</persName>
<idno type="halauthorid">367619</idno>
</author>
<author role="aut"> <persName> <forename type="first">G.</forename>
<surname>Desvignes</surname>
</persName>
<idno type="halauthorid">419562</idno>
</author>
<author role="aut"> <persName> <forename type="first">D.</forename>
<surname>Dumora</surname>
</persName>
<idno type="halauthorid">9055</idno>
<affiliation ref="#struct-121"></affiliation>
</author>
<author role="aut"> <persName> <forename type="first">E. C.</forename>
<surname>Ferrara</surname>
</persName>
<idno type="halauthorid">599612</idno>
</author>
<author role="aut"> <persName> <forename type="first">P. C. C.</forename>
<surname>Freire</surname>
</persName>
<idno type="halauthorid">367621</idno>
</author>
<author role="aut"> <persName> <forename type="first">J. E.</forename>
<surname>Grove</surname>
</persName>
<idno type="halauthorid">230831</idno>
</author>
<author role="aut"> <persName> <forename type="first">S.</forename>
<surname>Johnston</surname>
</persName>
<idno type="halauthorid">62894</idno>
</author>
<author role="aut"> <persName> <forename type="first">M.</forename>
<surname>Keith</surname>
</persName>
<idno type="halauthorid">398539</idno>
</author>
<author role="aut"> <persName> <forename type="first">M.</forename>
<surname>Kramer</surname>
</persName>
<idno type="halauthorid">12569</idno>
</author>
<author role="aut"> <persName> <forename type="first">A. G.</forename>
<surname>Lyne</surname>
</persName>
<idno type="halauthorid">367627</idno>
</author>
<author role="aut"> <persName> <forename type="first">P. F.</forename>
<surname>Michelson</surname>
</persName>
<idno type="halauthorid">398988</idno>
</author>
<author role="aut"> <persName> <forename type="first">D.</forename>
<surname>Parent</surname>
</persName>
<idno type="halauthorid">350327</idno>
</author>
<author role="aut"> <persName> <forename type="first">S. M.</forename>
<surname>Ransom</surname>
</persName>
<idno type="halauthorid">367631</idno>
</author>
<author role="aut"> <persName> <forename type="first">P. S.</forename>
<surname>Ray</surname>
</persName>
<idno type="halauthorid">374251</idno>
</author>
<author role="aut"> <persName> <forename type="first">R. W.</forename>
<surname>Romani</surname>
</persName>
<idno type="halauthorid">367633</idno>
</author>
<author role="aut"> <persName> <forename type="first">P. M. Saz</forename>
<surname>Parkinson</surname>
</persName>
<idno type="halauthorid">399007</idno>
</author>
<author role="aut"> <persName> <forename type="first">B. W.</forename>
<surname>Stappers</surname>
</persName>
<idno type="halauthorid">367634</idno>
</author>
<author role="aut"> <persName> <forename type="first">Gilles</forename>
<surname>Theureau</surname>
</persName>
<idno type="halauthorid">666628</idno>
<affiliation ref="#struct-833"></affiliation>
</author>
<author role="aut"> <persName> <forename type="first">D. J.</forename>
<surname>Thompson</surname>
</persName>
<idno type="halauthorid">162273</idno>
</author>
<author role="aut"> <persName> <forename type="first">P.</forename>
<surname>Weltevrede</surname>
</persName>
<idno type="halauthorid">367636</idno>
</author>
<author role="aut"> <persName> <forename type="first">K. S.</forename>
<surname>Wood</surname>
</persName>
<idno type="halauthorid">399030</idno>
</author>
</analytic>
<monogr> <idno type="halJournalId" status="VALID">3257</idno>
<idno type="issn">0004-637X</idno>
<title level="j">Astrophysical Journal</title>
<imprint> <publisher>American Astronomical Society</publisher>
<biblScope unit="volume">732</biblScope>
<biblScope unit="pp">47</biblScope>
<date type="datePub">2011-05-01</date>
</imprint>
</monogr>
<idno type="doi">10.1088/0004-637X/732/1/47</idno>
<idno type="arxiv">1102.4192</idno>
</biblStruct>
</sourceDesc>
<profileDesc> <langUsage> <language ident="en">English</language>
</langUsage>
<textClass> <keywords scheme="author"> <term xml:lang="id">J2302+4442)</term>
<term xml:lang="id">gamma rays: general</term>
<term xml:lang="id">pulsars: general</term>
<term xml:lang="id">pulsars: individual (J2017+0603</term>
</keywords>
<classCode scheme="classification">97.60.Gb Pulsars 95.85.Bh Radio, microwave (>1 mm) 97.10.Sj Pulsations, oscillations, and stellar seismology 98.70.Rz &ggr;-ray sources; &ggr;-ray bursts 97.60.Jd Neutron stars</classCode>
<classCode scheme="halDomain" n="phys.astr.he">Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]</classCode>
<classCode scheme="halDomain" n="sdu.astr.he">Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE]</classCode>
<classCode scheme="halTypology" n="ART">Journal articles</classCode>
</textClass>
<abstract xml:lang="en">We report the discovery of two millisecond pulsars in a search for radio pulsations at the positions of \emph{Fermi Large Area Telescope} sources with no previously known counterparts, using the Nançay radio telescope. The two millisecond pulsars, PSRs J2017+0603 and J2302+4442, have rotational periods of 2.896 and 5.192 ms and are both in binary systems with low-eccentricity orbits and orbital periods of 2.2 and 125.9 days respectively, suggesting long recycling processes. Gamma-ray pulsations were subsequently detected for both objects, indicating that they power the associated \emph{Fermi} sources in which they were found. The gamma-ray light curves and spectral properties are similar to those of previously-detected gamma-ray millisecond pulsars. Detailed modeling of the observed radio and gamma-ray light curves shows that the gamma-ray emission seems to originate at high altitudes in their magnetospheres. Additionally, X-ray observations revealed the presence of an X-ray source at the position of PSR J2302+4442, consistent with thermal emission from a neutron star. These discoveries along with the numerous detections of radio-loud millisecond pulsars in gamma rays suggest that many \emph{Fermi} sources with no known counterpart could be unknown millisecond pulsars.</abstract>
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