Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17498-2921
Identifieur interne : 005902 ( Main/Exploration ); précédent : 005901; suivant : 005903Spectral and timing properties of the accreting X-ray millisecond pulsar IGR J17498-2921
Auteurs : M. Falanga [Suisse] ; L. Kuiper [Pays-Bas] ; J. Poutanen [Finlande] ; D. K. Galloway [Australie] ; E. Bozzo [Suisse] ; A. Goldwurm [France] ; W. Hermsen [Pays-Bas] ; L. Stella [Italie]Source :
- Astronomy and astrophysics : (Berlin. Print) [ 0004-6361 ] ; 2012.
Descripteurs français
- Pascal (Inist)
- Propriété spectrale, Timing, Pulsar RX, Source RX transitoire, Pulsar milliseconde, Sursaut RX, Domaine énergie keV, Courbe lumière, Forme impulsion, Température électron, Epaisseur optique, Plasma, Température photon, Diffusion optique, Emission RX, Etoile neutron, Accrétion, Pulsation RX, Métallicité, Modèle, Binaire RX, Source RX binaire, Source RX cosmique.
English descriptors
- KwdEn :
- Accretion, Binary X ray source, Cosmic x-ray sources, Electron temperature, Light curves, Metallicity, Millisecond pulsar, Models, Neutron stars, Optical scattering, Optical thickness, Photon temperature, Plasma, Pulse shape, Spectral properties, Timing, Transient X ray source, X ray burst, X ray emission, X ray pulsar, X ray pulsation, X-ray binary stars, keV range.
Abstract
Context. IGR J 17498-2921 is the third X-ray transient accreting millisecond pulsar discovered by INTEGRAL. It was in outburst for about 40 days beginning on August 08, 2011. Aims. We analyze the spectral and timing properties of the object and the characteristics of X-ray bursts to constrain the physical processes responsible for the X-ray production in this class of sources. Methods. We studied the broad-band spectrum of the persistent emission in the 0.6-300 keV energy band using simultaneous INTEGRAL, RXTE, and Swift data obtained in August-September 2011. We also describe the timing properties in the 2-100 keV energy range such as the outburst lightcurve, pulse profile, pulsed fraction, pulsed emission, time lags, and study the properties of X-ray bursts discovered by RXTE, Swift, and INTEGRAL and the recurrence time. Results. The broad-band average spectrum is well-described by thermal Comptonization with an electron temperature of kTe ∼ 50 keV, soft seed photons of kTbb ∼ 1 keV, and Thomson optical depth τT ∼ I in a slab geometry. The slab area corresponds to a black body radius of Rbb ∼ 9 km. During the outburst, the spectrum stays remarkably stable with plasma and soft seed photon temperatures and scattering optical depth that are constant within the errors. This behavior has been interpreted as indicating that the X-ray emission originates above the neutron star (NS) surface in a hot slab (either the heated NS surface or the accretion shock). The INTEGRAL, RXTE, and Swift data reveal the X-ray pulsation at a period of 2.5 ms up to ∼65 keV. The pulsed fraction is consistent with being constant, i.e. energy independent and has a typical value of 6-7%. The nearly sinusoidal pulses show soft lags that seem to saturate near 10 keV at a rather small value of ∼-60 μs with those observed in other accreting pulsars. The short burst profiles indicate that there is a hydrogen-poor material at ignition, which suggests either that the accreted material is hydrogen-deficient, or that the CNO metallicity is up to a factor of about two times solar. However, the variation in the burst recurrence time as a function of m (inferred from the X-ray flux) is much smaller than predicted by helium-ignition models.
Affiliations:
- Australie, Finlande, France, Italie, Pays-Bas, Suisse
- Canton de Berne, Canton de Genève, Hollande-Septentrionale, Île-de-France
- Amsterdam, Berne, Genève, Paris
- Université d'Amsterdam, Université de Genève
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Hermsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>3584 CA Utrecht</wicri:noRegion></affiliation><affiliation wicri:level="4"><inist:fA14 i1="08"><s1>Astronomical Institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>7 aut.</sZ></inist:fA14><country>Pays-Bas</country><placeName><settlement type="city">Amsterdam</settlement><region nuts="2" type="province">Hollande-Septentrionale</region><settlement type="city">Amsterdam</settlement></placeName><orgName type="university">Université d'Amsterdam</orgName></affiliation></author><author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. 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Falanga</name><affiliation wicri:level="1"><inist:fA14 i1="01"><s1>International Space Science Institute (ISSI), Hallerstrasse 6</s1><s2>3012 Bern</s2><s3>CHE</s3><sZ>1 aut.</sZ></inist:fA14><country>Suisse</country><placeName><settlement type="city">Berne</settlement><region type="région" nuts="3">Canton de Berne</region></placeName></affiliation></author><author><name sortKey="Kuiper, L" sort="Kuiper, L" uniqKey="Kuiper L" first="L." last="Kuiper">L. Kuiper</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>3584 CA Utrecht</wicri:noRegion></affiliation></author><author><name sortKey="Poutanen, J" sort="Poutanen, J" uniqKey="Poutanen J" first="J." last="Poutanen">J. Poutanen</name><affiliation wicri:level="1"><inist:fA14 i1="03"><s1>Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu</s1><s3>FIN</s3><sZ>3 aut.</sZ></inist:fA14><country>Finlande</country><wicri:noRegion>Astronomy Division, Department of Physics, PO Box 3000, 90014 University of Oulu</wicri:noRegion></affiliation></author><author><name sortKey="Galloway, D K" sort="Galloway, D K" uniqKey="Galloway D" first="D. K." last="Galloway">D. K. Galloway</name><affiliation wicri:level="1"><inist:fA14 i1="04"><s1>Monash Center for Astrophysics, School of Physics, and School of Mathematical Sciences, Monash University</s1><s2>VIC 3800</s2><s3>AUS</s3><sZ>4 aut.</sZ></inist:fA14><country>Australie</country><wicri:noRegion>VIC 3800</wicri:noRegion></affiliation></author><author><name sortKey="Bozzo, E" sort="Bozzo, E" uniqKey="Bozzo E" first="E." last="Bozzo">E. Bozzo</name><affiliation wicri:level="4"><inist:fA14 i1="05"><s1>ISDC, Data centre for astrophysics, University of Geneva, Chemin d'Écogia 16</s1><s2>1290 Versoix</s2><s3>CHE</s3><sZ>5 aut.</sZ></inist:fA14><country>Suisse</country><wicri:noRegion>1290 Versoix</wicri:noRegion><orgName type="university">Université de Genève</orgName><placeName><settlement type="city">Genève</settlement><region nuts="3" type="region">Canton de Genève</region></placeName></affiliation></author><author><name sortKey="Goldwurm, A" sort="Goldwurm, A" uniqKey="Goldwurm A" first="A." last="Goldwurm">A. Goldwurm</name><affiliation wicri:level="1"><inist:fA14 i1="06"><s1>Service d'Astrophysique (SAp), IRFU/DSM/CEA-Saclay</s1><s2>91191 Gif-sur-Yvette</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion><wicri:noRegion>IRFU/DSM/CEA-Saclay</wicri:noRegion><wicri:noRegion>91191 Gif-sur-Yvette</wicri:noRegion></affiliation><affiliation wicri:level="1"><inist:fA14 i1="07"><s1>Unite mixte de recherche Astroparticule et Cosmologie, 10 rue Alice Domon et Léonie Duquet</s1><s2>75205 Paris</s2><s3>FRA</s3><sZ>6 aut.</sZ></inist:fA14><country>France</country><wicri:noRegion>75205 Paris</wicri:noRegion><placeName><settlement type="city">Paris</settlement><region type="région" nuts="2">Île-de-France</region></placeName></affiliation></author><author><name sortKey="Hermsen, W" sort="Hermsen, W" uniqKey="Hermsen W" first="W." last="Hermsen">W. Hermsen</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>SRON - Netherlands Institute for Space Research, Sorbonnelaan 2</s1><s2>3584 CA Utrecht</s2><s3>NLD</s3><sZ>2 aut.</sZ><sZ>7 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>3584 CA Utrecht</wicri:noRegion></affiliation><affiliation wicri:level="4"><inist:fA14 i1="08"><s1>Astronomical Institute "Anton Pannekoek", University of Amsterdam, Science Park 904</s1><s2>1098 XH, Amsterdam</s2><s3>NLD</s3><sZ>7 aut.</sZ></inist:fA14><country>Pays-Bas</country><placeName><settlement type="city">Amsterdam</settlement><region nuts="2" type="province">Hollande-Septentrionale</region><settlement type="city">Amsterdam</settlement></placeName><orgName type="university">Université d'Amsterdam</orgName></affiliation></author><author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name><affiliation wicri:level="1"><inist:fA14 i1="09"><s1>INAF - Osservatorio Astronomico di Roma, via Frascati 33</s1><s2>00040 Monteporzio Catone (Roma)</s2><s3>ITA</s3><sZ>8 aut.</sZ></inist:fA14><country>Italie</country><wicri:noRegion>00040 Monteporzio Catone (Roma)</wicri:noRegion></affiliation></author></analytic><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="2012">2012</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>Accretion</term><term>Binary X ray source</term><term>Cosmic x-ray sources</term><term>Electron temperature</term><term>Light curves</term><term>Metallicity</term><term>Millisecond pulsar</term><term>Models</term><term>Neutron stars</term><term>Optical scattering</term><term>Optical thickness</term><term>Photon temperature</term><term>Plasma</term><term>Pulse shape</term><term>Spectral properties</term><term>Timing</term><term>Transient X ray source</term><term>X ray burst</term><term>X ray emission</term><term>X ray pulsar</term><term>X ray pulsation</term><term>X-ray binary stars</term><term>keV range</term></keywords><keywords scheme="Pascal" xml:lang="fr"><term>Propriété spectrale</term><term>Timing</term><term>Pulsar RX</term><term>Source RX transitoire</term><term>Pulsar milliseconde</term><term>Sursaut RX</term><term>Domaine énergie keV</term><term>Courbe lumière</term><term>Forme impulsion</term><term>Température électron</term><term>Epaisseur optique</term><term>Plasma</term><term>Température photon</term><term>Diffusion optique</term><term>Emission RX</term><term>Etoile neutron</term><term>Accrétion</term><term>Pulsation RX</term><term>Métallicité</term><term>Modèle</term><term>Binaire RX</term><term>Source RX binaire</term><term>Source RX cosmique</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">Context. IGR J 17498-2921 is the third X-ray transient accreting millisecond pulsar discovered by INTEGRAL. It was in outburst for about 40 days beginning on August 08, 2011. Aims. We analyze the spectral and timing properties of the object and the characteristics of X-ray bursts to constrain the physical processes responsible for the X-ray production in this class of sources. Methods. We studied the broad-band spectrum of the persistent emission in the 0.6-300 keV energy band using simultaneous INTEGRAL, RXTE, and Swift data obtained in August-September 2011. We also describe the timing properties in the 2-100 keV energy range such as the outburst lightcurve, pulse profile, pulsed fraction, pulsed emission, time lags, and study the properties of X-ray bursts discovered by RXTE, Swift, and INTEGRAL and the recurrence time. Results. The broad-band average spectrum is well-described by thermal Comptonization with an electron temperature of kT<sub>e</sub> ∼ 50 keV, soft seed photons of kT<sub>bb</sub> ∼ 1 keV, and Thomson optical depth τ<sub>T</sub> ∼ I in a slab geometry. The slab area corresponds to a black body radius of R<sub>bb</sub> ∼ 9 km. During the outburst, the spectrum stays remarkably stable with plasma and soft seed photon temperatures and scattering optical depth that are constant within the errors. This behavior has been interpreted as indicating that the X-ray emission originates above the neutron star (NS) surface in a hot slab (either the heated NS surface or the accretion shock). The INTEGRAL, RXTE, and Swift data reveal the X-ray pulsation at a period of 2.5 ms up to ∼65 keV. The pulsed fraction is consistent with being constant, i.e. energy independent and has a typical value of 6-7%. The nearly sinusoidal pulses show soft lags that seem to saturate near 10 keV at a rather small value of ∼-60 μs with those observed in other accreting pulsars. The short burst profiles indicate that there is a hydrogen-poor material at ignition, which suggests either that the accreted material is hydrogen-deficient, or that the CNO metallicity is up to a factor of about two times solar. However, the variation in the burst recurrence time as a function of m (inferred from the X-ray flux) is much smaller than predicted by helium-ignition models.</div></front></TEI><affiliations><list><country><li>Australie</li><li>Finlande</li><li>France</li><li>Italie</li><li>Pays-Bas</li><li>Suisse</li></country><region><li>Canton de Berne</li><li>Canton de Genève</li><li>Hollande-Septentrionale</li><li>Île-de-France</li></region><settlement><li>Amsterdam</li><li>Berne</li><li>Genève</li><li>Paris</li></settlement><orgName><li>Université d'Amsterdam</li><li>Université de Genève</li></orgName></list><tree><country name="Suisse"><region name="Canton de Berne"><name sortKey="Falanga, M" sort="Falanga, M" uniqKey="Falanga M" first="M." last="Falanga">M. Falanga</name></region><name sortKey="Bozzo, E" sort="Bozzo, E" uniqKey="Bozzo E" first="E." last="Bozzo">E. Bozzo</name></country><country name="Pays-Bas"><noRegion><name sortKey="Kuiper, L" sort="Kuiper, L" uniqKey="Kuiper L" first="L." last="Kuiper">L. Kuiper</name></noRegion><name sortKey="Hermsen, W" sort="Hermsen, W" uniqKey="Hermsen W" first="W." last="Hermsen">W. Hermsen</name><name sortKey="Hermsen, W" sort="Hermsen, W" uniqKey="Hermsen W" first="W." last="Hermsen">W. Hermsen</name></country><country name="Finlande"><noRegion><name sortKey="Poutanen, J" sort="Poutanen, J" uniqKey="Poutanen J" first="J." last="Poutanen">J. Poutanen</name></noRegion></country><country name="Australie"><noRegion><name sortKey="Galloway, D K" sort="Galloway, D K" uniqKey="Galloway D" first="D. K." last="Galloway">D. K. Galloway</name></noRegion></country><country name="France"><noRegion><name sortKey="Goldwurm, A" sort="Goldwurm, A" uniqKey="Goldwurm A" first="A." last="Goldwurm">A. Goldwurm</name></noRegion><name sortKey="Goldwurm, A" sort="Goldwurm, A" uniqKey="Goldwurm A" first="A." last="Goldwurm">A. Goldwurm</name></country><country name="Italie"><noRegion><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name></noRegion></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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