AustralieFrV1, Istex, Curation, bibRecord, 000C63

Long‐term spectral and timing properties of the soft gamma‐ray repeater SGR 1833−0832 and detection of extended X‐ray emission around the radio pulsar PSR B1830−08

Identifieur interne : 000C63 ( Istex/Curation ); précédent : 000C62; suivant : 000C64

Long‐term spectral and timing properties of the soft gamma‐ray repeater SGR 1833−0832 and detection of extended X‐ray emission around the radio pulsar PSR B1830−08

Auteurs : P. Esposito [Italie] ; G. L. Israel [Italie] ; R. Turolla [Italie, Royaume-Uni] ; F. Mattana [France] ; A. Tiengo [Italie] ; A. Possenti [Italie] ; S. Zane [Royaume-Uni] ; N. Rea [Espagne] ; M. Burgay [Italie] ; D. Götz [France] ; S. Mereghetti [Italie] ; L. Stella [Italie] ; M. H. Wieringa [Australie] ; J. M. Sarkissian [Australie] ; T. Enoto [États-Unis] ; P. Romano [Italie] ; T. Sakamoto [États-Unis] ; Y. E. Nakagawa [Japon] ; K. Makishima [Japon] ; Nakazawa [Japon] ; H. Nishioka [Japon] ; C. François-Martin [France]

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-09-01.

RBID : ISTEX:43BA55885B793AD60EC9C7DD943FDE0DBD67425B

English descriptors

Abstract

SGR 1833−0832 was discovered on 2010 March 19, thanks to the Swift detection of a short hard X‐ray burst and follow‐up X‐ray observations. Since then, it was repeatedly observed with Swift, Rossi X‐ray Timing Explorer and XMM–Newton. Using these data, which span about 225 d, we studied the long‐term spectral and timing characteristics of SGR 1833−0832. We found evidence for diffuse emission surrounding SGR 1833−0832, which is most likely a halo produced by the scattering of the point‐source X‐ray radiation by dust along the line of sight, and we show that the source X‐ray spectrum is well described by an absorbed blackbody, with temperature kT∼ 1.2 keV and absorbing column NH= (10.4 ± 0.2) × 1022 cm−2, while different or more complex models are disfavoured. The source persistent X‐ray emission remained fairly constant at ∼3.7 × 10−12 erg cm−2 s−1 for the first ∼20 d after the onset of the bursting episode, then it faded by a factor of ∼40 in the subsequent ∼140 d, following a power‐law trend with index α≃−0.5. We obtained a phase‐coherent timing solution with the longest baseline (∼225 d) to date for this source which, besides period P= 7.565 4084(4) s and period derivative s s−1, includes higher order period derivatives. We also report on our search of the counterpart to the soft gamma‐ray repeater (SGR) at radio frequencies using the Australia Telescope Compact Array and the Parkes Radio Telescope. No evidence for radio emission was found, down to flux densities of 0.9 mJy (at 1.5 GHz) and 0.09 mJy (at 1.4 GHz) for the continuum and pulsed emissions, respectively, consistently with other observations at different epochs. Finally, the analysis of the field of PSR B1830−08 (J1833−0827), which was serendipitously imaged by the XMM–Newton observations, led to the discovery of the X‐ray pulsar wind nebula generated by this 85‐ms radio pulsar. We discuss its possible association with the unidentified TeV source HESS J1834−087.

Url:

https://api.istex.fr/document/43BA55885B793AD60EC9C7DD943FDE0DBD67425B/fulltext/pdf

DOI: 10.1111/j.1365-2966.2011.19022.x

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Le document en format XML

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<author><name sortKey="Mereghetti, S" sort="Mereghetti, S" uniqKey="Mereghetti S" first="S." last="Mereghetti">S. Mereghetti</name>
<affiliation wicri:level="1"><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</mods:affiliation>
<country xml:lang="fr">Italie</country>
<wicri:regionArea>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name>
<affiliation wicri:level="1"><mods:affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</mods:affiliation>
<country xml:lang="fr">Italie</country>
<wicri:regionArea>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Wieringa, M H" sort="Wieringa, M H" uniqKey="Wieringa M" first="M. H." last="Wieringa">M. H. Wieringa</name>
<affiliation wicri:level="1"><mods:affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</mods:affiliation>
<country xml:lang="fr">Australie</country>
<wicri:regionArea>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Sarkissian, J M" sort="Sarkissian, J M" uniqKey="Sarkissian J" first="J. M." last="Sarkissian">J. M. Sarkissian</name>
<affiliation wicri:level="1"><mods:affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</mods:affiliation>
<country xml:lang="fr">Australie</country>
<wicri:regionArea>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Enoto, T" sort="Enoto, T" uniqKey="Enoto T" first="T." last="Enoto">T. Enoto</name>
<affiliation wicri:level="1"><mods:affiliation>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA</mods:affiliation>
<country xml:lang="fr">États-Unis</country>
<wicri:regionArea>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Romano, P" sort="Romano, P" uniqKey="Romano P" first="P." last="Romano">P. Romano</name>
<affiliation wicri:level="1"><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy</mods:affiliation>
<country xml:lang="fr">Italie</country>
<wicri:regionArea>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Sakamoto, T" sort="Sakamoto, T" uniqKey="Sakamoto T" first="T." last="Sakamoto">T. Sakamoto</name>
<affiliation wicri:level="1"><mods:affiliation>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</mods:affiliation>
<country xml:lang="fr">États-Unis</country>
<wicri:regionArea>NASA Goddard Space Flight Center, Greenbelt, MD 20771</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Nakagawa, Y E" sort="Nakagawa, Y E" uniqKey="Nakagawa Y" first="Y. E." last="Nakagawa">Y. E. Nakagawa</name>
<affiliation wicri:level="1"><mods:affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</mods:affiliation>
<country xml:lang="fr">Japon</country>
<wicri:regionArea>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Makishima, K" sort="Makishima, K" uniqKey="Makishima K" first="K." last="Makishima">K. Makishima</name>
<affiliation wicri:level="1"><mods:affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</mods:affiliation>
<country xml:lang="fr">Japon</country>
<wicri:regionArea>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198</wicri:regionArea>
</affiliation>
<affiliation wicri:level="1"><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation>
<country xml:lang="fr">Japon</country>
<wicri:regionArea>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Nakazawa, " sort="Nakazawa, " uniqKey="Nakazawa " first="" last="Nakazawa"> Nakazawa</name>
<affiliation wicri:level="1"><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation>
<country xml:lang="fr">Japon</country>
<wicri:regionArea>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Nishioka, H" sort="Nishioka, H" uniqKey="Nishioka H" first="H." last="Nishioka">H. Nishioka</name>
<affiliation wicri:level="1"><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation>
<country xml:lang="fr">Japon</country>
<wicri:regionArea>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033</wicri:regionArea>
</affiliation>
</author>
<author><name sortKey="Francois Artin, C" sort="Francois Artin, C" uniqKey="Francois Artin C" first="C." last="François-Martin">C. François-Martin</name>
<affiliation wicri:level="1"><mods:affiliation>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France</mods:affiliation>
<country xml:lang="fr">France</country>
<wicri:regionArea>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5</wicri:regionArea>
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<monogr></monogr>
<series><title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="alt">MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY</title>
<idno type="ISSN">0035-8711</idno>
<idno type="eISSN">1365-2966</idno>
<imprint><biblScope unit="vol">416</biblScope>
<biblScope unit="issue">1</biblScope>
<biblScope unit="page" from="205">205</biblScope>
<biblScope unit="page" to="215">215</biblScope>
<biblScope unit="page-count">11</biblScope>
<publisher>Blackwell Publishing Ltd</publisher>
<pubPlace>Oxford, UK</pubPlace>
<date type="published" when="2011-09-01">2011-09-01</date>
</imprint>
<idno type="ISSN">0035-8711</idno>
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<seriesStmt><idno type="ISSN">0035-8711</idno>
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<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Ancillary response</term>
<term>Arbitrary distance</term>
<term>Astron</term>
<term>Australia telescope</term>
<term>Background counts</term>
<term>Background maps</term>
<term>Better statistics</term>
<term>Black squares</term>
<term>Blackbody</term>
<term>Blackbody model</term>
<term>Blackbody spectrum</term>
<term>Blackbody temperature</term>
<term>Blue stars</term>
<term>Bottom panel</term>
<term>Burgay</term>
<term>Cambridge univ</term>
<term>Centre</term>
<term>Column density</term>
<term>Compact emission</term>
<term>Compact structure</term>
<term>Data sets</term>
<term>Diffuse emission</term>
<term>Effective area</term>
<term>Energy band</term>
<term>Energy range</term>
<term>Epic instrument</term>
<term>Esposito</term>
<term>Event lists</term>
<term>Exponential function</term>
<term>Gaensler</term>
<term>Galactic plane</term>
<term>Halo</term>
<term>Halo spectra</term>
<term>Hess</term>
<term>Higher ratio</term>
<term>Hobbs</term>
<term>Hydrogen column density</term>
<term>Inaf istituto</term>
<term>Kargaltsev pavlov</term>
<term>Kaspi</term>
<term>Large absorption</term>
<term>Large window mode</term>
<term>Light curves</term>
<term>Magnetars</term>
<term>Magnetospheric twist</term>
<term>Mereghetti</term>
<term>Minimum ratio</term>
<term>Mnras</term>
<term>Monthly notices</term>
<term>More details</term>
<term>Mosaicked image</term>
<term>Neutron star</term>
<term>Outburst</term>
<term>Paris cedex</term>
<term>Paris diderot</term>
<term>Parkes observatory</term>
<term>Parkes radio telescope</term>
<term>Persistent emission</term>
<term>Phase residuals</term>
<term>Phase shifts</term>
<term>Photon</term>
<term>Photon index</term>
<term>Point source</term>
<term>Possible association</term>
<term>Proper motion direction</term>
<term>Pulsar</term>
<term>Pulsar position</term>
<term>Radio emission</term>
<term>Radio magnetars</term>
<term>Radio observations</term>
<term>Radio pulsar</term>
<term>Radio pulsars</term>
<term>Remnant</term>
<term>Rossi timing explorer</term>
<term>Rotational energy loss</term>
<term>Rxte</term>
<term>Rxte data</term>
<term>Soft repeater</term>
<term>Source events</term>
<term>Source hess</term>
<term>Sourcefree regions</term>
<term>Spectral</term>
<term>Spectral analysis</term>
<term>Spectral parameters</term>
<term>Spie conf</term>
<term>Supernova remnant</term>
<term>Surface brightness</term>
<term>Swift data</term>
<term>Swift observations</term>
<term>Timing analysis</term>
<term>Timing noise</term>
<term>Timing properties</term>
<term>Timing solution</term>
<term>Twist angle</term>
<term>Upper limit</term>
<term>Upper limits</term>
<term>Windowed timing</term>
</keywords>
<keywords scheme="Teeft" xml:lang="en"><term>Ancillary response</term>
<term>Arbitrary distance</term>
<term>Astron</term>
<term>Australia telescope</term>
<term>Background counts</term>
<term>Background maps</term>
<term>Better statistics</term>
<term>Black squares</term>
<term>Blackbody</term>
<term>Blackbody model</term>
<term>Blackbody spectrum</term>
<term>Blackbody temperature</term>
<term>Blue stars</term>
<term>Bottom panel</term>
<term>Burgay</term>
<term>Cambridge univ</term>
<term>Centre</term>
<term>Column density</term>
<term>Compact emission</term>
<term>Compact structure</term>
<term>Data sets</term>
<term>Diffuse emission</term>
<term>Effective area</term>
<term>Energy band</term>
<term>Energy range</term>
<term>Epic instrument</term>
<term>Esposito</term>
<term>Event lists</term>
<term>Exponential function</term>
<term>Gaensler</term>
<term>Galactic plane</term>
<term>Halo</term>
<term>Halo spectra</term>
<term>Hess</term>
<term>Higher ratio</term>
<term>Hobbs</term>
<term>Hydrogen column density</term>
<term>Inaf istituto</term>
<term>Kargaltsev pavlov</term>
<term>Kaspi</term>
<term>Large absorption</term>
<term>Large window mode</term>
<term>Light curves</term>
<term>Magnetars</term>
<term>Magnetospheric twist</term>
<term>Mereghetti</term>
<term>Minimum ratio</term>
<term>Mnras</term>
<term>Monthly notices</term>
<term>More details</term>
<term>Mosaicked image</term>
<term>Neutron star</term>
<term>Outburst</term>
<term>Paris cedex</term>
<term>Paris diderot</term>
<term>Parkes observatory</term>
<term>Parkes radio telescope</term>
<term>Persistent emission</term>
<term>Phase residuals</term>
<term>Phase shifts</term>
<term>Photon</term>
<term>Photon index</term>
<term>Point source</term>
<term>Possible association</term>
<term>Proper motion direction</term>
<term>Pulsar</term>
<term>Pulsar position</term>
<term>Radio emission</term>
<term>Radio magnetars</term>
<term>Radio observations</term>
<term>Radio pulsar</term>
<term>Radio pulsars</term>
<term>Remnant</term>
<term>Rossi timing explorer</term>
<term>Rotational energy loss</term>
<term>Rxte</term>
<term>Rxte data</term>
<term>Soft repeater</term>
<term>Source events</term>
<term>Source hess</term>
<term>Sourcefree regions</term>
<term>Spectral</term>
<term>Spectral analysis</term>
<term>Spectral parameters</term>
<term>Spie conf</term>
<term>Supernova remnant</term>
<term>Surface brightness</term>
<term>Swift data</term>
<term>Swift observations</term>
<term>Timing analysis</term>
<term>Timing noise</term>
<term>Timing properties</term>
<term>Timing solution</term>
<term>Twist angle</term>
<term>Upper limit</term>
<term>Upper limits</term>
<term>Windowed timing</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<front><div type="abstract" xml:lang="en">SGR 1833−0832 was discovered on 2010 March 19, thanks to the Swift detection of a short hard X‐ray burst and follow‐up X‐ray observations. Since then, it was repeatedly observed with Swift, Rossi X‐ray Timing Explorer and XMM–Newton. Using these data, which span about 225 d, we studied the long‐term spectral and timing characteristics of SGR 1833−0832. We found evidence for diffuse emission surrounding SGR 1833−0832, which is most likely a halo produced by the scattering of the point‐source X‐ray radiation by dust along the line of sight, and we show that the source X‐ray spectrum is well described by an absorbed blackbody, with temperature kT∼ 1.2 keV and absorbing column NH= (10.4 ± 0.2) × 1022 cm−2, while different or more complex models are disfavoured. The source persistent X‐ray emission remained fairly constant at ∼3.7 × 10−12 erg cm−2 s−1 for the first ∼20 d after the onset of the bursting episode, then it faded by a factor of ∼40 in the subsequent ∼140 d, following a power‐law trend with index α≃−0.5. We obtained a phase‐coherent timing solution with the longest baseline (∼225 d) to date for this source which, besides period P= 7.565 4084(4) s and period derivative  s s−1, includes higher order period derivatives. We also report on our search of the counterpart to the soft gamma‐ray repeater (SGR) at radio frequencies using the Australia Telescope Compact Array and the Parkes Radio Telescope. No evidence for radio emission was found, down to flux densities of 0.9 mJy (at 1.5 GHz) and 0.09 mJy (at 1.4 GHz) for the continuum and pulsed emissions, respectively, consistently with other observations at different epochs. Finally, the analysis of the field of PSR B1830−08 (J1833−0827), which was serendipitously imaged by the XMM–Newton observations, led to the discovery of the X‐ray pulsar wind nebula generated by this 85‐ms radio pulsar. We discuss its possible association with the unidentified TeV source HESS J1834−087.</div>
</front>
</TEI>
</record>

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	Serveur d'exploration sur les relations entre la France et l'Australie
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Long‐term spectral and timing properties of the soft gamma‐ray repeater SGR 1833−0832 and detection of extended X‐ray emission around the radio pulsar PSR B1830−08

Long‐term spectral and timing properties of the soft gamma‐ray repeater SGR 1833−0832 and detection of extended X‐ray emission around the radio pulsar PSR B1830−08

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