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/Corpus ); précédent : 000C62; suivant : 000C64Long‐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 ; G. L. Israel ; R. Turolla ; F. Mattana ; A. Tiengo ; A. Possenti ; S. Zane ; N. Rea ; M. Burgay ; D. Götz ; S. Mereghetti ; L. Stella ; M. H. Wieringa ; J. M. Sarkissian ; T. Enoto ; P. Romano ; T. Sakamoto ; Y. E. Nakagawa ; K. Makishima ; Nakazawa ; H. Nishioka ; C. François-MartinSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011-09-01.
English descriptors
- KwdEn :
- Ancillary response, Arbitrary distance, Astron, Australia telescope, Background counts, Background maps, Better statistics, Black squares, Blackbody, Blackbody model, Blackbody spectrum, Blackbody temperature, Blue stars, Bottom panel, Burgay, Cambridge univ, Centre, Column density, Compact emission, Compact structure, Data sets, Diffuse emission, Effective area, Energy band, Energy range, Epic instrument, Esposito, Event lists, Exponential function, Gaensler, Galactic plane, Halo, Halo spectra, Hess, Higher ratio, Hobbs, Hydrogen column density, Inaf istituto, Kargaltsev pavlov, Kaspi, Large absorption, Large window mode, Light curves, Magnetars, Magnetospheric twist, Mereghetti, Minimum ratio, Mnras, Monthly notices, More details, Mosaicked image, Neutron star, Outburst, Paris cedex, Paris diderot, Parkes observatory, Parkes radio telescope, Persistent emission, Phase residuals, Phase shifts, Photon, Photon index, Point source, Possible association, Proper motion direction, Pulsar, Pulsar position, Radio emission, Radio magnetars, Radio observations, Radio pulsar, Radio pulsars, Remnant, Rossi timing explorer, Rotational energy loss, Rxte, Rxte data, Soft repeater, Source events, Source hess, Sourcefree regions, Spectral, Spectral analysis, Spectral parameters, Spie conf, Supernova remnant, Surface brightness, Swift data, Swift observations, Timing analysis, Timing noise, Timing properties, Timing solution, Twist angle, Upper limit, Upper limits, Windowed timing.
- Teeft :
- Ancillary response, Arbitrary distance, Astron, Australia telescope, Background counts, Background maps, Better statistics, Black squares, Blackbody, Blackbody model, Blackbody spectrum, Blackbody temperature, Blue stars, Bottom panel, Burgay, Cambridge univ, Centre, Column density, Compact emission, Compact structure, Data sets, Diffuse emission, Effective area, Energy band, Energy range, Epic instrument, Esposito, Event lists, Exponential function, Gaensler, Galactic plane, Halo, Halo spectra, Hess, Higher ratio, Hobbs, Hydrogen column density, Inaf istituto, Kargaltsev pavlov, Kaspi, Large absorption, Large window mode, Light curves, Magnetars, Magnetospheric twist, Mereghetti, Minimum ratio, Mnras, Monthly notices, More details, Mosaicked image, Neutron star, Outburst, Paris cedex, Paris diderot, Parkes observatory, Parkes radio telescope, Persistent emission, Phase residuals, Phase shifts, Photon, Photon index, Point source, Possible association, Proper motion direction, Pulsar, Pulsar position, Radio emission, Radio magnetars, Radio observations, Radio pulsar, Radio pulsars, Remnant, Rossi timing explorer, Rotational energy loss, Rxte, Rxte data, Soft repeater, Source events, Source hess, Sourcefree regions, Spectral, Spectral analysis, Spectral parameters, Spie conf, Supernova remnant, Surface brightness, Swift data, Swift observations, Timing analysis, Timing noise, Timing properties, Timing solution, Twist angle, Upper limit, Upper limits, Windowed timing.
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:
DOI: 10.1111/j.1365-2966.2011.19022.x
Links to Exploration step
ISTEX:43BA55885B793AD60EC9C7DD943FDE0DBD67425BLe document en format XML
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Götz</name><affiliation><mods:affiliation>AIM (UMR 7158 CEA/DSM‐CNRS‐Université Paris Diderot) Irfu/Service d’Astrophysique, Saclay, F‐91191 Gif‐sur‐Yvette Cedex, France</mods:affiliation></affiliation></author><author><name sortKey="Mereghetti, S" sort="Mereghetti, S" uniqKey="Mereghetti S" first="S." last="Mereghetti">S. Mereghetti</name><affiliation><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</mods:affiliation></affiliation></author><author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</mods:affiliation></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><mods:affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</mods:affiliation></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><mods:affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</mods:affiliation></affiliation></author><author><name sortKey="Enoto, T" sort="Enoto, T" uniqKey="Enoto T" first="T." last="Enoto">T. Enoto</name><affiliation><mods:affiliation>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA</mods:affiliation></affiliation></author><author><name sortKey="Romano, P" sort="Romano, P" uniqKey="Romano P" first="P." last="Romano">P. Romano</name><affiliation><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy</mods:affiliation></affiliation></author><author><name sortKey="Sakamoto, T" sort="Sakamoto, T" uniqKey="Sakamoto T" first="T." last="Sakamoto">T. Sakamoto</name><affiliation><mods:affiliation>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</mods:affiliation></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><mods:affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</mods:affiliation></affiliation></author><author><name sortKey="Makishima, K" sort="Makishima, K" uniqKey="Makishima K" first="K." last="Makishima">K. Makishima</name><affiliation><mods:affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation></affiliation></author><author><name sortKey="Nakazawa, " sort="Nakazawa, " uniqKey="Nakazawa " first="" last="Nakazawa"> Nakazawa</name><affiliation><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation></affiliation></author><author><name sortKey="Nishioka, H" sort="Nishioka, H" uniqKey="Nishioka H" first="H." last="Nishioka">H. Nishioka</name><affiliation><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation></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><mods:affiliation>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France</mods:affiliation></affiliation></author></titleStmt><publicationStmt><idno type="wicri:source">ISTEX</idno><idno type="RBID">ISTEX:43BA55885B793AD60EC9C7DD943FDE0DBD67425B</idno><date when="2011" year="2011">2011</date><idno type="doi">10.1111/j.1365-2966.2011.19022.x</idno><idno type="url">https://api.istex.fr/document/43BA55885B793AD60EC9C7DD943FDE0DBD67425B/fulltext/pdf</idno><idno type="wicri:Area/Istex/Corpus">000C63</idno><idno type="wicri:explorRef" wicri:stream="Istex" wicri:step="Corpus" wicri:corpus="ISTEX">000C63</idno></publicationStmt><sourceDesc><biblStruct><analytic><title level="a" type="main">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</title><author><name sortKey="Esposito, P" sort="Esposito, P" uniqKey="Esposito P" first="P." last="Esposito">P. Esposito</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</mods:affiliation></affiliation><affiliation><mods:affiliation>E-mail: paoloesp@oa‐cagliari.inaf.it</mods:affiliation></affiliation></author><author><name sortKey="Israel, G L" sort="Israel, G L" uniqKey="Israel G" first="G. L." last="Israel">G. L. Israel</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</mods:affiliation></affiliation></author><author><name sortKey="Turolla, R" sort="Turolla, R" uniqKey="Turolla R" first="R." last="Turolla">R. Turolla</name><affiliation><mods:affiliation>Università di Padova, Dipartimento di Fisica, via F. Marzolo 8, I‐35131 Padova, Italy</mods:affiliation></affiliation><affiliation><mods:affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</mods:affiliation></affiliation></author><author><name sortKey="Mattana, F" sort="Mattana, F" uniqKey="Mattana F" first="F." last="Mattana">F. Mattana</name><affiliation><mods:affiliation>François Arago Centre, APC (Université Paris Diderot, CNRS/IN2P3, CEA/DSM, Observatoire de Paris), 13 rue Watt, F‐75205 Paris Cedex 13, France</mods:affiliation></affiliation></author><author><name sortKey="Tiengo, A" sort="Tiengo, A" uniqKey="Tiengo A" first="A." last="Tiengo">A. Tiengo</name><affiliation><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</mods:affiliation></affiliation></author><author><name sortKey="Possenti, A" sort="Possenti, A" uniqKey="Possenti A" first="A." last="Possenti">A. Possenti</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</mods:affiliation></affiliation></author><author><name sortKey="Zane, S" sort="Zane, S" uniqKey="Zane S" first="S." last="Zane">S. Zane</name><affiliation><mods:affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</mods:affiliation></affiliation></author><author><name sortKey="Rea, N" sort="Rea, N" uniqKey="Rea N" first="N." last="Rea">N. Rea</name><affiliation><mods:affiliation>Institut de Ciències de l’Espai (CSIC–IEEC), Campus UAB, Facultat de Ciències, Torre C5‐parell, E‐08193 Barcelona, Spain</mods:affiliation></affiliation></author><author><name sortKey="Burgay, M" sort="Burgay, M" uniqKey="Burgay M" first="M." last="Burgay">M. Burgay</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</mods:affiliation></affiliation></author><author><name sortKey="Gotz, D" sort="Gotz, D" uniqKey="Gotz D" first="D." last="Götz">D. Götz</name><affiliation><mods:affiliation>AIM (UMR 7158 CEA/DSM‐CNRS‐Université Paris Diderot) Irfu/Service d’Astrophysique, Saclay, F‐91191 Gif‐sur‐Yvette Cedex, France</mods:affiliation></affiliation></author><author><name sortKey="Mereghetti, S" sort="Mereghetti, S" uniqKey="Mereghetti S" first="S." last="Mereghetti">S. Mereghetti</name><affiliation><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</mods:affiliation></affiliation></author><author><name sortKey="Stella, L" sort="Stella, L" uniqKey="Stella L" first="L." last="Stella">L. Stella</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</mods:affiliation></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><mods:affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</mods:affiliation></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><mods:affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</mods:affiliation></affiliation></author><author><name sortKey="Enoto, T" sort="Enoto, T" uniqKey="Enoto T" first="T." last="Enoto">T. Enoto</name><affiliation><mods:affiliation>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA</mods:affiliation></affiliation></author><author><name sortKey="Romano, P" sort="Romano, P" uniqKey="Romano P" first="P." last="Romano">P. Romano</name><affiliation><mods:affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy</mods:affiliation></affiliation></author><author><name sortKey="Sakamoto, T" sort="Sakamoto, T" uniqKey="Sakamoto T" first="T." last="Sakamoto">T. Sakamoto</name><affiliation><mods:affiliation>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</mods:affiliation></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><mods:affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</mods:affiliation></affiliation></author><author><name sortKey="Makishima, K" sort="Makishima, K" uniqKey="Makishima K" first="K." last="Makishima">K. Makishima</name><affiliation><mods:affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</mods:affiliation></affiliation><affiliation><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation></affiliation></author><author><name sortKey="Nakazawa, " sort="Nakazawa, " uniqKey="Nakazawa " first="" last="Nakazawa"> Nakazawa</name><affiliation><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation></affiliation></author><author><name sortKey="Nishioka, H" sort="Nishioka, H" uniqKey="Nishioka H" first="H." last="Nishioka">H. Nishioka</name><affiliation><mods:affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</mods:affiliation></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><mods:affiliation>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France</mods:affiliation></affiliation></author></analytic><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></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><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><istex><corpusName>wiley</corpusName><keywords><teeft><json:string>pulsar</json:string><json:string>esposito</json:string><json:string>mnras</json:string><json:string>blackbody</json:string><json:string>rxte</json:string><json:string>magnetars</json:string><json:string>monthly notices</json:string><json:string>astron</json:string><json:string>hobbs</json:string><json:string>gaensler</json:string><json:string>mereghetti</json:string><json:string>burgay</json:string><json:string>kaspi</json:string><json:string>energy range</json:string><json:string>photon</json:string><json:string>diffuse emission</json:string><json:string>hess</json:string><json:string>upper limit</json:string><json:string>compact structure</json:string><json:string>pulsar position</json:string><json:string>australia telescope</json:string><json:string>rxte data</json:string><json:string>compact emission</json:string><json:string>halo</json:string><json:string>radio pulsars</json:string><json:string>timing noise</json:string><json:string>arbitrary distance</json:string><json:string>spectral analysis</json:string><json:string>radio emission</json:string><json:string>energy band</json:string><json:string>timing solution</json:string><json:string>data sets</json:string><json:string>blackbody model</json:string><json:string>spectral parameters</json:string><json:string>galactic plane</json:string><json:string>exponential function</json:string><json:string>bottom panel</json:string><json:string>phase shifts</json:string><json:string>background counts</json:string><json:string>more details</json:string><json:string>supernova remnant</json:string><json:string>timing properties</json:string><json:string>radio pulsar</json:string><json:string>outburst</json:string><json:string>remnant</json:string><json:string>point source</json:string><json:string>paris diderot</json:string><json:string>sourcefree regions</json:string><json:string>parkes observatory</json:string><json:string>paris cedex</json:string><json:string>parkes radio telescope</json:string><json:string>light curves</json:string><json:string>event lists</json:string><json:string>better statistics</json:string><json:string>higher ratio</json:string><json:string>timing analysis</json:string><json:string>inaf istituto</json:string><json:string>neutron star</json:string><json:string>large absorption</json:string><json:string>cambridge univ</json:string><json:string>surface brightness</json:string><json:string>hydrogen column density</json:string><json:string>possible association</json:string><json:string>persistent emission</json:string><json:string>swift observations</json:string><json:string>blackbody temperature</json:string><json:string>rossi timing explorer</json:string><json:string>photon index</json:string><json:string>upper limits</json:string><json:string>radio observations</json:string><json:string>black squares</json:string><json:string>blue stars</json:string><json:string>epic instrument</json:string><json:string>source hess</json:string><json:string>swift data</json:string><json:string>blackbody spectrum</json:string><json:string>kargaltsev pavlov</json:string><json:string>minimum ratio</json:string><json:string>effective area</json:string><json:string>background maps</json:string><json:string>mosaicked image</json:string><json:string>large window mode</json:string><json:string>rotational energy loss</json:string><json:string>source events</json:string><json:string>column density</json:string><json:string>halo spectra</json:string><json:string>soft repeater</json:string><json:string>proper motion direction</json:string><json:string>spie conf</json:string><json:string>phase residuals</json:string><json:string>windowed timing</json:string><json:string>magnetospheric twist</json:string><json:string>twist angle</json:string><json:string>radio magnetars</json:string><json:string>ancillary response</json:string><json:string>centre</json:string><json:string>spectral</json:string></teeft></keywords><author><json:item><name>P. Esposito</name><affiliations><json:string>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</json:string><json:string>E-mail: paoloesp@oa‐cagliari.inaf.it</json:string></affiliations></json:item><json:item><name>G. L. Israel</name><affiliations><json:string>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</json:string></affiliations></json:item><json:item><name>R. Turolla</name><affiliations><json:string>Università di Padova, Dipartimento di Fisica, via F. Marzolo 8, I‐35131 Padova, Italy</json:string><json:string>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</json:string></affiliations></json:item><json:item><name>F. Mattana</name><affiliations><json:string>François Arago Centre, APC (Université Paris Diderot, CNRS/IN2P3, CEA/DSM, Observatoire de Paris), 13 rue Watt, F‐75205 Paris Cedex 13, France</json:string></affiliations></json:item><json:item><name>A. Tiengo</name><affiliations><json:string>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</json:string></affiliations></json:item><json:item><name>A. Possenti</name><affiliations><json:string>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</json:string></affiliations></json:item><json:item><name>S. Zane</name><affiliations><json:string>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</json:string></affiliations></json:item><json:item><name>N. Rea</name><affiliations><json:string>Institut de Ciències de l’Espai (CSIC–IEEC), Campus UAB, Facultat de Ciències, Torre C5‐parell, E‐08193 Barcelona, Spain</json:string></affiliations></json:item><json:item><name>M. Burgay</name><affiliations><json:string>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</json:string></affiliations></json:item><json:item><name>D. Götz</name><affiliations><json:string>AIM (UMR 7158 CEA/DSM‐CNRS‐Université Paris Diderot) Irfu/Service d’Astrophysique, Saclay, F‐91191 Gif‐sur‐Yvette Cedex, France</json:string></affiliations></json:item><json:item><name>S. Mereghetti</name><affiliations><json:string>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</json:string></affiliations></json:item><json:item><name>L. Stella</name><affiliations><json:string>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</json:string></affiliations></json:item><json:item><name>M. H. Wieringa</name><affiliations><json:string>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</json:string></affiliations></json:item><json:item><name>J. M. Sarkissian</name><affiliations><json:string>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</json:string></affiliations></json:item><json:item><name>T. Enoto</name><affiliations><json:string>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA</json:string></affiliations></json:item><json:item><name>P. Romano</name><affiliations><json:string>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy</json:string></affiliations></json:item><json:item><name>T. Sakamoto</name><affiliations><json:string>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</json:string></affiliations></json:item><json:item><name>Y. E. Nakagawa</name><affiliations><json:string>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</json:string></affiliations></json:item><json:item><name>K. Makishima</name><affiliations><json:string>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</json:string><json:string>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</json:string></affiliations></json:item><json:item><name>K. Nakazawa</name><affiliations><json:string>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</json:string></affiliations></json:item><json:item><name>H. Nishioka</name><affiliations><json:string>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</json:string></affiliations></json:item><json:item><name>C. François‐Martin</name><affiliations><json:string>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France</json:string></affiliations></json:item></author><subject><json:item><lang><json:string>eng</json:string></lang><value>stars: neutron</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>pulsars: general</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>X‐rays: individual: PSR B1830−08 (J1833−0827)</value></json:item><json:item><lang><json:string>eng</json:string></lang><value>X‐rays: individual: SGR 1833−0832</value></json:item></subject><articleId><json:string>MNR19022</json:string></articleId><arkIstex>ark:/67375/WNG-SFP85DFN-W</arkIstex><language><json:string>eng</json:string></language><originalGenre><json:string>article</json:string></originalGenre><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.</abstract><qualityIndicators><score>10</score><pdfWordCount>9512</pdfWordCount><pdfCharCount>51933</pdfCharCount><pdfVersion>1.4</pdfVersion><pdfPageCount>11</pdfPageCount><pdfPageSize>595.274 x 782.286 pts</pdfPageSize><refBibsNative>true</refBibsNative><abstractWordCount>301</abstractWordCount><abstractCharCount>1957</abstractCharCount><keywordCount>4</keywordCount></qualityIndicators><title>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</title><genre><json:string>article</json:string></genre><host><title>Monthly Notices of the Royal Astronomical Society</title><language><json:string>unknown</json:string></language><doi><json:string>10.1111/(ISSN)1365-2966</json:string></doi><issn><json:string>0035-8711</json:string></issn><eissn><json:string>1365-2966</json:string></eissn><publisherId><json:string>MNR</json:string></publisherId><volume>416</volume><issue>1</issue><pages><first>205</first><last>215</last><total>11</total></pages><genre><json:string>journal</json:string></genre></host><namedEntities><unitex><date><json:string>09/10/0</json:string><json:string>6100</json:string><json:string>1374</json:string><json:string>2006</json:string><json:string>2007</json:string><json:string>7-3-1</json:string><json:string>11/07/0</json:string><json:string>10/06/0</json:string><json:string>2010</json:string></date><geogName></geogName><orgName><json:string>United Kingdom Infrared Telescope</json:string><json:string>Kavli Institute for Particle Astrophysics</json:string><json:string>Department of Physics, University of Tokyo</json:string><json:string>Stanford University</json:string><json:string>ATCA</json:string><json:string>RIKEN</json:string><json:string>NASA Goddard Space Flight Center</json:string><json:string>National Facility</json:string><json:string>Australia Telescope</json:string><json:string>ATNF</json:string><json:string>Australia Telescope National Facility, CSIRO Astronomy and Space Science</json:string><json:string>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research</json:string><json:string>Australia Telescope Compact Array</json:string><json:string>Newton Science Operation Center</json:string><json:string>Australia Telescope National Facility</json:string></orgName><orgName_funder></orgName_funder><orgName_provider></orgName_provider><persName><json:string>Y. E. Nakagawa</json:string><json:string>F. Marzolo</json:string><json:string>S. Zane</json:string><json:string>Paris Cedex</json:string><json:string>H. Wieringa</json:string><json:string>E. Bassini</json:string><json:string>K. Nakazawa</json:string><json:string>F. Mattana</json:string><json:string>T. Enoto</json:string><json:string>Paris Diderot</json:string><json:string>A. Tiengo</json:string><json:string>Denis Diderot</json:string><json:string>H. Nishioka</json:string><json:string>P. Esposito</json:string><json:string>The</json:string><json:string>S. Mereghetti</json:string><json:string>Vicky Kaspi</json:string><json:string>Norbert Schartel</json:string><json:string>Hans Krimm</json:string><json:string>M. Sarkissian</json:string><json:string>P. Romano</json:string><json:string>A. Possenti</json:string><json:string>U. La Malfa</json:string><json:string>C. Francois-Martin</json:string><json:string>Philip Edwards</json:string></persName><placeName><json:string>Sardinia</json:string><json:string>Stanford</json:string><json:string>Cagliari</json:string><json:string>Palermo</json:string><json:string>Australia</json:string><json:string>Greenbelt</json:string><json:string>Makishima</json:string><json:string>Japan</json:string><json:string>Frascati</json:string><json:string>Manchester</json:string><json:string>Barcelona</json:string><json:string>MD</json:string><json:string>Tokyo</json:string><json:string>CA</json:string><json:string>Gif-sur-Yvette</json:string><json:string>Compton</json:string><json:string>France</json:string><json:string>Italy</json:string><json:string>Spain</json:string></placeName><ref_url><json:string>http://xmm.vilspa.esa.es/external/xmm_sw_cal/background/index</json:string><json:string>http://www.atnf.csiro.au/ research/pulsar/psrcat/</json:string><json:string>http://www.narrabri.atnf.csiro.au/observing/con</json:string></ref_url><ref_bibl><json:string>Tam et al. 2006</json:string><json:string>Albert et al. 2006</json:string><json:string>P. 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L.</forename><surname>Israel</surname></persName><affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0002"><persName><forename type="first">R.</forename><surname>Turolla</surname></persName><affiliation>Università di Padova, Dipartimento di Fisica, via F. Marzolo 8, I‐35131 Padova, Italy<address><country key="IT"></country></address></affiliation><affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</affiliation></author><author xml:id="author-0003"><persName><forename type="first">F.</forename><surname>Mattana</surname></persName><affiliation>François Arago Centre, APC (Université Paris Diderot, CNRS/IN2P3, CEA/DSM, Observatoire de Paris), 13 rue Watt, F‐75205 Paris Cedex 13, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0004"><persName><forename type="first">A.</forename><surname>Tiengo</surname></persName><affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0005"><persName><forename type="first">A.</forename><surname>Possenti</surname></persName><affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0006"><persName><forename type="first">S.</forename><surname>Zane</surname></persName><affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</affiliation></author><author xml:id="author-0007"><persName><forename type="first">N.</forename><surname>Rea</surname></persName><affiliation>Institut de Ciències de l’Espai (CSIC–IEEC), Campus UAB, Facultat de Ciències, Torre C5‐parell, E‐08193 Barcelona, Spain<address><country key="ES"></country></address></affiliation></author><author xml:id="author-0008"><persName><forename type="first">M.</forename><surname>Burgay</surname></persName><affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0009"><persName><forename type="first">D.</forename><surname>Götz</surname></persName><affiliation>AIM (UMR 7158 CEA/DSM‐CNRS‐Université Paris Diderot) Irfu/Service d’Astrophysique, Saclay, F‐91191 Gif‐sur‐Yvette Cedex, France<address><country key="FR"></country></address></affiliation></author><author xml:id="author-0010"><persName><forename type="first">S.</forename><surname>Mereghetti</surname></persName><affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0011"><persName><forename type="first">L.</forename><surname>Stella</surname></persName><affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0012"><persName><forename type="first">M. H.</forename><surname>Wieringa</surname></persName><affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0013"><persName><forename type="first">J. M.</forename><surname>Sarkissian</surname></persName><affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia<address><country key="AU"></country></address></affiliation></author><author xml:id="author-0014"><persName><forename type="first">T.</forename><surname>Enoto</surname></persName><affiliation>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0015"><persName><forename type="first">P.</forename><surname>Romano</surname></persName><affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy<address><country key="IT"></country></address></affiliation></author><author xml:id="author-0016"><persName><forename type="first">T.</forename><surname>Sakamoto</surname></persName><affiliation>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA<address><country key="US"></country></address></affiliation></author><author xml:id="author-0017"><persName><forename type="first">Y. E.</forename><surname>Nakagawa</surname></persName><affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan<address><country key="JP"></country></address></affiliation></author><author xml:id="author-0018"><persName><forename type="first">K.</forename><surname>Makishima</surname></persName><affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan<address><country key="JP"></country></address></affiliation><affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan<address><country key="JP"></country></address></affiliation></author><author xml:id="author-0019"><persName><forename type="first"> K.</forename><surname>Nakazawa</surname></persName><affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan<address><country key="JP"></country></address></affiliation></author><author xml:id="author-0020"><persName><forename type="first">H.</forename><surname>Nishioka</surname></persName><affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan<address><country key="JP"></country></address></affiliation></author><author xml:id="author-0021"><persName><forename type="first">C.</forename><surname>François‐Martin</surname></persName><affiliation>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France<address><country key="FR"></country></address></affiliation></author><idno type="istex">43BA55885B793AD60EC9C7DD943FDE0DBD67425B</idno><idno type="ark">ark:/67375/WNG-SFP85DFN-W</idno><idno type="DOI">10.1111/j.1365-2966.2011.19022.x</idno><idno type="unit">MNR19022</idno><idno type="toTypesetVersion">file:MNR.MNR19022.pdf</idno></analytic><monogr><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="pISSN">0035-8711</idno><idno type="eISSN">1365-2966</idno><idno type="book-DOI">10.1111/(ISSN)1365-2966</idno><idno type="book-part-DOI">10.1111/mnr.2011.416.issue-1</idno><idno type="product">MNR</idno><idno type="publisherDivision">ST</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"></date></imprint></monogr></biblStruct></sourceDesc></fileDesc><profileDesc><abstract xml:lang="en" style="main"><head>ABSTRACT</head><p>SGR 1833−0832 was discovered on 2010 March 19, thanks to the <hi rend="italic">Swift</hi> detection of a short hard X‐ray burst and follow‐up X‐ray observations. Since then, it was repeatedly observed with <hi rend="italic">Swift</hi>, <hi rend="italic">Rossi X‐ray Timing Explorer</hi> and <hi rend="italic">XMM–Newton</hi>. 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 <hi rend="italic">kT</hi>∼ 1.2 keV and absorbing column <hi rend="italic">N</hi><hi rend="subscript">H</hi>= (10.4 ± 0.2) × 10<hi rend="superscript">22</hi> cm<hi rend="superscript">−2</hi>, while different or more complex models are disfavoured. The source persistent X‐ray emission remained fairly constant at ∼3.7 × 10<hi rend="superscript">−12</hi> erg cm<hi rend="superscript">−2</hi> s<hi rend="superscript">−1</hi> 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 <hi rend="italic">P</hi>= 7.565 4084(4) s and period derivative <graphic url="equation/MNR_19022_mu1.gif" rend="inline image"></graphic> s s<hi rend="superscript">−1</hi>, 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 <hi rend="italic">XMM–Newton</hi> 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.</p></abstract><textClass><keywords xml:lang="en"><term xml:id="k1">stars: neutron</term><term xml:id="k2">pulsars: general</term><term xml:id="k3">X‐rays: individual: PSR B1830−08 (J1833−0827)</term><term xml:id="k4">X‐rays: individual: SGR 1833−0832</term></keywords><keywords rend="tocHeading1"><term>Papers</term></keywords></textClass><langUsage><language ident="en"></language></langUsage></profileDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/43BA55885B793AD60EC9C7DD943FDE0DBD67425B/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="Wiley, elements deleted: body"><istex:xmlDeclaration>version="1.0" encoding="UTF-8" standalone="yes"</istex:xmlDeclaration><istex:document><component version="2.0" type="serialArticle" xml:lang="en"><header><publicationMeta level="product"><publisherInfo><publisherName>Blackwell Publishing Ltd</publisherName><publisherLoc>Oxford, UK</publisherLoc></publisherInfo><doi origin="wiley" registered="yes">10.1111/(ISSN)1365-2966</doi><issn type="print">0035-8711</issn><issn type="electronic">1365-2966</issn><idGroup><id type="product" value="MNR"></id><id type="publisherDivision" value="ST"></id></idGroup><titleGroup><title type="main" sort="MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY">Monthly Notices of the Royal Astronomical Society</title></titleGroup></publicationMeta><publicationMeta level="part" position="09101"><doi origin="wiley">10.1111/mnr.2011.416.issue-1</doi><numberingGroup><numbering type="journalVolume" number="416">416</numbering><numbering type="journalIssue" number="1">1</numbering></numberingGroup><coverDate startDate="2011-09-01">September 2011</coverDate></publicationMeta><publicationMeta level="unit" type="article" position="17" status="forIssue"><doi origin="wiley">10.1111/j.1365-2966.2011.19022.x</doi><idGroup><id type="unit" value="MNR19022"></id></idGroup><countGroup><count type="pageTotal" number="11"></count></countGroup><titleGroup><title type="tocHeading1">Papers</title></titleGroup><copyright>© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</copyright><eventGroup><event type="xmlConverted" agent="Converter:BPG_TO_WML3G version:2.9.1 mode:FullText" date="2011-08-18"></event><event type="publishedOnlineEarlyUnpaginated" date="2011-06-16"></event><event type="firstOnline" date="2011-06-16"></event><event type="publishedOnlineFinalForm" date="2011-08-18"></event><event type="xmlConverted" agent="Converter:WILEY_ML3G_TO_WILEY_ML3GV2 version:3.8.8" date="2014-02-03"></event><event type="xmlConverted" agent="Converter:WML3G_To_WML3G version:4.1.7 mode:FullText,remove_FC" date="2014-10-31"></event></eventGroup><numberingGroup><numbering type="pageFirst" number="205">205</numbering><numbering type="pageLast" number="215">215</numbering></numberingGroup><correspondenceTo>
E‐mail: <email normalForm="paoloesp@oa-cagliari.inaf.it">paoloesp@oa‐cagliari.inaf.it</email></correspondenceTo><linkGroup><link type="toTypesetVersion" href="file:MNR.MNR19022.pdf"></link></linkGroup></publicationMeta><contentMeta><unparsedEditorialHistory>Accepted 2011 May 6. Received 2011 May 4; in original form 2011 April 12</unparsedEditorialHistory><countGroup><count type="figureTotal" number="7"></count><count type="tableTotal" number="3"></count><count type="formulaTotal" number="20"></count><count type="referenceTotal" number="83"></count><count type="linksCrossRef" number="193"></count></countGroup><titleGroup><title type="main">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</title><title type="shortAuthors"><i>P. 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Marzolo 8, I‐35131 Padova, Italy</unparsedAffiliation></affiliation><affiliation xml:id="a4"><unparsedAffiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</unparsedAffiliation></affiliation><affiliation xml:id="a5" countryCode="FR"><unparsedAffiliation>François Arago Centre, APC (Université Paris Diderot, CNRS/IN2P3, CEA/DSM, Observatoire de Paris), 13 rue Watt, F‐75205 Paris Cedex 13, France</unparsedAffiliation></affiliation><affiliation xml:id="a6" countryCode="IT"><unparsedAffiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</unparsedAffiliation></affiliation><affiliation xml:id="a7" countryCode="ES"><unparsedAffiliation>Institut de Ciències de l’Espai (CSIC–IEEC), Campus UAB, Facultat de Ciències, Torre C5‐parell, E‐08193 Barcelona, Spain</unparsedAffiliation></affiliation><affiliation xml:id="a8" countryCode="FR"><unparsedAffiliation>AIM (UMR 7158 CEA/DSM‐CNRS‐Université Paris Diderot) Irfu/Service d’Astrophysique, Saclay, F‐91191 Gif‐sur‐Yvette Cedex, France</unparsedAffiliation></affiliation><affiliation xml:id="a9" countryCode="AU"><unparsedAffiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</unparsedAffiliation></affiliation><affiliation xml:id="a10" countryCode="US"><unparsedAffiliation>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA</unparsedAffiliation></affiliation><affiliation xml:id="a11" countryCode="IT"><unparsedAffiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy</unparsedAffiliation></affiliation><affiliation xml:id="a12" countryCode="US"><unparsedAffiliation>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</unparsedAffiliation></affiliation><affiliation xml:id="a13" countryCode="JP"><unparsedAffiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</unparsedAffiliation></affiliation><affiliation xml:id="a14" countryCode="JP"><unparsedAffiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</unparsedAffiliation></affiliation><affiliation xml:id="a15" countryCode="FR"><unparsedAffiliation>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France</unparsedAffiliation></affiliation></affiliationGroup><keywordGroup xml:lang="en"><keyword xml:id="k1">stars: neutron</keyword><keyword xml:id="k2">pulsars: general</keyword><keyword xml:id="k3">X‐rays: individual: PSR B1830−08 (J1833−0827)</keyword><keyword xml:id="k4">X‐rays: individual: SGR 1833−0832</keyword></keywordGroup><abstractGroup><abstract type="main" xml:lang="en"><title type="main">ABSTRACT</title><p>SGR 1833−0832 was discovered on 2010 March 19, thanks to the <i>Swift</i> detection of a short hard X‐ray burst and follow‐up X‐ray observations. Since then, it was repeatedly observed with <i>Swift</i>, <i>Rossi X‐ray Timing Explorer</i> and <i>XMM–Newton</i>. 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 <i>kT</i>∼ 1.2 keV and absorbing column <i>N</i><sub>H</sub>= (10.4 ± 0.2) × 10<sup>22</sup> cm<sup>−2</sup>, while different or more complex models are disfavoured. The source persistent X‐ray emission remained fairly constant at ∼3.7 × 10<sup>−12</sup> erg cm<sup>−2</sup> s<sup>−1</sup> 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 <i>P</i>= 7.565 4084(4) s and period derivative <inlineGraphic alt="inline image" location="equation/MNR_19022_mu1.gif" href=""></inlineGraphic> s s<sup>−1</sup>, 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 <i>XMM–Newton</i> 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.</p></abstract></abstractGroup></contentMeta></header></component></istex:document></istex:metadataXml><mods version="3.6"><titleInfo lang="en"><title>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</title></titleInfo><titleInfo type="abbreviated" lang="en"><title>Observations of SGR 1833−0832 and PSR B1830−08</title></titleInfo><titleInfo type="alternative" contentType="CDATA" lang="en"><title>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</title></titleInfo><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Esposito</namePart><affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</affiliation><affiliation>E-mail: paoloesp@oa‐cagliari.inaf.it</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">G. L.</namePart><namePart type="family">Israel</namePart><affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Turolla</namePart><affiliation>Università di Padova, Dipartimento di Fisica, via F. Marzolo 8, I‐35131 Padova, Italy</affiliation><affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">F.</namePart><namePart type="family">Mattana</namePart><affiliation>François Arago Centre, APC (Université Paris Diderot, CNRS/IN2P3, CEA/DSM, Observatoire de Paris), 13 rue Watt, F‐75205 Paris Cedex 13, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Tiengo</namePart><affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">A.</namePart><namePart type="family">Possenti</namePart><affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Zane</namePart><affiliation>Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey RH5 6NT</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">N.</namePart><namePart type="family">Rea</namePart><affiliation>Institut de Ciències de l’Espai (CSIC–IEEC), Campus UAB, Facultat de Ciències, Torre C5‐parell, E‐08193 Barcelona, Spain</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Burgay</namePart><affiliation>INAF – Osservatorio Astronomico di Cagliari, località Poggio dei Pini, strada 54, I‐09012 Capoterra, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">D.</namePart><namePart type="family">Götz</namePart><affiliation>AIM (UMR 7158 CEA/DSM‐CNRS‐Université Paris Diderot) Irfu/Service d’Astrophysique, Saclay, F‐91191 Gif‐sur‐Yvette Cedex, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Mereghetti</namePart><affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Milano, via E. Bassini 15, I‐20133 Milano, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">L.</namePart><namePart type="family">Stella</namePart><affiliation>INAF – Osservatorio Astronomico di Roma, via Frascati 33, I‐00040 Monteporzio Catone, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M. H.</namePart><namePart type="family">Wieringa</namePart><affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J. M.</namePart><namePart type="family">Sarkissian</namePart><affiliation>Australia Telescope National Facility, CSIRO Astronomy and Space Science, PO Box 76, Epping 1710, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.</namePart><namePart type="family">Enoto</namePart><affiliation>Kavli Institute for Particle Astrophysics & Cosmology (KIPAC), SLAC/Stanford University, PO Box 20450, MS 29, Stanford, CA 94309, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">P.</namePart><namePart type="family">Romano</namePart><affiliation>INAF – Istituto di Astrofisica Spaziale e Fisica Cosmica – Palermo, via U. La Malfa 153, I‐90146 Palermo, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T.</namePart><namePart type="family">Sakamoto</namePart><affiliation>NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">Y. E.</namePart><namePart type="family">Nakagawa</namePart><affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">K.</namePart><namePart type="family">Makishima</namePart><affiliation>High Energy Astrophysics Laboratory, Institute of Physical and Chemical Research (RIKEN), Wako, Saitama 351‐0198, Japan</affiliation><affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given"> K.</namePart><namePart type="family">Nakazawa</namePart><affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">H.</namePart><namePart type="family">Nishioka</namePart><affiliation>Department of Physics, University of Tokyo, 7‐3‐1 Hongo, Bunkyo‐ku, Tokyo 113‐0033, Japan</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">C.</namePart><namePart type="family">François‐Martin</namePart><affiliation>Université Denis Diderot – Paris 7, 4 place Jussieu, F‐75252 Paris Cedex 5, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="article" displayLabel="article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-6N5SZHKN-D">article</genre><originInfo><publisher>Blackwell Publishing Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2011-09-01</dateIssued><edition>Accepted 2011 May 6. Received 2011 May 4; in original form 2011 April 12</edition><copyrightDate encoding="w3cdtf">2011</copyrightDate></originInfo><language><languageTerm type="code" authority="rfc3066">en</languageTerm><languageTerm type="code" authority="iso639-2b">eng</languageTerm></language><physicalDescription><extent unit="figures">7</extent><extent unit="tables">3</extent><extent unit="formulas">20</extent><extent unit="references">83</extent><extent unit="linksCrossRef">193</extent></physicalDescription><abstract 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.</abstract><subject lang="en"><genre>keywords</genre><topic>stars: neutron</topic><topic>pulsars: general</topic><topic>X‐rays: individual: PSR B1830−08 (J1833−0827)</topic><topic>X‐rays: individual: SGR 1833−0832</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">0035-8711</identifier><identifier type="eISSN">1365-2966</identifier><identifier type="DOI">10.1111/(ISSN)1365-2966</identifier><identifier type="PublisherID">MNR</identifier><part><date>2011</date><detail type="volume"><caption>vol.</caption><number>416</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>205</start><end>215</end><total>11</total></extent></part></relatedItem><identifier type="istex">43BA55885B793AD60EC9C7DD943FDE0DBD67425B</identifier><identifier type="ark">ark:/67375/WNG-SFP85DFN-W</identifier><identifier type="DOI">10.1111/j.1365-2966.2011.19022.x</identifier><identifier type="ArticleID">MNR19022</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS</accessCondition><recordInfo><recordContentSource authority="ISTEX" authorityURI="https://loaded-corpus.data.istex.fr" valueURI="https://loaded-corpus.data.istex.fr/ark:/67375/XBH-L0C46X92-X">wiley</recordContentSource><recordOrigin>Blackwell Publishing Ltd</recordOrigin></recordInfo></mods><json:item><extension>json</extension><original>false</original><mimetype>application/json</mimetype><uri>https://api.istex.fr/document/43BA55885B793AD60EC9C7DD943FDE0DBD67425B/metadata/json</uri></json:item></metadata><serie></serie></istex></record>Pour manipuler ce document sous Unix (Dilib)
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