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dc.contributor.authorTiengo, Andrea-
dc.contributor.authorVianello, Giacomo-
dc.contributor.authorEsposito, Paolo-
dc.contributor.authorGiuliani, Andrea-
dc.contributor.authorCostantini, Elisa-
dc.contributor.authorIsrael, Gian Luca-
dc.contributor.authorStella, Luigi-
dc.contributor.authorTurolla, Roberto-
dc.contributor.authorZane, Silvia-
dc.contributor.authorRea, Nanda-
dc.contributor.authorGötz, Diego-
dc.contributor.authorBernardini, Federico-
dc.contributor.authorMoretti, Alberto-
dc.contributor.authorRomano, Patrizia-
dc.contributor.authorEhle, Matthias-
dc.contributor.authorGehrels, Neil-
dc.date.accessioned2011-07-26T07:46:13Z-
dc.date.available2011-07-26T07:46:13Z-
dc.date.issued2010-04-
dc.identifier.citationAstrophysical Journal 710 (1) : 227 (2010)es_ES
dc.identifier.issn0004-637X-
dc.identifier.urihttp://hdl.handle.net/10261/37981-
dc.descriptionPublicado en línea el 15 de enero de 2010.es_ES
dc.description.abstractOn 2009 January 22 numerous strong bursts were detected from the anomalous X-ray pulsar 1E 1547.0-5408. Swift/XRT and XMM-Newton/EPIC observations carried out in the following two weeks led to the discovery of three X-ray rings centered on this source. The ring radii increased with time following the expansion law expected for a short impulse of X-rays scattered by three dust clouds. Assuming different models for the dust composition and grain size distribution, we fit the intensity decay of each ring as a function of time at different energies, obtaining tight constraints on the distance of the X-ray source. Although the distance strongly depends on the adopted dust model, we find that some models are incompatible with our X-ray data, restricting to 4-8 kpc the range of possible distances for 1E 1547.0-5408. The best-fitting dust model provides a source distance of 3.91 ± 0.07 kpc, which is compatible with the proposed association with the supernova remnant G327.24-0.13, and implies distances of 2.2 kpc, 2.6 kpc and 3.4 kpc for the dust clouds, in good agreement with the dust distribution inferred by CO line observations toward 1E 1547.0-5408. However, dust distances in agreement with CO data are also obtained for a set of similarly well-fitting models that imply a source distance of ~5 kpc. A distance of ~4-5 kpc is also favored by the fact that these dust models are already known to provide good fits to the dust-scattering halos of bright X-ray binaries. Assuming N H = 1022 cm–2 in the dust cloud responsible for the brightest ring and a bremsstrahlung spectrum with kT = 100 keV, we estimate that the burst producing the X-ray ring released an energy of 1044-1045 erg in the 1-100 keV band, suggesting that this burst was the brightest flare without any long-lasting pulsating tail ever detected from a magnetar.es_ES
dc.language.isoenges_ES
dc.publisherAmerican Astronomical Societyes_ES
dc.publisherInstitute of Physics Publishinges_ES
dc.rightsopenAccesses_ES
dc.subjectDust, extinctiones_ES
dc.subjectStars: neutrones_ES
dc.subjectX-rays: individual (1E 1547.0-5408)es_ES
dc.subjectX-rays: starses_ES
dc.titleThe dust-scattering X-ray rings of the anomalous X-ray pulsar 1E 1547.0-5408es_ES
dc.typeartículoes_ES
dc.identifier.doi10.1088/0004-637X/710/1/227-
dc.description.peerreviewedPeer reviewedes_ES
dc.relation.publisherversionhttp://dx.doi.org/10.1088/0004-637X/710/1/227es_ES
dc.identifier.e-issn1538-4357-
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