X-Ray and Radio Observations of the Magnetar SGR J1935+2154 during Its 2014, 2015, and 2016 Outbursts

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dc.citation.articleNumber85en_US
dc.citation.journalTitleThe Astrophysical Journalen_US
dc.citation.volumeNumber847en_US
dc.contributor.authorYounes, Georgeen_US
dc.contributor.authorKouveliotou, Chryssaen_US
dc.contributor.authorJaodand, Amrutaen_US
dc.contributor.authorBaring, Matthew G.en_US
dc.contributor.authorvan der Horst, Alexander J.en_US
dc.contributor.authorHarding, Alice K.en_US
dc.contributor.authorHessels, Jason W.T.en_US
dc.contributor.authorGehrels, Neilen_US
dc.contributor.authorGill, Ramandeepen_US
dc.contributor.authorHuppenkothen, Danielaen_US
dc.contributor.authorGranot, Jonathanen_US
dc.contributor.authorGöğüş Ersinen_US
dc.contributor.authorLin, Linen_US
dc.date.accessioned2017-10-19T17:11:53Zen_US
dc.date.available2017-10-19T17:11:53Zen_US
dc.date.issued2017en_US
dc.description.abstractWe analyzed broadband X-ray and radio data of the magnetar SGR J1935+2154 taken in the aftermath of its 2014, 2015, and 2016 outbursts. The source soft X-ray spectrum <10 keV is well described with a blackbody+power-law (BB+PL) or 2BB model during all three outbursts. Nuclear Spectroscopic Telescope Array observations revealed a hard X-ray tail, with a PL photon index Γ = 0.9, extending up to 50 keV, with flux comparable to the one detected <10 keV. Imaging analysis of Chandra data did not reveal small-scale extended emission around the source. Following the outbursts, the total 0.5–10 keV flux from SGR J1935+2154 increased in concordance to its bursting activity, with the flux at activation onset increasing by a factor of ~7 following its strongest 2016 June outburst. A Swift/X-Ray Telescope observation taken 1.5 days prior to the onset of this outburst showed a flux level consistent with quiescence. We show that the flux increase is due to the PL or hot BB component, which increased by a factor of 25 compared to quiescence, while the cold BB component kT = 0.47 keV remained more or less constant. The 2014 and 2015 outbursts decayed quasi-exponentially with timescales of ~40 days, while the stronger 2016 May and June outbursts showed a quick short-term decay with timescales of about four days. Our Arecibo radio observations set the deepest limits on the radio emission from a magnetar, with a maximum flux density limit of 14 μJy for the 4.6 GHz observations and 7 μJy for the 1.4 GHz observations. We discuss these results in the framework of the current magnetar theoretical models.en_US
dc.identifier.citationYounes, George, Kouveliotou, Chryssa, Jaodand, Amruta, et al.. "X-Ray and Radio Observations of the Magnetar SGR J1935+2154 during Its 2014, 2015, and 2016 Outbursts." <i>The Astrophysical Journal,</i> 847, (2017) The American Astronomical Society: https://doi.org/10.3847/1538-4357/aa899a.en_US
dc.identifier.digitalYounes_2017_ApJ_847_85en_US
dc.identifier.doihttps://doi.org/10.3847/1538-4357/aa899aen_US
dc.identifier.urihttps://hdl.handle.net/1911/97804en_US
dc.language.isoengen_US
dc.publisherThe American Astronomical Societyen_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.titleX-Ray and Radio Observations of the Magnetar SGR J1935+2154 during Its 2014, 2015, and 2016 Outburstsen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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