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dc.contributor.authorBeri, Aru
dc.contributor.authorTetarenko, B. E.
dc.contributor.authorBahramian, A.
dc.contributor.authorAltamirano, Diego
dc.contributor.authorGandhi, Poshak
dc.contributor.authorSivakoff, G. R.
dc.contributor.authorDegenaar, N.
dc.contributor.authorMiddleton, M. J.
dc.contributor.authorWijnands, R.
dc.contributor.authorHernández Santisteban, J. V.
dc.contributor.authorPaice, John A.
dc.date.accessioned2019-09-11T10:30:04Z
dc.date.available2019-09-11T10:30:04Z
dc.date.issued2019-05
dc.identifier.citationBeri , A , Tetarenko , B E , Bahramian , A , Altamirano , D , Gandhi , P , Sivakoff , G R , Degenaar , N , Middleton , M J , Wijnands , R , Hernández Santisteban , J V & Paice , J A 2019 , ' The black hole X-ray transient Swift J1357.2-0933 as seen with Swift and NuSTAR during its 2017 outburst ' Monthly Notices of the Royal Astronomical Society , vol. 485 , no. 3 , pp. 3064-3075 . https://doi.org/10.1093/mnras/stz616en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 261033197
dc.identifier.otherPURE UUID: 3ef21242-9467-43aa-8c1d-5290af304176
dc.identifier.otherBibCode: 2019MNRAS.485.3064B
dc.identifier.otherScopus: 85063159634
dc.identifier.otherORCID: /0000-0002-6733-5556/work/61370249
dc.identifier.urihttp://hdl.handle.net/10023/18460
dc.description.abstractWe report on observations of black hole Swift J1357.2–0933, a member of the modest population of very faint X-ray transients. This source has previously shown intense dips in the optical light curve, a phenomena that has been linked to the existence of a ‘unique toroidal structure’ in the inner region of the disc, seen at a high inclination. Our observations, carried out by the Neil Gehrels Swift and NuSTAR X-ray observatories, do not show the presence of intense dips in the optical light curves. We find that the X-ray light curves do not show any features that would straightforwardly support an edge-on configuration or high inclination configuration of the orbit. This is similar to what was seen in the X-ray observations of the source during its 2011 outburst. Moreover, the broad-band spectra were well described with an absorbed power-law model without any signatures of cut-off at energies above 10 keV, or any reflection from the disc or the putative torus. Thus, the X-ray data do not support the unique ‘obscuring torus’ scenario proposed for J1357. We also performed a multiwavelength study using the data of X-ray telescope and Ultraviolet/Optical Telescope aboard Swift, taken during the ∼4.5 months duration of the 2017 outburst. This is consistent with what was previously inferred for this source. We found a correlation between the simultaneous X-ray and ultraviolet/optical data and our study suggests that most of the reprocessed flux must be coming out in the ultraviolet.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rightsCopyright © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stz616en
dc.subjectAccretionen
dc.subjectAccretion discsen
dc.subjectBlack hole physicsen
dc.subjectStars: black holesen
dc.subjectX-rays: binariesen
dc.subjectX-rays: individual: Swift J1357.2-0933en
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe black hole X-ray transient Swift J1357.2-0933 as seen with Swift and NuSTAR during its 2017 outbursten
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stz616
dc.description.statusPeer revieweden
dc.identifier.urlhttps://arxiv.org/abs/1903.00146en
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2019MNRAS.485.3064Ben


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