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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/7141
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dc.contributor.authorMaitra, Chandreyee-
dc.contributor.authorPaul, Biswajit-
dc.contributor.authorHaberl, F-
dc.contributor.authorVasilopoulos, G-
dc.date.accessioned2019-01-29T15:15:07Z-
dc.date.available2019-01-29T15:15:07Z-
dc.date.issued2018-10-11-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 2018, Vol. 480, pL136-L140en_US
dc.identifier.issn0035-8711-
dc.identifier.issn1365-2966 - (online)-
dc.identifier.urihttp://hdl.handle.net/2289/7141-
dc.descriptionOpen Accessen_US
dc.description.abstractWe report the results of AstroSat and NuSTAR observations of the Be/X-ray binary pulsar SXP 15.3 in the Small Magellanic Cloud during its outburst in late 2017, when the source reached a luminosity level of ˜1038 erg s-1, close to the Eddington limit. The unprecedented broad-band coverage of the source allowed us to perform timing and spectral analysis between 3 and 80 keV. The pulse profile exhibits a significant energy dependence, and morphs from a double-peaked profile to a single broad pulse at energies >15 keV. This can be explained by a spectral hardening during an intensity dip seen between the two peaks of the pulse profile. We detect a Cyclotron Resonance Scattering Feature at ˜5 keV in the X-ray spectrum, independent of the choice of the continuum model. This indicates a magnetic field strength of 6 × 1011 G for the neutron star.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_US
dc.relation.urihttp://adsabs.harvard.edu/abs/2018MNRAS.480L.136Men_US
dc.relation.urihttps://arxiv.org/abs/1807.10696en_US
dc.relation.urihttps://doi.org/10.1093/mnrasl/sly141en_US
dc.rights2018 The Author(s)en_US
dc.subjectstars: neutronen_US
dc.subjectpulsars: individual: SMCen_US
dc.subjectgalaxies: individual: SXP 15.3en_US
dc.subjectX-rays: binariesen_US
dc.titleDetection of a cyclotron line in SXP 15.3 during its 2017 outbursten_US
dc.title.alternativeG Vasilopoulosen_US
dc.typeArticleen_US
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