Please use this identifier to cite or link to this item: http://hdl.handle.net/123456789/3474
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dc.contributor.authorBeri, A.-
dc.contributor.authorSingh, Kulinder Pal-
dc.date.accessioned2020-12-31T10:07:27Z-
dc.date.available2020-12-31T10:07:27Z-
dc.date.issued2020-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, 500(1), pp. 565-575.en_US
dc.identifier.otherhttps://doi.org/10.1093/mnras/staa3254-
dc.identifier.urihttps://academic.oup.com/mnras/article/500/1/565/5934387-
dc.identifier.urihttp://hdl.handle.net/123456789/3474-
dc.descriptionOnly IISERM authors are available in the record.-
dc.description.abstractSwift J0243.6+6124, the first Galactic ultraluminous X-ray pulsar, was observed during its 2017–2018 outburst with AstroSat at both sub- and super-Eddington levels of accretion with X-ray luminosities of LX ∼ 7 × 1037 and 6 × 1038 erg s−1, respectively. Our broad-band timing and spectral observations show that X-ray pulsations at ∼9.85 s have been detected up to 150 keV when the source was accreting at the super-Eddington level. The pulse profiles are a strong function of both energy and source luminosity, showing a double-peaked profile with pulse fraction increasing from ∼10 per cent at 1.65 keV to 40–80 per cent at 70 keV. The continuum X-ray spectra are well modelled with a high-energy cut-off power law (Γ ∼ 0.6–0.7) and one or two blackbody components with temperatures of ∼0.35 and 1.2 keV, depending on the accretion level. No iron line emission is observed at sub-Eddington level, while a broad emission feature at around 6.9 keV is observed at the super-Eddington level, along with a blackbody radius (121–142 km) that indicates the presence of optically thick outflows.en_US
dc.language.isoenen_US
dc.publisherOxford University Pressen_US
dc.subjectPulsars: individual: (Swift J0243.6+6124)en_US
dc.subjectX-rays: binariesen_US
dc.titleAstroSat observations of the first galactic ULX pulsar swift J0243.6+6124en_US
dc.typeArticleen_US
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