1. IGR J17503–2636: a candidate supergiant fast X-ray transient
- Author
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Gaurava K. Jaisawal, Enrico Bozzo, Carlo Ferrigno, T. Di Salvo, J. M. Girard, A. Sanna, Luciano Burderi, Ferrigno C., Bozzo E., Sanna A., Jaisawal G.K., Girard J.M., DI Salvo T., and Burderi L.
- Subjects
Accretion ,X-ray transient ,Astrophysics::High Energy Astrophysical Phenomena ,Cyclotron ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,law.invention ,binaries [x-rays] ,X-rays: binaries ,Settore FIS/05 - Astronomia E Astrofisica ,Methods: observational ,Binaries: close ,law ,0103 physical sciences ,Spectral analysis ,010303 astronomy & astrophysics ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,individuals: IGR J17503-2636 [X-rays] ,010308 nuclear & particles physics ,Scattering ,Astronomy and Astrophysics ,Stars: neutron ,Accretion (astrophysics) ,Neutron star ,Accretion disk ,Space and Planetary Science ,Spectral energy distribution ,Supergiant ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
IGR J17503-2636 is a hard X-ray transient discovered by INTEGRAL on 2018 August 11. This was the first ever reported X-ray emission from this source. Following the discovery, follow-up observations were carried out with Swift, Chandra, NICER, and NuSTAR. We report in this paper the analysis and results obtained from all these X-ray data. Based on the fast variability in the X-ray domain, the spectral energy distribution in the 0.5-80 keV energy range, and the reported association with a highly reddened OB supergiant at ~10 kpc, we conclude that IGR J17503-2636 is most likely a relatively faint new member of the supergiant fast X-ray transients. Spectral analysis of the NuSTAR data revealed a broad feature in addition to the typical power-law with exponential roll-over at high energy. This can be modeled either in emission or as a cyclotron scattering feature in absorption. If confirmed by future observations, this feature would indicate that IGR J17503-2636 hosts a strongly magnetized neutron star with B~2e12 G., Submitted to A&A, revised version after referee's comments
- Published
- 2019
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