A multi-wavelength study of SXP 1062, the long period X-ray pulsar associated with a supernova remnant

A. Gonzalez-Galan, L. M. Oskinova, S. B. Popov, F. Haberl, M. Kuehnel, J. S. Gallagher III, M. P. E. Schurch, M. A. Guerrero

SXP 1062 is a Be X-ray binary located in the Small Magellanic Cloud. It hosts a long-period X-ray pulsar and is likely associated with the supernova remnant MCSNR J0127-7332. In this work we present a multi-wavelength view on SXP 1062 in different luminosity regimes. The data set analyzed in this paper consists of optical OGLE photometric data, an X-ray monitoring campaign with SWIFT, XMM-Newton observations during quiescence of the source, Chandra observations following an X-ray outburst, as well as optical spectroscopy using the RSS/SALT telescope obtained nearly simultaneously with the Chandra observations. During this campaign we observed a tight coincidence of an X-ray and an optical outburst, i.e., a typical Type I outburst as often detected in Be X-ray binaries at periastron passage of the neutron star. To explain the results of our multi-wavelength campaign we propose a simple scenario where the disc of the Be star is observed face-on, while the orbit of the neutron star is inclined with respect to the disc. According to the model of quasi-spherical settling accretion our estimation of the magnetic field of the pulsar in SXP 1062 does not require an extremely strong magnetic field at the present time.

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