Broadband spectral analysis of MXB 1659-298 in its soft and hard state. (arXiv:1906.10960v1 [astro-ph.HE])

Broadband spectral analysis of MXB 1659-298 in its soft and hard state. (arXiv:1906.10960v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Mazzola_S/0/1/0/all/0/1">S. M. Mazzola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Iaria_R/0/1/0/all/0/1">R. Iaria</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gambino_A/0/1/0/all/0/1">A. F. Gambino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marino_A/0/1/0/all/0/1">A. Marino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salvo_T/0/1/0/all/0/1">T. Di Salvo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bassi_T/0/1/0/all/0/1">T. Bassi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanna_A/0/1/0/all/0/1">A. Sanna</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Riggio_A/0/1/0/all/0/1">A. Riggio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burderi_L/0/1/0/all/0/1">L. Burderi</a>

The X-ray transient eclipsing source MXB 1659-298 went in outburst in 1999
and 2015, respectively, during which it was observed by XMM-Newton, NuSTAR and
Swift. Using these observations we studied the broadband spectrum of the source
to constrain the continuum components and to verify the presence of a
reflection component. We analysed the soft and hard state of the source,
finding that the soft state can be modelled with a thermal component associated
with the inner accretion disc plus a Comptonised component. A smeared
reflection component and the presence of an ionised absorber are also requested
in the best-fit model. On the other hand, the direct continuum emission in the
hard state can be described by a Comptonised component with a temperature
larger than 150 keV. Also in this case a reflection component and a ionised
absorber are observed.

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