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We report the results provided by the XMM-Newton observation of the X-raybinary pulsar SXP59.0 during its most recent outburst in April 2017. The sourcewas detected at $f_{\rm X}$(0.2-12 keV) = 8$\times 10^{-11}$ erg cm$^{-2}$s$^{-1}$, one of its highest flux levels reported to date. The measured pulseperiod was $P_{\rm spin}$ = 58.949(1) s, very similar to the periods measuredin most of the previous observations. The pulsed emission was clearly detectedover the whole energy range between 0.2 and 12 keV, but the pulse profile isenergy dependent and the pulsed fraction increases as the energy increases.Although the time-averaged EPIC spectrum is dominated by a power-law component(with photon index $\Gamma = 0.76 \pm 0.01$), the data show an evident softexcess, which can be described with the sum of a black-body and a hot thermalplasma component (with temperatures $kT_{\rm BB} = 171^{+11}_{-14}$ eV and$kT_{\rm APEC} = 1.09^{+0.16}_{-0.09}$ keV, respectively). Moreover, the EPICand RGS spectra show narrow emission lines due to N, O, Ne, Mg, and Fe. Thephase-resolved spectral analysis of the EPIC data shows that the flux of theblack-body component varies with the pulse phase, while the plasma component isalmost constant. We show that the black-body component can be attributed to thereprocessing of the primary emission by the optically thick material at theinner edge of the accretion disc, while the hot plasma component is due to adiffuse gas far from the accretion region and the narrow emission lines of theRGS spectrum are most probably due to photoionized matter around the accretingsource.

Spectral analysis of SXP59.0 during its 2017 outburst and properties of the soft excess in X-ray binary pulsars