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We report on an X-ray observation of the Be X-ray Binary Pulsar RXJ0059.2-7138, performed by XMM-Newton in March 2014. The 19 ks long observationwas carried out about three months after the discovery of the latest outburstfrom this Small Magellanic Cloud transient, when the source luminosity was Lx ~10$^{38}$ erg/s. A spin period of P=2.762383(5) s was derived, corresponding toan average spin-up of $\dot{P}_{\mathrm{spin}} = -(1.27\pm0.01)\times10^{-12}$s $s^{-1}$ from the only previous period measurement, obtained more than 20years earlier. The time-averaged continuum spectrum (0.2-12 keV) consisted of ahard power-law (photon index ~0.44) with an exponential cut-off at aphase-dependent energy (20-50 keV) plus a significant soft excess below about0.5 keV. In addition, several features were observed in the spectrum: anemission line at 6.6 keV from highly ionized iron, a broad feature at 0.9-1 keVlikely due to a blend of Fe L-shell lines, and narrow emission and absorptionlines consistent with transitions in highly ionized oxygen, nitrogen and ironvisible in the high resolution RGS data (0.4-2.1 keV). Given the differentionization stages of the narrow line components, indicative of photoionizationfrom the luminous X-ray pulsar, we argue that the soft excess in RXJ0059.2-7138 is produced by reprocessing of the pulsar emission in the innerregions of the accretion disc.

Spectral properties of the soft excess pulsar RX J0059.2-7138 during its 2013 outburst