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We report on the results of the $XMM-Newton$ observation of IGR J01572-7259during its most recent outburst in 2016 May, the first since 2008. The sourcereached a flux $f \sim 10^{-10}$ erg cm$^{-2}$ s$^{-1}$, which allowed us toperform a detailed analysis of its timing and spectral properties. We obtaineda pulse period $P_{\rm spin}$ = 11.58208(2) s. The pulse profile is doublepeaked and strongly energy dependent, as the second peak is prominent only atlow energies and the pulsed fraction increases with energy. The main spectralcomponent is a power-law model, but at low energies we also detected a softthermal component, which can be described with either a blackbody or a hotplasma model. Both the EPIC and RGS spectra show several emission lines, whichcan be identified with the transition lines of ionized N, O, Ne, and Fe andcannot be described with a thermal emission model. The phase-resolved spectralanalysis showed that the flux of both the soft excess and the emission linesvary with the pulse phase: the soft excess disappears in the first pulse andbecomes significant only in the second, where also the Fe line is stronger.This variability is difficult to explain with emission from a hot plasma, whilethe reprocessing of the primary X-ray emission at the inner edge of theaccretion disk provides a realiable scenario. On the other hand, the narrowemission lines can be due to the presence of photoionized matter around theaccreting source.

Spectral analysis of IGR J01572-7259 during its 2016 outburst