Spectral analysis of IGR J01572-7259 during its 2016 outburst

TL;DR

This paper presents a detailed timing and spectral analysis of IGR J01572-7259 during its 2016 outburst, revealing energy-dependent pulse profiles, emission lines from ionized elements, and phase-dependent spectral variability.

Contribution

It provides the first detailed spectral and timing analysis of IGR J01572-7259 during its 2016 outburst, highlighting the role of reprocessing and photoionized matter.

Findings

Pulse period of 11.58208 seconds identified.

Energy-dependent double-peaked pulse profile observed.

Emission lines from ionized N, O, Ne, and Fe detected.

Abstract

We report on the results of the $XMM-Newton$ observation of IGR J01572-7259 during its most recent outburst in 2016 May, the first since 2008. The source reached a flux $f \sim 10^{-10}$ erg cm$^{-2}$ s$^{-1}$, which allowed us to perform a detailed analysis of its timing and spectral properties. We obtained a pulse period $P_{\rm spin}$ = 11.58208(2) s. The pulse profile is double peaked and strongly energy dependent, as the second peak is prominent only at low energies and the pulsed fraction increases with energy. The main spectral component is a power-law model, but at low energies we also detected a soft thermal component, which can be described with either a blackbody or a hot plasma model. Both the EPIC and RGS spectra show several emission lines, which can be identified with the transition lines of ionized N, O, Ne, and Fe and cannot be described with a thermal emission model. The phase-resolved spectral analysis showed that the flux of both the soft excess and the emission lines vary with the pulse phase: the soft excess disappears in the first pulse and becomes significant only in the second, where also the Fe line is stronger. This variability is difficult to explain with emission from a hot plasma, while the reprocessing of the primary X-ray emission at the inner edge of the accretion disk provides a realiable scenario. On the other hand, the narrow emission lines can be due to the presence of photoionized matter around the accreting source.