📝 SummarXiv

Abstract

With the discovery of pulsations in some of the ultra-luminous X-ray sources (ULXs), it is quite clear that most of the ULXs harbor either a neutron star or a stellar mass black hole as a compact object accreting at super-Eddington rates. In spite of having such a high accretion rate, the reprocessed emission in the ULX sources is quite meagre compared to that observed in Galactic X-ray binaries, except for some absorption lines in the winds. In this work, we investigate the extent of reprocessed emission in ULXs using three diagnostics: (i) searches for Fe $\rm K\alpha$ lines in bright well-known ULXs and Ultra luminous X-ray Pulsars (ULXPs), (ii) evolution of hardness ratio around the eclipse transitions in the eclipsing ULXs, and (iii) the flux ratio between eclipse and out-of-eclipse (OOE) phases in eclipsing ULXs. We placed the most stringent constraints to date on the upper limits on EW of the iron line, 11--20 eV. Furthermore, we have not observed any significant changes in the hardness ratio during the ingress or egress, while in Galactic eclipsing X-ray binaries, an increase in the hardness ratio is observed during the transitions. Finally, the reprocessing efficiency (eclipse to OOE flux ratio) is found to be larger in ULXs compared to Galactic eclipsing X-ray binaries. Based on these results, we discuss the possibility of a metal-poor or highly ionized environment surrounding the ULXs, which suppresses reprocessed emission features.