XMM-Newton and Swift observations of WZ Sge: spectral and timing analysis

TL;DR

This study analyzes XMM-Newton and Swift data to characterize the spectral and timing properties of WZ Sge in quiescence, revealing a stable spectral shape, a 28.96 s modulation, and variations in intrinsic luminosity over time.

Contribution

It provides the first detailed timing analysis of simultaneous X-ray and UV data for WZ Sge in quiescence, confirming the X-ray modulation period and comparing spectral stability across observations.

Findings

X-ray intensity modulated at ~28.96 s period

Spectral shape remains stable over years

Intrinsic luminosity varies between observations

Abstract

WZ Sagittae is the prototype object of a subclass of dwarf novae, with rare and long (super)outbursts, in which a white dwarf primary accretes matter from a low mass companion. High-energy observations offer the possibility of a better understanding of the disk-accretion mechanism in WZ Sge-like binaries. We used archival XMM-Newton and Swift data to characterize the X-ray spectral and temporal properties of WZ Sge in quiescence. We performed a detailed timing analysis of the simultaneous X-ray and UV light curves obtained with the EPIC and OM instruments on board XMM-Newton in 2003. We employed several techniques in this study, including a correlation study between the two curves. We also performed an X-ray spectral analysis using the EPIC data, as well as Swift/XRT data obtained in 2011. We find that the X-ray intensity is clearly modulated at a period of about 28.96 s, confirming previously published preliminary results. We find that the X-ray spectral shape of WZ Sge remains practically unchanged between the XMM-Newton and Swift observations. However, after correcting for inter-stellar absorption, the intrinsic luminosity is estimated to be about 2.65X10^ 30 erg/s/cm^2 and 1.57X10^30 erg/s/cm^2 in 2003 and 2011, respectively. During the Swift/XRT observation, the observed flux is a factor of about 2 lower than that observed by XMM-Newton, but is similar to the quiescent levels observed various times before the 2001 outburst.