Variations in the dip properties of the low-mass X-ray binary XB 1254-69 observed with XMM-Newton and INTEGRAL

TL;DR

This study analyzes XMM-Newton and INTEGRAL data of the low-mass X-ray binary XB 1254-69 to understand the variable dipping behavior and its relation to spectral and optical variations, suggesting a tilted accretion disc as a possible cause.

Contribution

It provides a detailed spectral and timing analysis of dipping variability in XB 1254-69 and proposes a new model involving a tilted accretion disc to explain observed phenomena.

Findings

Deep dips correlate with cooler disc temperatures (~1.8 keV).

Optical light curves show sinusoid-like variations with different phases.

Spectral parameters are mostly unaffected by dip depth except for disc temperature.

Abstract

We have analysed data from five XMM-Newton observations of XB 1254-69, one of them simultaneous with INTEGRAL, to investigate the mechanism responsible for the highly variable dips durations and depths seen from this low-mass X-ray binary. Deep dips were present during two observations, shallow dips during one and no dips were detected during the remaining two observations. At high (1-4 s) time resolution ``shallow dips'' are seen to include a few, very rapid, deep dips whilst the ``deep'' dips consist of many similar very rapid, deep, fluctuations. The folded V-band Optical Monitor light curves obtained when the source was undergoing deep, shallow and no detectable dipping exhibit sinusoid-like variations with different amplitudes and phases. We fit EPIC spectra obtained from "persistent" or dip-free intervals with a model consisting of disc-blackbody and thermal comptonisation components together with Gaussian emission features at 1 and 6.6 keV modified by absorption due to cold and photo-ionised material. None of the spectral parameters appears to be strongly correlated with the dip depth except for the temperature of the disc blackbody which is coolest (kT ~ 1.8 keV) when deep dips are present and warmest (kT ~ 2.1 keV) when no dips are detectable. We propose that the changes in both disc temperature and optical modulation could be explained by the presence of a tilted accretion disc in the system. We provide a revised estimate of the orbital period of 0.16388875 +/- 0.00000017 day.