Spectral analysis of the low-mass X-ray pulsar 4U 1822-371: Reflection component in a high-inclination system

Abstract

The X-ray source 4U 1822-371 is an eclipsing low-mass X-ray binary and X-ray pulsar, hosting a NS that shows periodic pulsations in the X-ray band. The inclination angle of the system is so high that in principle, it should be hard to observe both the direct thermal emission of the central object and the reflection component of the spectrum because they are hidden by the outer edge of the accretion disc. Assuming that the source accretes at the Eddington limit, we analysed non-simultaneous XMM-Newton and NuSTAR observations and studied the average broadband spectrum, with the aim to investigate the presence of a reflection component. No such component has been observed before in a high-inclination source such as 4U 1822-371. We modelled the spectral emission of the source using two different reflection models, Diskline plus Pexriv and the self-consistent model RfxConv. In our analysis, we find significant evidence of a reflection component in the spectrum, in addition to two lines associated with neutral or mildly ionised iron. The continuum spectrum is well fitted by a saturated Comptonisation model and a thermal black-body component emitted by the accretion disc at a lower temperature. We updated the ephemeris, adding two new eclipse times to the most recent ephemeris reported in literature. In our proposed scenario, the source is accreting at the Eddington limit with an intrinsic luminosity of $10^{38}$ erg/s, while the observed luminosity is two orders of magnitude lower. Despite the high inclination, we find that a reflection component is required to fit residuals at the Fe line range and the hard excess observed in the spectrum. The best-fit value of the inner disc radius is still uncertain and model dependent. More observations are therefore needed to confirm these results, which can give important information on this enigmatic and peculiar source.

References in corpus (4)

• New ephemeris of the ADC source 2A 1822-371: a stable orbital-period derivative over 30 years
• A possible cyclotron resonance scattering feature near 0.7 keV in X1822-371
• Detailed study of the X-ray and Optical/UV orbital ephemeris of X1822-371
• Updated orbital ephemeris of the ADC source X 1822-371: a stable orbital expansion over 40 years

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