The quiescent X-ray properties of the accreting millisecond X-ray pulsar and eclipsing binary Swift J1749.4-2807

TL;DR

This study analyzes the quiescent X-ray properties of Swift J1749.4-2807, a unique eclipsing millisecond pulsar binary, revealing its spectral and timing characteristics and implications for neutron star mass and thermal state.

Contribution

First detailed X-ray analysis of Swift J1749.4-2807 in quiescence, providing insights into its spectral shape, thermal luminosity, and timing properties.

Findings

X-ray luminosity ~1E33 erg/s in quiescence

Spectrum best described by a power law, not a hydrogen atmosphere

No pulsations detected near the neutron star's spin frequency

Abstract

Swift J1749.4-2807 is a transient neutron star low-mass X-ray binary that contains an accreting millisecond X-ray pulsar spinning at 518 Hz. It is the first of its kind that displays X-ray eclipses, which holds significant promise to precisely constrain the mass of the neutron star. We report on a ~105 ks long XMM-Newton observation performed when Swift J1749.4-2807 was in quiescence. We detect the source at a 0.5-10 keV luminosity of ~1E33(D/6.7 kpc)^2 erg/s. The X-ray light curve displays three eclipses that are consistent in orbital phase and duration with the ephemeris derived during outburst. Unlike most quiescent neutron stars, the X-ray spectrum is best described with a simple power law, while a pure-hydrogen atmosphere model does not fit the data. We place an upper limit on the 0.01-100 keV thermal luminosity of the cooling neutron star of <2E33 erg/s and constrain its temperature to be <0.1 keV (for an observer at infinity). Timing analysis does not reveal evidence for X-ray pulsations near the known spin frequency of the neutron star or its first overtone with a fractional rms of <34% and <28%, respectively. We discuss the implications of our findings for dynamical mass measurements, the thermal state of the neutron star and the origin of the quiescent X-ray emission.