The Quiescent X-Ray Properties of the Accreting Millisecond X-Ray Pulsar and Eclipsing binary Swift J1749.4-2807

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 ##IMG## [http://ej.iop.org/icons/Entities/sime.gif] {sime 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 ##IMG## [http://ej.iop.org/icons/Entities/sime.gif] {sime 1 × 10 33 ( D /6.7 kpc) 2 erg s –1 . 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 can be adequately 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 ##IMG## [http://ej.iop.org/icons/Entities/lsim.gif] {lsim 2 × 10 33 erg s –1 and constrain its temperature to be ##IMG## [http://ej.iop.org/icons/Entities/lsim.gif] {lsim 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 ##IMG## [http://ej.iop.org/icons/Entities/lsim.gif] {lsim 34% and ##IMG## [http://ej.iop.org/icons/Entities/lsim.gif] {lsim 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.