Discovery of two eclipsing X-ray binaries in M51

TL;DR

This paper reports the discovery of two eclipsing X-ray binaries in M51, including their spectral properties, orbital parameters, and the identification of a likely neutron star system through combined X-ray and optical data.

Contribution

It introduces a method to identify luminous neutron star X-ray binaries in high-inclination systems without relying on pulsations or phase-resolved spectroscopy.

Findings

One system is an ultraluminous supersoft source with a 0.1 keV thermal spectrum.

The binary period of the second system is 52.75 hours with a 22% eclipse fraction.

The optical counterpart suggests a massive donor star, implying a high mass ratio and a neutron star primary.

Abstract

We discovered eclipses and dips in two luminous (and highly variable) X-ray sources in M\,51. One (CXOM51 J132943.3$+$471135) is an ultraluminous supersoft source, with a thermal spectrum at a temperature of about 0.1 keV and characteristic blackbody radius of about $10^4$ km. The other (CXOM51 J132946.1$+$471042) has a two-component spectrum with additional thermal-plasma emission; it approached an X-ray luminosity of $10^{39}$erg s$^{-1}$ during outbursts in 2005 and 2012. From the timing of three eclipses in a series of {\it Chandra} observations, we determine the binary period ($52.75 \pm 0.63$ hr) and eclipse fraction ($22\% \pm 0.1\%$) of CXOM51 J132946.1$+$471042. We also identify a blue optical counterpart in archival {\it Hubble Space Telescope} images, consistent with a massive donor star (mass of $\sim$20--35 $M_{\odot}$). By combining the X-ray lightcurve parameters with the optical constraints on the donor star, we show that the mass ratio in the system must be $M_2/M_1 \gtrsim ~18$, and therefore the compact object is most likely a neutron star (exceeding its Eddington limit in outburst). The general significance of our result is that we illustrate one method (applicable to high-inclination sources) of identifying luminous neutron star X-ray binaries, in the absence of X-ray pulsations or phase-resolved optical spectroscopy. Finally, we discuss the different X-ray spectral appearance expected from super-Eddington neutron stars and black holes at high viewing angles.