Optical identification of X-ray source 1RXS J180431.1-273932 as a magnetic cataclysmic variable

TL;DR

This study identifies the X-ray source 1RXS J180431.1-273932 as a magnetic cataclysmic variable, specifically an intermediate polar, through optical spectroscopy and X-ray spectral analysis, excluding its previous classification as a symbiotic X-ray binary.

Contribution

The paper provides the first optical spectroscopic confirmation of the source as a magnetic CV, clarifying its nature and excluding the symbiotic X-ray binary classification.

Findings

Optical spectroscopy reveals a magnetic CV with specific emission lines.

X-ray spectral analysis indicates a hot bremsstrahlung component and a cooler black-body component.

The source has a spin period of 494 seconds, consistent with a magnetic white dwarf.

Abstract

The X-ray source 1RXS J180431.1-273932 has been proposed as a new member of the symbiotic X-ray binary (SyXB) class of systems, which are composed of a late-type giant that loses matter to an extremely compact object, most likely a neutron star. In this paper, we present an optical campaign of imaging plus spectroscopy on selected candidate counterparts of this object. We also reanalyzed the available archival X-ray data collected with XMM-Newton. We find that the brightest optical source inside the 90% X-ray positional error circle is spectroscopically identified as a magnetic cataclysmic variable (CV), most likely of intermediate polar type, through the detection of prominent Balmer, He I, He II, and Bowen blend emissions. On either spectroscopic or statistical grounds, we discard as counterparts of the X-ray source the other optical objects in the XMM-Newton error circle. A red giant star of spectral type M5 III is found lying just outside the X-ray position: we consider this latter object as a fore-/background one and likewise rule it out as a counterpart of 1RXS J180431.1-273932. The description of the X-ray spectrum of the source using a bremsstrahlung plus black-body model gives temperatures of around 40 keV and around 0.1 keV for these two components, respectively. We estimate a distance of about 450 pc and a 0.2-10 keV X-ray luminosity of about 1.7e32 erg/s for this system and, using the information obtained from the X-ray spectral analysis, a mass of about 0.8 solar masses for the accreting white dwarf (WD). We also confirm an X-ray periodicity of 494 s for this source, which we interpret as the spin period of the WD. In summary, 1RXS J180431.1-273932 is identified as a magnetic CV and its SyXB nature is excluded.