Swift J2218.4+1925: a new hard X-ray selected Polar observed with XMM-Newton

TL;DR

This paper presents detailed timing and spectral analysis of Swift J2218.4+1925, a newly identified hard X-ray polar, revealing its orbital period, accretion characteristics, and spectral properties, including a warm absorber and IR excess.

Contribution

It provides the first detailed timing and spectral characterization of Swift J2218.4+1925, confirming it as a low orbital period polar with unique spectral features.

Findings

Detected a 2.16 h orbital period consistent with spectroscopic data.

Identified a warm absorber and neon overabundance in spectra.

Estimated white dwarf mass of 0.97 solar masses and distance of 230-250 pc.

Abstract

Swift J2218.4+1925, a hard X-ray source detected by Swift BAT, has been proposed as a candidate magnetic cataclysmic variable of the polar type from optical spectroscopy. Using XMM-Newton we perform detailed timing and spectral analysis with simultaneous X-ray ($0.3-10$ keV) and optical B band data. We complement the spectral study with archival hard X-ray (14-70 keV) spectra collected by Swift BAT as well as with optical, near and mid-infrared photometry from $SDSS$, $2MASS$ and $WISE$ archive, respectively. A strong periodic X-ray signal at 2.16 h, consistent with the recently determined spectroscopic orbital period, adds Swift J2218.4+1925 to the small group of hard X-ray polars and locates it at the low edge of the orbital period gap. The X-ray pulse profile shows the typical bright and faint phases seen in polars ($\sim 70%$ and $\sim 30%$ of the orbit, respectively). A pronounced dip centred on the bright phase is also detected. It is stronger at lower energies and is mainly produced by photoelectric absorption. A binary inclination $i \sim 40^o - 50^o$ and a magnetic colatitude $\beta \sim 55^o - 64^o$ are estimated. The source appears to accrete over a large area $\sim 24^o$ wide. A multi-temperature optically thin emission with complex absorption well describes the broad-band ($0.3-70$ keV) spectrum, with no signs of a soft X-ray blackbody component. The spectral shape varies with the source rotation reaching plasma temperatures up to 55 keV, hardening at the dip and being softer during the faint phase ($\sim7$ keV). We find the first indication of an absorption edge due to a warm absorber in a polar. Indication of overabundance of neon is found in the RGS spectra. The UV to mid-IR spectral energy distribution reveals an excess in the near and mid-IR, likely due to low cyclotron harmonics. We estimate a WD mass of 0.97 M$_{\odot}$ and a distance of 230-250 pc.