Timing and Spectral Analysis of the Unusual X-Ray Transient XTE J0421+560/CI Camelopardalis

TL;DR

This study provides a detailed spectral and timing analysis of the 2003 X-ray observation of the unusual high-mass X-ray binary XTE J0421+560/CI Cam, revealing complex iron line features and potential circumnuclear material structures.

Contribution

The paper offers the first detailed spectral decomposition and timing analysis of XTE J0421+560, suggesting the presence of circumstellar material and estimating the location of iron emission regions.

Findings

Detection of a flat power-law spectrum with high absorption

Decomposition of iron line into three components

Marginal evidence for a 10 ks lag in Fe-Kα line

Abstract

We present a detailed X-ray study of the 2003 XMM-Newton observation of the High Mass X-ray Binary XTE J0421+560/CI Cam. The continuum of the X-ray spectrum is well described by a flat power law (Gamma=1.0+/-0.2) with a large intrinsic absorbing column (N_H=(4.4+/-0.5)\times10^{23} cm^{-2}). We have decomposed the broad iron line into 3 separate components: Fe\textsc{i}-K$\alpha$, Fe\textsc{i}-K$\beta$ and Fe\textsc{xxiv-xxv}K$\alpha$. It is unclear how both neutral and almost fully ionised iron can exist simultaneously, however we suggest this could be evidence that the compact object is embedded in the circumstellar material. This doesn't appear to be consistent with the X-ray flux and spectrum of the source, which has remained essentially unchanged since the initial outburst. The iron abundance implied by the ratio of the neutral Fe-K$\alpha$ and Fe-K$\beta$ is compatible with solar. We search for lags in the neutral Fe-K$\alpha$ with respect to the continuum and find marginal evidence for a lag at ~10 ks. We interpret this as the light crossing time of the torus which would suggest that the neutral iron is located at a radius of 10 AU. This result depends on several assumptions including the distance to the system, the inclination, the mass of system and the orbital period none of which are known with any great certainty. Better constraints on these system parameters and further observations of this system are required to confirm this result. We discuss the nature of this system in light of our results and place it in context with other binary B[e] stars.