Our spatial and spectral analysis of a recent deep Chandra observation of H 1413+117 confirms a microlensing event in a previous Chandra observation of this object performed about 5 years earlier. We present constraints on the structure of H 1413+117 based on the time-scale of this microlensing event. The analysis of the combined spectrum of the images indicates the presence of two emission line peaks at rest-frame energies of 5.35 keV and 6.32 keV and detected at the ≳ 97% and ≳ 99% confidence levels, respectively. The double peaked Fe emission is fit well with an accretion disk-line model, however, the best-fit accretion disk model parameters are neither well constrained nor unique. Another possible interpretation of the Fe emission is fluorescent Fe emission from the back-side of the wind. Additional observations are required to constrain better the model parameters.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science