HEG spectrum binned at 5 mÅ at the energy of the Fe Kα emission line. The blue labels indicate the main features present in the spectrum. Although it is not statistically required we also included a Gaussian line to account for the Fe Kβ emission line at 7.06 keV. No clear residuals in emission are present at the expected energy of the Fe xxv and Fe xxvi lines (i.e., at 6.7 keV and 6.97 keV, respectively), which are commonly seen in highly obscured AGN. A clear absorption feature is detected at ~ 6.7 keV, which suggests the presence of a ionized absorber.