Hardness ratio diagram of eROSITA detections of HMXBs and HMXB candidates compared to contours showing where the eRASS counterparts of AGN in Kozłowski et al. (2013) with maximum separations of 2^′′ lie, for which 1, 2 and 3σ contours of the entire sample are plotted. The large error bars of fainter sources make a spectral identifi-cation through HR alone impossible. We identify objects #35, #37, and #46 as Be/WD candidates with spectra fit best by absorbed blackbody spectra (see Sect. 7.2.4).