SIMBAD references

The distribution of the mass of white dwarfs (WDs) is one of the fundamental questions in the field of cataclysmic variables (CVs). In this work, we make a systematical investigation on the WD masses in two subclass of CVs: intermediate polars (IPs) and non-magnetic CVs in the solar vicinity based on the flux ratios of Fe XXVI-Lyα to Fe XXV-Heα emission lines (I_7.0/I_6.7) from archival XMM-Newton and Suzaku observations. We first verify the (semi-empirical) relations between I_7.0/I_6.7, the maximum emission temperature (T_max) and the WD mass (M_WD) with the mkcflow model based on the apec description and the latest AtomDB. We then introduce a new spectral model to measure M_WD directly based on the above relations. A comparison shows that the derived M_WD is consistent with dynamically measured ones. Finally, we obtain the average WD masses of 58 CVs (including 36 IPs and 22 non-magnetic CVs), which is the largest X-ray selected sample. The average WD masses are <M_WD,IP> = 0.81 ± 0.21 M_☉ and <M_WD,{DN>= 0.81 ±0.21 M_☉ for IPs and non-magnetic CVs, respectively. These results are consistent with previous works.