X-ray spectroscopy method of white dwarf mass determination in intermediate polars - External systematic uncertainties

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Table 1.

WD masses in IPs obtained from hard X-ray spectral fitting (M_x, Suleimanov et al. 2019) and from non-X-ray spectroscopy methods, mostly optical (M_opt).

Name	$M_{x}^{a}$ $M_{\mathrm{x}}^{\mathrm{a}}$	M_opt^a
GK Per	0.79 ± 0.01	1.03 $_{- 0.11}^{+ 0.16}$ $_{-0.11}^{+0.16}$ ^b
XY Ari	1.06 ± 0.10	1.21 ± 0.04 ^c
		1.04 ± 0.13 ^d
DO Dra	0.76 ± 0.06	0.99 ± 0.10 ^e
		0.83 ± 0.10 ^f
EX Hya	0.70 ± 0.04	0.78 ± 0.03 ^g
		0.79 ± 0.03 ^h

Notes. a – in solar masses; b – Álvarez-Hernández et al. (2021); c – Álvarez-Hernández et al. (2023); d – Hellier (1997); e – Álvarez-Hernández et al. (2024); f – Haswell et al. (1997); g – Echevarría et al. (2016); h – Beuermann & Reinsch (2008).

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