**Table 5:** Examples of distances of CVs determined by the surface brightness method. Columns (1) to (4) contain information of the secondary star, Col. (5) the contribution of the secondary star to the observed flux at 7500 Å, Cols. (6) and (7) the V and K-magnitudes of the secondary star, Col. (8) the mass used in calculating the distances $d_{\rm 7500}$ , d_V, and d_K in Cols. (9)-(11), and Col. (12) gives the trigonometric distance if available. See text for errors of the quantities in Cols. (4) to (8).
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)	(10)	(11)	(12)
Name	Type	$P_{\rm orb}$	Sp.T.	f₇₅₀₀	V	K	M₂	d₇₅₀₀	d_V	d_K	$1/\pi$
		(h)		(erg cm^-2 s^-1 Å^-1)	(mag)	(mag)	$(M_{\odot})$	(pc)	(pc)	(pc)	(pc)
(1) CVs with trigonometric distances:
U Gem	DN	4.246	M4+	$4.6\times 10^{-15}$		10.95	0.41	$97\pm7$		$94\pm 7$	$100\pm4$
AM Her	AM	3.094	M4-	$2.7\times 10^{-15}$		11.79	0.20	$88\pm8$		$89\pm 8$	$83\pm5^{~1}$
SS Cyg	DN	6.603	K4		12.7		0.80		$156\pm17$		$165\pm12$
RU Peg	DN	8.990	K3		13.35		0.94		$299\pm 50$		$299\pm24$
(2) CVs with f₇₅₀₀ and K-band measurements:
V834Cen	AM	1.692	M5.5	$2.3\times 10^{-16}$		13.85	0.110	$110\pm7$		$104\pm6$
Z Cha	SU	1.788	M6	$1.6\times 10^{-16}$		14.03	0.125	$114\pm8$		$112\pm8$

¹ Mean of the trigonometric distances by Thorstensen (2003) and C. Dahn, $\pi=85\pm 5$ pc, private communication.