Table 4:

Derived inclination angles, companion masses and likely nature of the companions.

System	P*		i				Companion
	[d]	[ ]	[deg]	[ ]	[deg]	[ ]
PG 1017-08612	0.07	>0.47	<73	>0.06			MS/BDr
KPD 1930+27526	0.10						WDel
HS 0705+67003	0.10	0.48					MSr,ec
PG 1336-0182,16	0.10	0.459	<90	>0.12			MSr
HW Vir4	0.12	0.53					MSr,ec
PG 1043+76013	0.12		<78	>0.10	90	0.06	WDn
BPS CS 22169-000114	0.18				13	0.09	MSr
PG 1432+15912	0.22				25	0.92	NS/BHn
PG 2345+3182	0.24						WDec not synchronised
PG 1329+15912	0.25				26	0.16	MSr
HE 0532-450311	0.27				19	1.27	NS/BHf
CPD -64 481	0.28				11	0.24	WD
PG 1101+249	0.35				40	0.68	WD/NS/BHf
PG 1232-136	0.36		<14	>6.00	17	3.58	BHf
Feige 4815	0.38	0.52					MS/WD
GD 6875,7	0.38				63	0.32	WDf
KPD 1946+43401	0.40				90	0.58	WDel,ec
HE 0929-042411	0.44				34	0.73	WD/NS/BHf
HE 0230-43239	0.45				61	0.15	MSr
PG 1743+477	0.52		<27	>1.66	32	1.00	NS/BHf
PG 0001+275	0.53				48	0.37	WD
PG 0101+0398	0.57				64	0.33	WDel,n
PG 1248+164	0.73				90	0.12	MS/WD
JL 8210	0.74				51	0.10	MSr
TON S 183	0.83				47	0.40	WDf
PG 1627+017	0.83		<34	>0.50	45	0.32	WD
PG 1116+301	0.86		90		90	0.27	WD
HE 2135-3749	0.92				90	0.29	MS/WD
HE 1421-1206	1.19				90	0.16	MS/WD
HE 1047-0436	1.21				90	0.28	WD
PG 0133+114	1.24	>0.51	90	>0.38			MS/WD/not synchronised?
PG 1512+244	1.27						not synchronised?
[CW83] 1735+22	1.28						not synchronised
HE 2150-0238	1.32						not synchronised
HD 171858	1.63				90	0.37	WD
PG 1716+426	1.78						not synchronised
PB 7352	3.62						not synchronised
CD -24 731	5.85						not synchronised
HE 1448-0510	7.16						not synchronised
PHL 861	7.44						not synchronised

Notes. If the sdB mass couldn't be constrained with other methods the theoretically predicted mass range of was taken from Han et al. (2002,2003). The minimum masses of the companions and maximum inclinations of the binaries were calculated for the lowest possible sdB mass ( , Han et al. 2002,2003). * The orbital periods given here are rounded to the second decimal place. The accurate values are given in Table 1. Additional constraints to clarify the nature of the unseen companions: ^r The detection of a reflection effect from a cool MS/BD or a ⁿ non-detection to exclude this option. The presence of eclipses ^ec or ellipsoidal deformations ^el in the light curves. No signatures of a main-sequence companion within the given mass range are visible in the flux distribution or in the spectrum ^f. These informations are taken from ⁽¹⁾ Bloemen et al. (2010), ⁽²⁾ Charpinet et al. (2008), ⁽³⁾ Drechsel et al. (2001), ⁽⁴⁾ Edelmann (2008), ⁽⁵⁾ Farihi et al. (2005), ⁽⁶⁾ Geier et al. (2007), ⁽⁷⁾ Geier et al. (2010a), ⁽⁸⁾ Geier et al. (2008a), ⁽⁹⁾ Koen (2007), ⁽¹⁰⁾ Koen (2009), ⁽¹¹⁾ Lisker et al. (2005), ⁽¹²⁾ Maxted et al. (2002), ⁽¹³⁾ Maxted et al. (2004), ⁽¹⁴⁾ Østensen (priv. comm.), ⁽¹⁵⁾ van Grootel et al. (2008), and ⁽¹⁶⁾ Vuckovic et al. (2007).