Table 4:

Summary of the stellar, orbital and, where determined, the X-ray properties of confirmed or candidate massive WNLh binary systems in the Galaxy and LMC.

ID	Spec.	log(LWR)				kT	Fe sc xxv	References
	type	()	()	(days)	(1033 erg s-1)	(keV)	(Y/N)
CXO J1745-28	WN9h +	6.24	-	189  6	110	0.7+4.7	Y	1, 2
	mid-O?	-	-
		-	-
BAT99-116 (Mk34)	WN5h	-	-	RV var.	240	3.9	-	3, 4
WR25 (HD 93162)	WN6h + ?		-	207.8  0.3	130  10	0.7+2.8	Y	5, 6
BAT99-112 (R136c)	WN5h	-	-	RV var.	110	3.0	-	3, 7
NGC3603 C	WN6ha + ?	6.1	-	8.89  0.01	>40	-	-	8, 9, 10
NGC3603 A1	WN6ha +	6.2	116  31	3.77  ?	>20	-	-	8, 9, 10, 11
	WN6ha	-	89  16
BAT99-99 (Mk39)	O3If*/WN6	-	-	92.6  0.3	13  2	1.6	-	4
WR20a	WN6ha +	6.1	82.7  5.5	3.7	8.0	0.35+1.55	-	12, 13, 14
	WN6ha	6.1	81.9  5.5
BAT99-118 (R144)	WN6h	-	-	RV var.	3.3	2.1	-	3, 4
WR21a	WN6ha +	-	87  6	31.7	0.4-1.6	3.3	-	15, 16
	O4	-	53  4
BAT99-119 (R145)	WN6h	-	-	158.8	1.0	1.6	-	3, 17
WR22 (HD 92740)	WN7h +		55.3  7.3	80.3	0.9	-	-	18, 19
BAT99-103 (R140b)	WN6h	-	-	2.76	0.8  0.3	-	-	4
WR 148 (HD 197406)	WN8h + ?	-	-	4.32	0.6  0.3	-	-	20, 21, 22
BAT99-77	WN7ha	-	-	3.00	0.5	-	-	4
WR12	WN8h + ?	-	-	23.9	0.3	-	-	20, 23, 24
BAT99-12	O3If*/WN6	-	-	3.23	<6.0	-	-	4
BAT99-32	WN6(h)	-	-	1.91	<4.5	-	-	4
BAT99-113 (Mk30)	O3If*/WN6	-	-	4.70	<1.3	-	-	4
BAT99-95 (R135)	WN7h	-	-	2.11	<0.6	-	-	4
Arches-F6	WN9h	6.3	-	-	11.0	1.9	Y	25, 26
R136a3(bl)	WN5h	-	-	-	8.5	4.2	-	3, 7
WR20b	WN6ha	5.9	-	-	6.5	0.5+5.5	-	12, 13
Arches-F7	WN9h	6.25	-	-	7.2	2.1	Y	25, 26
Arches-F9	WN9h	6.3	-	-	4.6	3.3	Y	25, 26

Top panel: summary of the properties of CXO J1745-28 and X-ray bright (>10³⁵ erg s^-1) binary systems. Middle panel: remaining spectroscopically or photometrically confirmed binaries. Bottom panel: binary candidates selected on the basis of their X-ray properties (see Sect. 4). Stars are ordered in terms of decreasing X-ray flux, with errors given for this parameter and orbital period if provided in the original study. We quote dynamical masses only, with those given in italics representing lower limits. Regarding individual sources, WR20a, 22 and 25 have all been flagged as X-ray variable (Naze et al. 2008a; Gosset et al. 2003; Pollock & Corcoran 2006), while the X-ray fluxes given for the Arches sources assume a 1T fit; a similar fit for CXO J1745-28 results in a directly comparable flux (Wang et al. 2006; Mikles et al. 2006). The converse is also true; the 2T (0.9 + 5.8 keV) fit for F9 favoured by Yusef-Zadeh et al. (2002) yields  erg s^-1; we choose to present the 1T fits for all three stars since Yusef-Zadeh et al. (2002) only present a spectral fit for F9. References for the values quoted in the table are: (1) Mikles et al. (2006); (2) Mikles et al. (2008); (3) Townsley et al. (2006); (4) Schnurr et al. (2008a); (5) Gamen et al. (2006); (6) Raassen et al. (2003); (7) Schnurr et al. (2009b); (8) Crowther & Dessart (1998); (9) Schnurr et al. (2008b); (10) Moffat et al. (2002); (11) Moffat et al. (2004); (12) Naze et al. (2008a); (13) Tsujimoto et al. (2007); (14) Rauw et al. (2005); (15) Benaglia et al. (2005); (16) Niemela et al. (2008); (17) Schnurr et al. (2009a); (18) Schweickhardt et al. (1999); (19) Pollock (1987); (20) Hamann et al. (2006); (21) Pollock et al. (1995); (22) Drissen et al. (1986); (23) Lamontagne et al. (1996); (24) Ignace et al. (2000); (25) Martins et al. (2008) and (26) Wang et al. (2006).