Table 3:

Synoptic table containing the main results concerning the 6 X-ray binaries (see Fig. 7) identified in the present sample of INTEGRAL sources.

Object	H		H		He II 4686		Optical	AV	d	Spectral
	EW	Flux	EW	Flux	EW	Flux	mag	(mag)	(kpc)	type
IGR J01054-7253	7.15 0.15	16.8 0.3	0.47 0.12	2.0 0.5	in abs.	in abs.	14.81a (V)	0.7	60b	B0 III	0.13 (0.1-2.4)
											700c (3-10)
											77 (20-100)
Swift J0208.4-7428	2.9 0.3	4.5 0.5	in abs.	in abs.	<0.5	<0.2	14.75d (V)	0.18e	60b	B1 III	19 (0.2-12)
											6.5 (3-10)
											108 (15-35)
IGR J08262-3736	65 2	1050 30	5.5 0.4	96 7	in abs.?	in abs.?	12.9f (V)	3.3e	6.1	OB V	0.43 (20-100)
IGR J16327-4940	31.3 0.9	370 11	7.6 0.7	3.8 0.4	in abs.	in abs.	15.5 (R)	11.2	2	OB giant	<0.0072 (20-40)
											0.018 (40-100)
IGR J19113+1533	22.5 1.1	159 8	3.6 0.7	5.9 1.2	<1.2	<1.5	13.3 (R)	7.0	9.1	sgB[e]	<0.15 (20-40)
											<0.28 (40-100)
IGR J16287-5021	52 3	1.75 0.09	19 6	0.23 0.07	15 5	0.16 0.05	19.5g (R)	3.1	<19	--	<1.3 (0.2-12)
											<2.9 (0.3-10)
											<2.8 (2-10)
											<3.8 (17-60)
											<2.3 (20-40)
											<1.2 (40-100)

Notes. EWs are expressed in Å, line fluxes are in units of 10^-15 erg cm^-2 s^-1, whereas X-ray luminosities are in units of 10³⁵ erg s^-1 and the reference band (between round brackets) is expressed in keV.
^(a) From Massey (2002); ^(b) from Harries et al. (2003); ^(c) from Coe et al. (2010); ^(d) from Demers & Irwin (1991); ^(e) only the Galactic reddening along the line of sight was assumed; ^(f) from Pettersson (1987); ^(g) this work.