Table 2:

O and WR stellar populations for the galaxies analyzed here in which WR features are detected.

		SV98a				CH06b
Galaxy	Zone	WNL	Oc			WNL	Od	WCEe	Of
		[]	[]	(g)		[]	[]	[]	[]	(g,h)	(e)	(e)	(e)	(i)
HCG 31	AC	312	10798	0.028		427	9646	203	7075	0.042	0.028	0.476	0.082	0.051j
	F2	4.6	200	0.022		7.1	192	...	192	0.036	...	...	...	0.015
Mkn 1087	C	7181	24680	0.225		7994	16509	...	16509	0.326	...	...	...	0.115
Haro 15	C	347	8806	0.038		432	8271	...	8271	0.050	...	...	...	0.037
	A	173	7963	0.021		257	7542	...	7542	0.033	...	...	...	0.021
Mkn 1199	C	960	6063	0.137		975	5985	932	94	0.140	0.909	0.956	0.953	0.127j
Mkn 5	A	2.7	143	0.018		4.1	134	...	134	0.029	...	...	...	0.022
IRAS 08208+2816	C	1344	33338	0.039		1715	29611	932:	17828:	0.055	0.050:	0.543:	0.129:	0.051
IRAS 08339+6517	#1	658	8444	0.072		782	7819	...	7819	0.091	...	...	...	0.050
POX 4	C	122	4346	0.027		191	4058	113	3464	0.045	0.032	0.590	0.081	0.022
UM 420	...	398	17453	0.022		660	16134	...	16134	0.039	...	...	...	0.021
SBS 0926+606	A	32	1987	0.016		54	1897	...	1897	0.028	...	...	...	0.014
SBS 0948+532	...	230	11460	0.020		358	10921	...	10921	0.032	...	...	...	0.017
SBS 1054+365	C	1.1	52	0.020		1.7	48.1	...	1.7	0.034	...	...	...	0.023
SBS 1211+540	...	<0.27	>14.5	<0.018		<0.58	>13	...	>13	<0.043	...	...	...	...
SBS 1319+579	A	6.0	321	0.018		9.2	312	...	312	0.029	...	...	...	0.011
SBS 1415+437	C	<1.0	>62.8	<0.016		<2.4	>57	...	>57	<0.040	...	...	...	...
III Zw 107	A	309	5567	0.053		420	5010	...	5010	0.077	...	...	...	0.041
Tol 9	C	244	981	0.199		272	842	127:	37:	0.244	0.776:	0.469:	0.916:	0.090
ESO 566-8	...	8097	53392	0.132		9574	45975	4768	15839	0.172	0.231	0.498	0.475	0.073
NGC 5253	A	0.73	35.0	0.020		1.03	34.2	...	34.2	0.029	...	...	...	0.012
	B	0.74	32.0	0.022		1.03	31.3	...	31.3	0.032	...	...	...	0.012
	Ck	3.2	49.2	0.061		4.2	42.8	0.65	37.7	0.090	0.017	0.154	0.114	0.084j

Notes. ^(a) We consider the solar value for the luminosity of a single WNL star to the broad He II 4686 emission line (SV98 method). ^(b) We consider a metallicity-dependent value for the luminosity of a single WNL star to the broad He II 4686 emission line (CH06 method). ^(c) Total number of O stars after correcting by the ionization of the WNL stars (Eq. (10)) using the SV98 method. ^(d) Total number of O stars after correcting by the ionization of the WNL stars (Eq. (10)) using the CH06 method. ^(e) The number of WCE stars and the WCE/(WCE+O), WCE/WNL and WR/(WR+O) ratios were computed assuming the metallicity-dependent (CH06) method. ^(f) Total number of O stars after correcting by the ionization of the WNL and WCE stars (Eq. (10)) using the CH06 method. ^(g) This coincides with the WR/(WR+O) ratio when no emission from WCE stars is detected. ^(h) This considers the total number of O stars after correcting by the ionization of the WNL and WCE stars derived using the CH06 method. ⁽ⁱ⁾ Using the empirical calibration given by Schaerer & Vacca (1998, Eq. (11)). ^(j) Considering not only the flux of the broad He II 4686 flux but also the N III 4640 and C IV 4658 fluxes. ^(k) Number of WCE stars computed using the C IV 4658 line. See text for details.