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Table 2:

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

SV98a

   CH06b  

Galaxy

 Zone WNL Oc ${\rm\frac{WNL}{WNL+O}}$   WNL Od WCEe Of ${\rm\frac{WNL}{WNL+O}}$ ${\rm\frac{WCE}{WCE+O}}$ ${\rm\frac{WCE}{WNL}}$ ${\rm\frac{WR}{WR+O}}$ ${\rm\frac{WR}{WR+O}}$
    [$\star$] [$\star$] (g)   [$\star$] [$\star$] [$\star$] [$\star$] (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 $\lambda $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 $\lambda $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 $\lambda $4686 flux but also the N III $\lambda $4640 and C IV $\lambda $4658 fluxes. (k) Number of WCE stars computed using the C IV $\lambda $4658 line. See text for details.


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