\begin{table}%t2
%\centering
\par
  \caption{\label{wrpop}O and WR stellar populations for the galaxies analyzed here in which WR features are detected.} 
  \tiny
  %
\par
\begin{tabular}{l@{\hspace{3pt}}c  c@{\hspace{3pt}}ccc   c@{\hspace{3pt}}cc    cccccc}
    \hline\hline    
	\noalign{\smallskip}
\par
 & & 
\par
\multicolumn{3}{c@{\hspace{4pt}}}{SV98\tablefootmark{a}} & &
\multicolumn{8}{c@{\hspace{4pt}}}{CH06\tablefootmark{b}} \\  
\par
\cline{3-5}
\cline{7-14}
\noalign{\smallskip}
\par
Galaxy & Zone &  
WNL  &  O\tablefootmark{c} &  ${\rm \frac{WNL}{WNL+O}}$ & &
WNL  &  O\tablefootmark{d} &  WCE\tablefootmark{e} & O\tablefootmark{f} & ${\rm \frac{WNL}{WNL+O}}$  
 & ${\rm \frac{WCE}{WCE+O}}$ &     ${\rm \frac{WCE}{WNL}}$  &   ${\rm \frac{WR}{WR+O}}$     &${\rm \frac{WR}{WR+O}}$  \\
\noalign{\smallskip} 
\par
& &  
[$\star$] & [$\star$] & (g) & &
[$\star$] & [$\star$] & 
[$\star$] & [$\star$] & (g,h) & (e)  &  (e) &  (e)    & (i)\\
\par
	\noalign{\smallskip}    
  \tableline
\noalign{\smallskip}
\par
HCG 31          & AC    & 312 & 10798 & 0.028 & &  427 &  9646 &   203 &  7075 & 0.042 & 0.028 & 0.476 & 0.082 &  0.051$^j$ \\ %0.042
                & F2    & 4.6 &   200 & 0.022 & &  7.1 &   192 &\nodata&   192 & 0.036 &\nodata&\nodata&\nodata&  0.015    \\
Mkn 1087        & C     &7181 & 24680 & 0.225 & & 7994 & 16509 &\nodata& 16509 & 0.326 &\nodata&\nodata&\nodata&  0.115    \\
    Haro 15     &  C    & 347 &  8806 & 0.038 & &  432 &  8271 &\nodata&  8271 & 0.050 &\nodata&\nodata&\nodata&  0.037    \\
                &  A    & 173 &  7963 & 0.021 & &  257 &  7542 &\nodata&  7542 & 0.033 &\nodata&\nodata&\nodata&  0.021    \\
    Mkn 1199    &  C    & 960 &  6063 & 0.137 & &  975 &  5985 &   932 &    94 & 0.140 & 0.909 & 0.956 & 0.953 &  0.127$^j$ \\ %0.074
    Mkn 5       &  A    & 2.7 &   143 & 0.018 & & 4.1  &   134 &\nodata&   134 & 0.029 &\nodata&\nodata&\nodata&  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 &\nodata&  7819 & 0.091 &\nodata&\nodata&\nodata&  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 &\nodata& 398 & 17453 & 0.022 & &  660 & 16134 &\nodata& 16134 & 0.039 &\nodata&\nodata&\nodata&  0.021    \\
SBS 0926+606    & A     &  32 &  1987 & 0.016 & &   54 &  1897 &\nodata&  1897 & 0.028 &\nodata&\nodata&\nodata&  0.014    \\
SBS 0948+532    &\nodata& 230 & 11460 & 0.020 & &  358 & 10921 &\nodata& 10921 & 0.032 &\nodata&\nodata&\nodata&  0.017    \\
SBS 1054+365    & C     &  1.1&    52 & 0.020 & &  1.7 &  48.1 &\nodata&   1.7 & 0.034 &\nodata&\nodata&\nodata&  0.023    \\
SBS 1211+540    &\nodata&$<$0.27&$>$14.5&$<$0.018&&$<$0.58&$>$13&\nodata&$>$13 &$<$0.043&\nodata&\nodata&\nodata& \nodata   \\
SBS 1319+579    & A     &  6.0&   321 & 0.018 & &  9.2 &   312 &\nodata& 312   & 0.029 &\nodata&\nodata&\nodata&  0.011    \\
SBS 1415+437    & C     &$<$1.0& $>$62.8&$<$0.016&&$<$2.4&$>$57&\nodata&$>$57  &$<$0.040&\nodata&\nodata&\nodata& \nodata   \\
III Zw 107      & A     & 309 &  5567 & 0.053 & &  420 &  5010 &\nodata&  5010 & 0.077 &\nodata&\nodata&\nodata&  0.041    \\
Tol 9           & C     & 244 &   981 & 0.199 & &  272 &   842 &  127: &    37:& 0.244 & 0.776:& 0.469:& 0.916:&  0.090    \\			
ESO 566-8       &\nodata&8097 & 53392 & 0.132 & & 9574 & 45975 & 4768  & 15839 & 0.172 & 0.231 & 0.498 & 0.475 &  0.073    \\
   NGC 5253     & A     & 0.73&  35.0 & 0.020 & & 1.03 &  34.2 &\nodata&   34.2& 0.029 &\nodata&\nodata&\nodata&  0.012    \\
                & B     & 0.74&  32.0 & 0.022 & & 1.03 &  31.3 &\nodata&   31.3& 0.032 &\nodata&\nodata&\nodata&  0.012    \\
%               & C     & 3.2 &  49.2 & 0.061 & & 4.5  &  42.8 &\nodata& 42.8  & 0.100 &\nodata&\nodata&\nodata&  0.055    \\   
                & C$^k$ & 3.2 &  49.2 & 0.061 & & 4.2  &  42.8 &  0.65 &  37.7 & 0.090 & 0.017 & 0.154 & 0.114 &  0.084$^j$  \\ %0.052, 0.067 
	\noalign{\smallskip}    
  \tableline
  \end{tabular}
\tablefoot{\tablefoottext{a}{We consider  the solar value for the luminosity of a single WNL star to the broad \ion{He}{ii} $\lambda$4686 emission line (SV98 method).}
  \tablefoottext{b}{We consider a metallicity-dependent value for the luminosity of a single WNL star to  the broad \ion{He}{ii} $\lambda$4686 emission line  (CH06 method).}
    \tablefoottext{c}{Total number of O stars after correcting by the ionization of the WNL stars (Eq.~(\ref{GIT00WR})) using the SV98 method.}
  \tablefoottext{d}{Total number of O stars after correcting by the ionization of the WNL stars (Eq.~(\ref{GIT00WR})) using the CH06 method.}
  \tablefoottext{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.} 
  \tablefoottext{f}{Total number of O stars after correcting by the ionization of the WNL and WCE stars (Eq.~(\ref{GIT00WR})) using the CH06 method.}
  \tablefoottext{g}{This coincides with the WR/(WR+O) ratio when no emission from WCE stars is detected.}
  \tablefoottext{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.} 
  \tablefoottext{i}{Using the empirical calibration given by Schaerer \& Vacca (1998, Eq.~(\ref{ewr1})).}
  \tablefoottext{j}{Considering not only the flux of the broad \ion{He}{ii} $\lambda$4686 flux but also the \ion{N}{iii} $\lambda$4640 and \ion{C}{iv}  
$\lambda$4658 fluxes.}
 \tablefoottext{k}{Number of WCE stars computed using the \ion{C}{iv} $\lambda$4658 line. See text for details.}}
\end{table}