\begin{table}%t1
\caption{Galactic O-star sample: Stellar and wind parameters adopted (\MV)
and derived using {\sc fastwind}. \teff\ in kK, \Rstar\ in \Rsuna,
\Vr\ and \Vi\ in~\kms, \Mstar\ in \Msuna, $L$ in \Lsun, \Mdot\ in 10$^{-6}$~\Msuna/yr
(terminal velocities \Vi\ from Paper~I). HD~93129A and HD~303308 have 
recently been detected as binary systems but they are treated here as single
stars (see text). Bold face numbers denote $\beta$-values which could be
derived with high precision from emission profiles. Stars with absorption
profiles were fitted with an assumed value of $\beta = 0.80$.
$R_{\rm old}$ is the stellar radius resulting from our new models which was
calculated by means of the "old'' \MV\ values from Paper~I (not tabulated
here).\label{para}}
%\centerline
{\begin{tabular}{l l c c c c c l r c c c r l c}
\hline\hline
Star & Sp.Type & \MV & \teff & \g & $\log g_{\rm true}^{2)}$ & \Rstar & \Y & \Vr & \Vi & \Lum & \Mstar & \Mdot & $\beta$ &$R_{\rm old}$\\
\hline
HD~93129A$^{1)}$ & O2 If$^*$  &--6.74&42.5&3.70&3.71&(22.5) & 0.10&130&3200&(6.17)& (94.8)&      (26.30)  & $\bf 0.80$      & (21.4)\\
HD~93128  & O3 V ((f))        &--5.24&46.5&4.00&4.01& 10.4  & 0.10&100&3100&5.66& 39.8&        2.64   &      0.85$^{3)}$&  10.2 \\
HD~93250  & O3 V ((f))        &--6.14&46.0&3.95&3.96& 15.9  & 0.10&130&3250&6.01& 83.3&        3.45   &      0.90$^{3)}$&  17.6 \\
HD~66811  & O4 I(f)           &--6.32&39.0&3.55&3.59& 19.4  & 0.20&220&2250&5.90& 53.9&        8.80   & $\bf 0.90$      &  16.8 \\
HD~303308$^{1)}$ & O4 V ((f$^+$)) &--5.29&41.0&3.90&3.91&(11.5) &0.075&120&3100&(5.53)& (39.0)&      (1.63)  &      0.80       & (12.6)\\
HD~14947  & O5 If$^+$         &--5.94&37.5&3.45&3.48& 16.8  & 0.20&140&2350&5.70& 30.7&        8.52   & $\bf 0.95 $     &  18.1 \\
HD~15558  & O5 III(f)         &--6.27&41.0&3.80&3.81& 18.2  & 0.10&150&2800&5.93& 78.7&        5.58   &      0.80       &  19.4 \\
HD~193682 & O5 III(f)         &--5.55&40.0&3.60&3.65& 13.1  & 0.20&200&2800&5.60& 27.9&        1.73   &      0.80       &  12.3 \\
HD~15629  & O5 V ((f))        &--5.50&40.5&3.70&3.71& 12.8  & 0.08& 90&3200&5.60& 30.4&        1.28   &      0.80       &  12.8 \\
HD~210839 & O6 I(n) fp        &--6.40&36.0&3.55&3.58& 21.1  & 0.10&200&2250&5.83& 62.2&        6.85   & $\bf 1.00 $     &  20.2 \\
HD~190864 & O6.5 III(f)      &--5.29&37.0&3.55&3.57& 12.3  & 0.15&105&2500&5.41& 20.3&        1.39   &      0.80       &  14.2 \\
HD~192639 & O7 Ib (f)        &--6.10&35.0&3.45&3.47& 18.7  & 0.20&125&2150&5.68& 37.5&        6.32   & $\bf 0.90 $     &  19.6 \\
HD~193514 & O7 Ib (f)        &--6.15&34.5&3.30&3.32& 19.3  & 0.10&105&2200&5.68& 28.2&        3.48   &      0.80       &  19.7 \\
HD~24912  & O7.5 III(n)((f)) &--5.50&35.0&3.50&3.56& 14.0  & 0.15&220&2450&5.42& 26.1&        1.08   &      0.80       &  11.6 \\
HD~203064 & O7.5 III:n ((f)) &--5.74&34.5&3.50&3.60& 15.7  & 0.10&300&2550&5.50& 35.9&        1.41   &      0.80       &  14.1 \\
HD~217086 & O7 V n           &--4.50&36.0&3.50&3.72&  8.6  & 0.15&350&2550&5.05& 14.2&       $\le$0.23   & 0.80       &  10.4 \\
HD~13268  & ON8 V          &--4.77&33.0&3.25&3.48& 10.3  & 0.25&300&2150&5.05& 11.7&       $\le$0.26   & 0.80       &  11.4 \\
HD~210809 & O9 Iab           &--6.20&31.5&3.10&3.12& 21.2  & 0.14&100&2100&5.60& 21.7&        5.30   & $\bf 0.90 $     &  21.2 \\
HD~207198 & O9 Ib            &--5.80&33.0&3.45&3.46& 16.6  & 0.12& 80&2150&5.47& 29.0&        1.79   &      0.80       &  14.5 \\
HD~30614  & O9.5 Ia          &--7.00&29.0&2.97&2.99& 32.5  & 0.10&100&1550&5.83& 37.6&        6.04   & $\bf 1.15 $     &  21.5 \\
HD~209975 & O9.5 Ib          &--6.41&32.0&3.20&3.22& 22.9  & 0.10&100&2050&5.69& 31.4&        2.15   &      0.80       &  16.5 \\
HD~18409  & O9.7 Ib          &--5.58&30.0&2.95&3.04& 16.3  & 0.14&150&1750&5.29& 10.6&        1.02   &      0.85$^{3)}$&  15.7 \\
HD~191423 & O9 III:n$^*$     &--5.24&32.5&3.35&3.60& 12.9  & 0.20&400&1150&5.23& 24.6&       $\le$0.41   & 0.80       &  12.7 \\
HD~149757 & O9 V             &--4.35&32.0&3.65&3.85&  8.9  & 0.17&400&1550&4.87& 20.2&       $\le$0.18   & 0.80       &   8.2 \\
\hline
\end{tabular}}
\smallskip
$^{1)}$ Component of binary system. \\
$^{2)}$ \g\ including centrifugal correction (see text). \\
$^{3)}$ Denotes those absorption profiles for which there are indications that
$\beta$ differs from 0.80 (see text). 
\end{table}