\begin{table}%t1 \caption{Sample of galactic early B supergiants from Crowther et~al. (\cite{Crowther}).} \label{targets} %\centerline { \begin{tabular}{rrrlccrlccrrcc} \hline \hline\noalign{\smallskip} \# & HD & Name & Sp. Type & $V$ & $B-V$ & D.M.& Ref. %\footnote{References to the distances modulus, D.M., are (a) Brown et~al. (\cite{Brown}); (b) Blaha \& Humphreys (\cite{Blaha}); (c) Baume et~al. (\cite{Baume1}); (d) Baume et~al. (\cite{Baume2}); (e) Garmany \& Stencel (\cite{Garmany}); (f) Humphreys (\cite{Humphreys}); (g) Crowther et~al. (\cite{Crowther}).} & $T_{\rm eff}$ & $\log g$ & $R_{*}$ & $\varv_{\infty}$ & $\dot{M}$ & $\beta$ \\ & & & & [mag] & [mag] & & & [K] & & [$R_{\odot}$] & [km~s$^{-1}$] & [$10^{-6}~M_{\odot}$~yr$^{-1}$] & \\ \hline 1 & 30614 & $\alpha$ Cam & O9.5 Ia & 4.29 & +0.02 & 10.0 & g & 29~000 & 3.00 & 26.0 & 1560 & 5.00 & 1.5 \\ 2 & 37128 & $\epsilon$ Ori & B0 Ia & 1.70 & $-0.19$ & 7.8 & a & 27~000 & 2.90 & 24.0 & 1910 & 2.50 & 1.5 \\ 3 & 91969 & & B0 Ia & 6.52 & +0.00 & 12.2 & d & 27~500 & 2.95 & 25.3 & 1470 & 1.00 & 1.5 \\ 4 & 94909 & & B0 Ia & 7.34 & +0.48 & 11.5 & g & 27~000 & 2.90 & 25.5 & 1050 & 2.00 & 1.5 \\ 5 & 122879 & & B0 Ia & 6.42 & +0.12 & 11.7 & g & 28~000 & 2.95 & 24.4 & 1620 & 3.00 & 1.5 \\ 6 & 38771 & $\kappa$ Ori & B0.5 Ia & 2.05 & $-0.18$ & 8.0 & a & 26~500 & 2.90 & 22.2 & 1525 & 0.90 & 1.5 \\ 7 & 115842 & & B0.5 Ia & 6.02 & +0.29 & 11.3 & g & 25~500 & 2.85 & 34.2 & 1180 & 2.00 & 1.5 \\ 8 & 152234 & & B0.5 Ia & 5.44 & +0.20 & 11.5 & c & 26~000 & 2.85 & 42.4 & 1450 & 2.70 & 1.5 \\ 9 & 2905 & $\kappa$ Cas & BC0.7 Ia & 4.16 & +0.14 & 10.2 & b & 21~500 & 2.60 & 41.4 & 1105 & 2.00 & 2.0 \\ 10 & 91943 & & B0.7 Ia & 6.73 & +0.07 & 12.2 & d & 24~500 & 2.80 & 26.3 & 1470 & 0.75 & 1.2 \\ 11 & 152235 & & B0.7 Ia & 6.34 & +0.51 & 11.5 & c & 23~000 & 2.65 & 47.1 & 850 & 1.25 & 1.5 \\ 12 & 154090 & & B0.7 Ia & 4.87 & +0.26 & 10.2 & g & 22~500 & 2.65 & 36.0 & 915 & 0.95 & 1.5 \\ 13 & 13854 & & B1 Iab & 6.48 & +0.28 & 11.8 & e & 21~500 & 2.55 & 37.4 & 920 & 0.85 & 2.0 \\ 14 & 91316 & $\rho$ Leo & B1 Iab & 3.85 & $-0.14$ & 10.5 & g & 22~000 & 2.55 & 37.4 & 1110 & 0.35 & 1.0 \\ 15 & 148688 & & B1 Ia & 5.33 & +0.33 & 10.5 & g & 22~000 & 2.60 & 36.7 & 725 & 1.75 & 2.0 \\ 16 & 14956 & & B1.5 Ia & 7.19 & +0.72 & 11.8 & e & 21~000 & 2.50 & 50.6 & 500 & 1.00 & 2.0 \\ 17 & 152236 & $\zeta^{1}$ Sco & B1.5 Ia$^{+}$& 4.73 & +0.48 & 11.5 & c & 18~000 & 2.20 &112.4 & 390 & 6.00 & 2.0 \\ 18 & 190603 & & B1.5 Ia$^{+}$& 5.65 & +0.54 & 10.9 & g & 18~500 & 2.25 & 59.6 & 485 & 2.50 & 3.0 \\ 19 & 14143 & & B2 Ia & 6.66 & +0.50 & 11.8 & e & 18~000 & 2.25 & 52.9 & 645 & 1.05 & 2.0 \\ 20 & 14818 & 10 Per & B2 Ia & 6.25 & +0.30 & 11.8 & e & 18~500 & 2.40 & 46.1 & 565 & 0.55 & 2.0 \\ 21 & 41117 & $\chi^{2}$ Ori & B2 Ia & 4.63 & +0.28 & 10.9 & b & 19~000 & 2.35 & 61.9 & 510 & 0.90 & 2.0 \\ 22 & 194279 & & B2 Ia & 7.05 & +1.02 & 10.4 & f & 19~000 & 2.30 & 44.7 & 550 & 1.05 & 2.5 \\ 23 & 198478 & 55 Cyg & B2.5 Ia & 4.86 & +0.42 & 9.5 & f$^{1}$%\footnote{Humphreys (\cite{Humphreys}) gives for this object a distance of 10.22~mag. To stay conform with CLW, we will use their value of 9.5.} & 16~500 & 2.15 & 40.0 & 470 & 0.23 & 2.0 \\ 24 & 14134 & & B3 Ia & 6.55 & +0.45 & 11.8 & e & 16~000 & 2.05 & 56.7 & 465 & 0.52 & 2.0 \\ 25 & 53138 & $o^{2}$ CMa & B3 Ia & 3.01 & $-0.08$ & 10.2 & g & 15~500 & 2.05 & 65.0 & 865 & 0.36 & 2.0 \\ \hline \end{tabular}} \medskip \par References to the distance modulus, D.M., are (a) Brown et~al. (\cite{Brown}); (b) Blaha \& Humphreys (\cite{Blaha}); (c) Baume et~al. (\cite{Baume1}); (d) Baume et~al. (\cite{Baume2}); (e) Garmany \& Stencel (\cite{Garmany}); (f) Humphreys (\cite{Humphreys}); (g) Crowther et~al. (\cite{Crowther}).\protect\\ $^{1}$The distance modulus for the star HD~198478 is 10.22~mag according to Humphreys (\cite{Humphreys}). To stay conform with CLW, we will use their value of 9.5. \end{table}