\begin{table}%t3 %\centering \par \caption{\label{table_parameters}Stellar parameters of the analyzed GAUDI B type stars as derived from the best-fit model to the observations found by AnalyseBstar. } \par \begin{tabular}{rllcccrcrccl} \hline \hline \noalign{\smallskip} HD & SpT & \Teff\tablefootmark{a} & \loggc & $\frac{n({\rm He})}{n({\rm H})}$\tablefootmark{b} & $\log \frac{n({\rm Si})}{n({\rm H})}$\tablefootmark{b} & $\xi$\tablefootmark{b}& \vsini & $\vmacro$ & Suspected & Flag\tablefootmark{c} & Remarks\\ number & SIMBAD & (K) & (cgs) & & & (km~s$^{-1}$) & (km~s$^{-1}$) & (km~s$^{-1}$) & pulsator & & \\ \hline 48434 & B0III & 28000 & 3.11 $\pm$ 0.10 & 0.10 & --4.44 & 15 & 62 $\pm$ 3 & 31 & yes & 4 & ELODIE, poor quality spectrum,\\ & & & & & & & & & & & He~lines too strong, Balmer \\ & & & & & & & & & & & lines not well fitted\\ & & & & & & & & & & & due to bumps in blue wings\\ 52382 & B1Ib & 23000 & 2.71 $\pm$ 0.10 & 0.15 & --4.67 & 20 & 56 $\pm$ 5 & 53 & yes & 4 & P Cygni profile $\Ha$ not reproduced,\\ & & & & & & & & & & & $\Hb$ and $\Hg$ not well fitted\\ \par 170580 & B2V & 20000 & 4.10 $\pm$ 0.10 & 0.10 & --4.81 & 6 & 11 $\pm$ 1 & 0 & no & 1 & $N$(He)/$N$(H) lower than solar\\ 44700 & B3V & 17500 & 3.80 $\pm$ 0.10 & 0.10 & --4.93 & 6 & 8 $\pm$ 1 & 0 & no & 1 & $N$(He)/$N$(H) lower than solar\\ 181074 & B3 & 20000 & 3.64 $\pm$ 0.10 & 0.10 & --4.35 & 12 & 133 $\pm$ 7 & 0 & no & 2 & probably B2, fast rotator\\ 45418 & B5 & 16000 & 4.0 $\pm$ 0.20 & 0.10 & --4.49 & 3 & 237 $\pm$ 28 & 0 & no & 3 & \\ 46487 & B5Vn & 14500 & 3.69 $\pm$ 0.10 & 0.15 & --4.49 & 3 & 265 $\pm$ 5 & 0 & no & 3 & \\ 48215 & B5V & 14500 & 3.82 $\pm$ 0.10 & 0.10 & --4.49 & 3 & 98 $\pm$ 3 & 48 & yes & 1 & only Si~II \\ 54596 & B5 & 20000 & 3.31 $\pm$ 0.05 & 0.10 & --4.48 & 6 & 69 $\pm$ 6 & 53 & yes & 2 & only Si~III, probably B2\\ 58973 & B5 & 15000 & 3.43 $\pm$ 0.20 & 0.10 & --4.49 & 3 & 94 $\pm$ 1 & 50 & yes & 1 & \\ 177880 & B5V & 14500 & 3.81 $\pm$ 0.10 & 0.10 & --4.49 & 3 & 49 $\pm$ 1 & 23 & yes & 1 & \\ 178744 & B5Vn & 14500 & 3.71 $\pm$ 0.20 & 0.10 & --4.49 & 12 & 224 $\pm$ 5 & 0 & no & 3 & \\ 43461 & B6V & 13500 & 3.35 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 210 $\pm$ 5 & 0 & no & 3 & \\ 48807 & B7Iab & 12500 & 2.00 $\pm$ 0.10 & 0.10 & --4.28 & 6 & 24 $\pm$ 1 & 27 & yes & 1 & \\ 51360 & B7III & 13500 & 3.12 $\pm$ 0.10 & 0.10 & --3.93 & 3 & 73 $\pm$ 1 & 55 & yes & 1 & very high Si abundance\\ 42677 & B8 & 11000 & 3.55 $\pm$ 0.20 & 0.10 & --4.79 & 6 & 121 $\pm$ 14 & 104 & yes & 2 & probably B9\\ 44720 & B8 & 14000 & 3.96 $\pm$ 0.10 & 0.10 & --4.19 & 3 & 160 $\pm$ 5 & 0 & no & 2 & probably B5 or B6\\ 45153 & B8 & 11000 & 3.66 $\pm$ 0.10 & 0.10 & --4.49 & 3 & 142 $\pm$ 4 & 0 & no & 2 & probably B9\\ 45284 & B8 & 15000 & 4.10 $\pm$ 0.10 & 0.10 & --4.19 & 3 & 52 $\pm$ 5 & 42 & yes & 2 & SPB with magnetic field, skew Si~II lines,\\ & & & & & & & & & & & probably B5 \\ 45397 & B8 & 11500 & 3.59 $\pm$ 0.10 & 0.20 & --4.79 & 6 & 156 $\pm$ 12 & 0 & no & 3 & \\ 45515 & B8V & 11000 & 4.18 $\pm$ 0.10 & 0.15 & --4.49 & 3 & 190 $\pm$ 5 & 0 & no & 2, 3 & probably B9\\ 46616 & B8 & 17500 & 4.20 $\pm$ 0.50 & 0.10 & --4.24 & 3 & 8 $\pm$ 1 & 7 & yes & 5 & He-weak star\\ 47964 & B8III & 11500 & 3.01 $\pm$ 0.20 & 0.10 & --4.79 & 3 & 49 $\pm$ 1 & 44 & yes & 1 & \\ 48497 & B8 & 14000 & 3.70 $\pm$ 0.10 & 0.10 & --4.58 & 3 & 14 $\pm$ 1 & 13 & yes & 4, 6 & $N$(He)/$N$(H) lower than solar\\ 49481 & B8 & 11000 & 2.70 $\pm$ 0.10 & 0.20 & --4.79 & 3 & 9 $\pm$ 1 & 13 & yes & 2, 6 & probably B9\\ 49643 & B8IIIn & 14500 & 3.88 $\pm$ 0.10 & 0.10 & --4.19 & 3 & 296 $\pm$ 2 & 13 & no & 3 &\\ 49886 & B8 & 10000 & 3.30 $\pm$ 0.20 & 0.10 & --4.79 & 6 & 8 $\pm$ 1 & 16 & yes & 4, 6 & \\ 49935 & B8 & 12500 & 3.33 $\pm$ 0.20 & 0.10 & --4.79 & 6 & 92 $\pm$ 9 & 72 & yes & 1 & $\logg$ may be too low?\\ 50251 & B8V & 11500 & 3.00 $\pm$ 0.20 & 0.10 & --4.79 & 3 & 9 $\pm$ 1 & 17 & yes & 1 & emission line \\ & & & & & & & & & & & around Si~III~4813 and Si~IV~4212\\ 50513 & B8 & 11500 & 4.04 $\pm$ 0.10 & 0.10 & --4.79 & 6 & 112 $\pm$ 5 & 80 & yes & 1 & \\ 55793 & B8 & 11000 & 3.05 $\pm$ 0.05 & 0.20 & --4.79 & 3 & 101 $\pm$ 1 & 56 & yes & 2 & probably B9, $\logg$ may be too low?\\ 56446 & B8III & 11500 & 3.21 $\pm$ 0.20 & 0.20 & --4.19 & 3 & 229 $\pm$ 32 & 13 & no & 3 & \\ 170795 & B8 & 15500 & 4.01 $\pm$ 0.10 & 0.10 & --4.49 & 3 & 79 $\pm$ 7 & 37 & yes & 2 & probably B5\\ 171247 & B8IIIsp & 10000 & 2.83 $\pm$ 0.10 & 0.10 & --4.19 & 6 & 66 $\pm$ 2 & 20 & yes & 4 & peculiar line behaviour\\ 173673 & B8 & 10000 & 2.90 $\pm$ 0.10 & 0.20 & --4.49 & 3 & 25 $\pm$ 2 & 26 & yes & 4, 6 & too low $\logg$?\\ 179761 & B8II-III & 12500 & 3.30 $\pm$ 0.05 & 0.10 & --4.49 & 3 & 17 $\pm$ 1 & 12 & yes& 1 & \\ 180760 & B8 & 17000 & 4.05 $\pm$ 0.10 & 0.10 & --4.49 & 6 & 167 $\pm$ 3 & 0 & no & 3 & wrong spectral type?\\ 44321 & B9 & 11000 & 3.62 $\pm$ 0.05 & 0.10 & --4.79 & 6 & 90 $\pm$ 3 & 30 & yes & 1 & \\ 44354 & B9 & 13000 & 3.94 $\pm$ 0.05 & 0.15 & --4.79 & 10 & 121 $\pm$ 5 & 72 & yes & 2 & probably B7 or B8\\ 45050 & B9V & 11500 & 3.86 $\pm$ 0.10 & 0.10 & --4.79 & 10 & 140 $\pm$ 47 & 0 & no & 3 & \\ 45516 & B9 & 13000 & 3.90 $\pm$ 0.10 & 0.10 & --4.49 & 6 & 281 $\pm$ 55 & 12 & no & 3 & \\ 45657 & B9 & 11000 & 4.24 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 153 $\pm$ 36 & 0 & no& 3 & \\ 45709 & B9 & 11000 & 3.95 $\pm$ 0.30 & 0.20 & --4.79 & 10 & 231 $\pm$ 24 & 10 & no & 3 & \\ 45975 & B9 & 11000 & 3.51 $\pm$ 0.10 & 0.15 & --4.79 & 3 & 54 $\pm$ 1 & 56 & yes & 1 & $\vmacro$ too high\\ 46138 & B9 & 12000 & 3.93 $\pm$ 0.05 & 0.10 & --4.19 & 3 & 100 $\pm$ 5 & 0 & no & 4 &\\ 46886 & B9 & 11000 & 3.00 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 16 $\pm$ 3 & 23 & yes & 1 & $\logg$ too low?\\ 47278 & B9 & 10000 & 3.60 $\pm$ 0.05 & 0.10 & --4.79 & 3 & 31 $\pm$ 4 & 25 & yes & 2 & rather A0\\ 48808 & B9 & 12000 & 3.21 $\pm$ 0.10 & 0.10 & --79 & 3 & 47 $\pm$ 14 & 63 & yes & 1 & $\vmacro$ too high, rather B8\\ 48957 & B9 & 12000 & 3.10 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 24 $\pm$ 2 & 23 & yes & 4 & $\Teff$ too low?, wrong spectral type?\\ 49123 & B9 & 10000 & 3.41 $\pm$ 0.05 & 0.10 & --4.79 & 3 & 45 $\pm$ 2 & 0 & no & 2 & rather A0\\ 52312 & B9III & 11000 & 3.04 $\pm$ 0.05 & 0.20 & --4.49 & 3 & 175 $\pm$ 5 & 0 & no & 3 & \\ 53004 & B9 & 11000 & 3.91 $\pm$ 0.20 & 0.10 & --4.79 & 6 & 51 $\pm$ 7 & 54 & yes & 1 & \\ 54761 & B9 & 11500 & 3.11 $\pm$ 0.10 & 0.10 & --4.79 & 6 & 53 $\pm$ 1 & 71 & yes & 1 & Balmer line cores slightly \\ & & & & & & & & & & &refilled, $\logg$ too high?\\ 54929 & B9 & 10000 & 3.11 $\pm$ 0.10 & 0.10 & --4.49 & 3 & 46 $\pm$ 1 & 107 & yes & 4 & fast rotator, difficult to fit, \\ &&&&&&&&&&&too high $\vmacro$\\ 56613 & B9 & 13000 & 3.92 $\pm$ 0.20 & 0.10 & --4.79 & 6 & 91 $\pm$ 7 & 36 & yes & 2 & rather, B7 or B8\\ \hline 172850 & B9 & 11000 & 3.62 $\pm$ 0.10 & 0.10 & --4.49 & 3 & 77 $\pm$ 4 & 0 & no & 1 & \\ 173370 & B9V & 11500 & 3.46 $\pm$ 0.10 & 0.10 & --4.79 & 15 & 282 $\pm$ 8 & 0 & no & 4 & very fast rotator, no Si~lines available,\\ & & & & & & & & & & & double-peaked $\Ha$ profile, \\ & & & & & & & & & & & $\Hb$ refilled on both sides of the line core\\ 173693 & B9 & 10000 & 3.32 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 60 $\pm$ 1 & 22 & yes & 2 & rather A0\\ 174701 & B9 & 12500 & 3.68 $\pm$ 0.10 & 0.15 & --4.49 & 3 & 170 $\pm$ 2 & 10 & no & 3 & \\ 175640 & B9III & 10000 & 3.20 $\pm$ 0.10 & 0.15 & --4.49 & 3 & 7 $\pm$ 1 & 10 & yes & 2 & rather A0\\ 176076 & B9 & 10000 & 3.41 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 42 $\pm$ 2 & 0 & no & 2 & rather A0\\ 176158 & B9 & 13500 & 3.64 $\pm$ 0.10 & 0.15 & --4.79 & 3 & 121 $\pm$ 11 & 0 & no & 2 & rather B8\\ 179124 & B9V & 12000 & 3.45 $\pm$ 0.10 & 0.10 & --4.49 & 15 & 277 $\pm$ 6 & 0 & no & 3 & \\ 181440 & B9III & 11500 & 3.61 $\pm$ 0.50 & 0.10 & --4.49 & 3 & 55 $\pm$ 7 & 32 & yes & 1 & \\ 181690 & B9V & 13000 & 3.42 $\pm$ 0.10 & 0.10 & --4.49 & 6 & 189 $\pm$ 5 & 0 & no & 3 & \\ 182198 & B9V & 11000 & 3.10 $\pm$ 0.10 & 0.10 & --4.79 & 3 & 23 $\pm$ 1 & 12 & yes & 1 & \\ \hline \end{tabular} \tablefoot{In some cases, we need an additional broadening to explain the line profiles. Stars suspected to be pulsators on the basis of their significant $\vmacro$ are indicated. \tablefoottext{a}{The formal uncertainty in the effective temperature is 1000~K for $\Teff > 20,000$~K and $\Teff < 15~000~K$, and 500~K for $\Teff < 15,000~K \le \Teff \le 20~000~K$.} \tablefoottext{b}{The formal uncertainty in the microturbulence and the He and Si abundance is half of the grid step in most cases: 2~km~s$^{-1}$ and 0.025 dex, respectively. For objects below $15~000~K$, we adopt somewhat larger errors (3-$\sigma$ deviation corresponding to 2~grid steps): 3~km~s$^{-1}$, 0.033 and 0.2~dex, respectively.} \tablefoottext{c}{We attribute a flag to each star, to represent the obtained fit quality or problems we encountered during the fitting procedure: 1~--~well-fitted, 2~--~probably a wrong spectral type (about 1000~K or more away from the calibrations, proposed spectral type indicated in the ``remarks''-column), 3~--~no or hardly any Si~lines available, mostly due to rapid rotation, 4~--~not very reliable fit (for other reasons than fast rotation, see ``remarks''), 5~--~He weak/Si strong, 6~--~fitting of $\Ha$, $\Hb$, and $\Hg$ line profiles complicated due to very broad wings that abruptly change into very narrow line cores ($\logg$ may be less accurate).}} \end{table}