\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}