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Home All issues Volume 515 (June 2010) A&A, 515 (2010) A74 Full HTML
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Table 3:

Stellar parameters of the analyzed GAUDI B type stars as derived from the best-fit model to the observations found by AnalyseBstar.

HD 		SpT $T_{\rm eff}$a $\log g_c$ $\frac{n({\rm He})}{n({\rm H})}$b $\log \frac{n({\rm Si})}{n({\rm H})}$b $\xi $b $\nu \sin i$ $\hbox {$\nu _{\rm macro}$ }$ Suspected Flagc Remarks
number SIMBAD (K) (cgs)     (km s-1) (km s-1) (km s-1) pulsator    
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 $\mbox{H$\alpha$ }$ not reproduced,
                      $\mbox{H$\beta$ }$ and $\mbox{H$\gamma$ }$ not well fitted

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 $\hbox{$\log g$ }$ 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, $\hbox{$\log g$ }$ 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 $\hbox{$\log g$ }$?
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 $\hbox {$\nu _{\rm macro}$ }$ 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 $\hbox{$\log g$ }$ 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 $\hbox {$\nu _{\rm macro}$ }$ too high, rather B8
48957 B9 12000 3.10 $\pm$ 0.10 0.10 -4.79 3 24 $\pm$ 2 23 yes 4 $\hbox {$T_{\rm eff}$ }$ 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, $\hbox{$\log g$ }$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 $\hbox {$\nu _{\rm macro}$ }$
56613 B9 13000 3.92 $\pm$ 0.20 0.10 -4.79 6 91 $\pm$ 7 36 yes 2 rather, B7 or B8
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 $\mbox{H$\alpha$ }$ profile,
                      $\mbox{H$\beta$ }$ 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  

Notes. In some cases, we need an additional broadening to explain the line profiles. Stars suspected to be pulsators on the basis of their significant $\hbox {$\nu _{\rm macro}$ }$ are indicated. (a) The formal uncertainty in the effective temperature is 1000 K for $\hbox{$T_{\rm eff}$ }> 20,000$ K and $\hbox{$T_{\rm eff}$ }< 15~000~K$, and 500 K for $\hbox{$T_{\rm eff}$ }< 15,000~K \le \hbox{$T_{\rm eff}$ }\le 20~000~K$. (b) The formal uncertainty in the microturbulence and the He and Si abundance is half of the grid step in most cases: 2 km s-1 and 0.025 dex, respectively. For objects below 15 000 K, we adopt somewhat larger errors (3-$\sigma $ deviation corresponding to 2 grid steps): 3 km s-1, 0.033 and 0.2 dex, respectively. (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 $\mbox{H$\alpha$ }$, $\mbox{H$\beta$ }$, and $\mbox{H$\gamma$ }$ line profiles complicated due to very broad wings that abruptly change into very narrow line cores ( $\hbox{$\log g$ }$ may be less accurate).


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