All Tables

Table 7: Comparison of mean rotational velocities for B and Be stars with spectral types B1-B3 and luminosity classes from V to III in the SMC, LMC, and MW. *Values in brackets represent the number of stars in the samples.
Table 9: Comparison by mass sub-samples of the mean rotational velocities in the SMC and LMC B stars. For each sub-sample, the mean age, mean mass, mean $V\sin i$ and the number of stars (N*) are given. No result is given for massive stars in the SMC, because of their small number.
Table 10: Comparison by mass sub-samples of the mean rotational velocities for the samples of Be stars in the SMC, LMC and in the MW. For each sample, the mean age, the mean mass, the mean rotational velocity and the number of stars are given. Note no low-mass Be star in the LMC.
Table 12: Ratio of angular velocity to the breakup angular velocity $\Omega /\Omega _{\rm {c}}$ (%) at the ZAMS for Be stars in the MW and in the SMC (this study) for a 5, 12, 20 $M_{\odot }$ star.
Table 13: Proportions in SMC, LMC, and MW of Be stars (in %) in the upper ( $\frac{\tau}{\tau_{\rm MS}}$ > 0.5) and lower ( $\frac{\tau}{\tau_{\rm MS}}$ $\leq 0.5$ ) MS for masses >12 $M_{\odot }$ and $\leq$ $12~M_{\odot}$ . * values come from from Zorec et al. (2005).
Table 1: Fundamental parameters for O, B, A stars in the SMC. The name, coordinates ( $\alpha$ (2000), $\delta$ (2000)), V magnitude and (B-V) colour index of stars are taken from the EIS catalogues. The effective temperature $T_{\rm eff}$ is given in K, $\log~g$ in dex, $V\sin i$ in km s^-1 and RV in km s^-1. The 1 $\sigma$ error is given for each parameter. The abbreviation "CFP'' is the spectral type and luminosity classification determined from fundamental parameters (method 2), whereas "CEW'' is the spectral type and luminosity classification determined from EW diagrams (method 1). The localization in clusters is indicated in the last column: cl0 for NGC 330 (0h56min19s -72 $^{\circ }$ 27 $^\prime$ 52 $^{\prime \prime }$ ), cl1 for H 86 170 (0h56min21s -72 $^{\circ }$ 21 $^\prime$ 12 $^{\prime \prime }$ ), cl2 for [BS95]78 (0h56min04s -72 $^{\circ }$ 20 $^\prime$ 12 $^{\prime \prime }$ ), cl3 for the association SMC ASS 39 (0h56min6s -72 $^{\circ }$ 18 $^\prime$ 00 $^{\prime \prime }$ ), cl4 for OGLE-SMC109 (0h57min29.8s -72 $^{\circ }$ 15 $^\prime$ 51.9 $^{\prime \prime }$ ), cl5 for NGC299 (0h53min24.5s -72 $^{\circ }$ 11 $^\prime$ 49 $^{\prime \prime }$ ) corrected coordinates, cl6 for NGC306 (0h54min15s -72 $^{\circ }$ 14 $^\prime$ 30 $^{\prime \prime }$ ), cl7 for H86 145 (0h53min37s -72 $^{\circ }$ 21 $^\prime$ 00 $^{\prime \prime }$ ), cl8 for OGLE-SMC99 (0h54min48.24s -72 $^{\circ }$ 27 $^\prime$ 57.8 $^{\prime \prime }$ ).
Table 2: Parameters: $\log(L/L_{\odot}$ ), $M/M_{\odot }$ et $R/R_{\odot }$ interpolated or calculated for our sample of O, B, A stars in the SMC from HR diagrams published in Schaller et al. (1992) for Z=0.001.
Table 3: Apparent fundamental parameters for Be stars in the SMC. The name, coordinates ( $\alpha$ (2000), $\delta$ (2000)), V magnitude and (B-V) colour index of stars are taken from the EIS catalogues, except for 2 stars identified by our catalogue number of emission line stars (MHF[SX]XXXXX). The effective temperature $T_{\rm eff}$ is given in K, $\log~g$ in dex, $V\sin i$ in km s^-1 and RV in km s^-1. For each parameter the 1 $\sigma$ error is given. The abbreviation "CFP'' is the spectral type and luminosity classification determined from fundamental parameters (method 2). The localization in clusters is indicated in the last column: cl0 for NGC 330 (0h56min19s -72 $^{\circ }$ 27 $^\prime$ 52 $^{\prime \prime }$ ), cl1 for H86 170 (0h56min21s -72 $^{\circ }$ 21 $^\prime$ 12 $^{\prime \prime }$ ), cl2 for [BS95]78 (0h56min04s -72 $^{\circ }$ 20 $^\prime$ 12 $^{\prime \prime }$ ), cl3 for the association SMC ASS 39 (0h56min6s -72 $^{\circ }$ 18 $^\prime$ 00 $^{\prime \prime }$ ), cl4 for OGLE-SMC109 (0h57min29.8s -72 $^{\circ }$ 15 $^\prime$ 51.9 $^{\prime \prime }$ ), cl5 for NGC299 (0h53min24.5s -72 $^{\circ }$ 11 $^\prime$ 49 $^{\prime \prime }$ ) corrected coordinates, cl6 for NGC306 (0h54min15s -72 $^{\circ }$ 14 $^\prime$ 30 $^{\prime \prime }$ ), cl7 for H86 145 (0h53min37s -72 $^{\circ }$ 21 $^\prime$ 00 $^{\prime \prime }$ ), cl8 for OGLE-SMC99 (0h54min48.24s -72 $^{\circ }$ 27 $^\prime$ 57.8 $^{\prime \prime }$ ); the letter "k'' followed by a number corresponds to the star number in Keller et al. (1999), and the "#'' indicates that the star was pre-selected in our catalogue of emission line stars (unpublished). In the last column the spectral classification from the SIMBAD database is also given. The last three lines correspond to emission-line objects which are not Be stars.
Table 4: Apparent parameters $\log(L/L_{\odot}$ ), $M/M_{\odot }$ , and $R/R_{\odot }$ interpolated or calculated for Be stars in the SMC from HR diagrams published in Schaller et al. (1992) for Z=0.001.
Table 5: Fundamental parameters for Be stars in the SMC corrected from the effects of fast rotation assuming different rotation rates ( $\Omega /\Omega _{\rm {c}}$ ). The most suitable corrections are those corresponding to $\Omega /\Omega _{\rm {c}}$ = 95%. The units are K for $T_{\rm eff}^{\rm o}$ , dex for $\log g_{\rm o}$ , and km s^-1 for $V\!\sin i^{\rm true}$ .
Table 6: Parameters: $\log(L/L_{\odot}$ ), $M/M_{\odot }$ , $R/R_{\odot }$ , and age of Be stars in the SMC, obtained by interpolation in the evolutionary tracks published in Schaller et al. (1992) with Z=0.001 with fundamental parameters corrected for fast rotation effects with $\Omega /\Omega _{\rm {c}}$ = 95%.
Table 8: Comparison of the rotational velocities for B and Be stars in fields and clusters in the SMC, LMC, and in the MW following statistical tests. Column 3 gives the result of the Student's t-test, Col. 4 gives the $\alpha$ coefficient, Col. 5 gives the probability of difference, and the last column comments on the result following the convention. The comment "limit'' means that the number of stars in samples is low and the value of mean $V\sin i$ may be affected by the distribution of the inclination angles.
Table 11: Comparison of the rotational velocities for Be stars in the SMC, LMC, and in the MW, which have similar age and masses by the Student's t-test. The second column gives the $\alpha$ coefficient, the fourth column gives the probability of difference, and the last column comments on the result following the convention. The comment "limit'' means that the number of stars in samples is low and the value of mean $V\sin i$ may be affected by the distribution of the inclination angles.