All Tables

Table 1: Observational details of the telescope/instrument combinations used for this paper. The second column presents the complete wavelength coverage of the data, whilst the numbers in parentheses are the number of wavelength settings required to obtain this coverage. The third and fourth columns display the mean signal-to-noise (S/N) ratio and resolution of the data.
Table 2: Details of the Magellanic Cloud observations for FLAMES. Columns denoted by (a) give the number of exposures, where as columns denoted by (b) give the maximum separation in days between exposures. Only single exposures were obtained for the galactic objects and hence they are not included in this table.
Table 3: Atmospheric parameters for B-type stars in NGC 3293 and NGC 4755 as derived from non-LTE TLUSTY model atmospheres. The majority of the data comes from FEROS however those taken with FLAMES are marked with¹. Identifications and spectral classifications are taken from Paper I. Both the initial and corrected atmospheric parameters are shown following the discussion in Sect. 4. The uncertainties in these parameters are typically 1000 K for $T_{\rm eff}$ , 0.20 dex for $\log {g}$ , 3-5 km s^-1 for $\xi$ and 5 km s^-1 for $v \sin i$ .
Table 4: Atmospheric parameters for B-type stars in NGC 2004 and NGC 330 as derived from non-LTE TLUSTY models. Identifications and spectral classifications are taken from Paper II. The uncertainties are as described in Table 3.
Table 5: Results of analysis of HR3468. The first column are the TLUSTY atmospheric parameters and abundances obtained following the procedures described in Sects. 2 and 4, the third column are the TLUSTY results using the parameters from Nieva & Przybilla (2007), and the fourth column are those from Nieva & Przybilla. Nieva & Przybilla estimate the $T_{\rm eff}$ from the C II/C III ionisation equilibrium and derive the microturbulence from the carbon lines not the silicon lines, as done in the TLUSTY analysis. Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex.
Table 6: Absolute abundances of NGC 3293, NGC 4755, NGC 2004 and NGC 330 stars. Presented are the mean of the absolute abundances for each species studied, obtained using the final corrected atmospheric parameters from Tables 3 and 4. Those objects with <0 in the microturbulence column are those for which the microturbulence could not be lowered any further to obtain a Si abundance close to or at the mean silicon abundance of the cluster. Carbon abundances presented here are based solely on the C II 4267 Å line and should only be used as a guide to the relative carbon abundance between the stars (see Sect. 5.3). Uncertainties on the abundances account for both random and systematic errors as discussed in Sect. 5.1. Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex, $T_{\rm eff}$ in K, $\log {g}$ in cm s^-2 and $\xi$ in km s^-1.
Table 7: Comparison of NGC 2004 analyses in this paper with that from Korn et al. (2000, K00). In K00, NGC 2004-022 is labeled with the Robertson (1974) identification - B30. K00 use LTE model atmospheres with NLTE line formations. Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex.
Table 8: Comparison of NGC 330 analyses in this paper with those from Lennon et al. (2003, L03), and Korn et al. (2000, K00). In L03 and K00, NGC 330-002, -004 and -018 are labeled with Robertson (1974) identifications, which are A02, B37 and B30. Fe has been omitted from this comparison as the other analyses did not consider this element. Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex.
Table 9: Weighted average abundances of the FLAMES clusters. Results for the clusters NGC 6611, N11 and NGC 346 are taken from Paper III, except for the Fe abundances which were derived from LTE calculations following the method described in Sect. 5.3. Solar abundances are taken from Asplund et al. (2005). Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex.
Table 10: Effective temperature scales of B-type stars in the Milky Way, LMC and SMC for different luminosity classes. These scales are based on parameters presented in this paper and Paper IV, as well as a number of SMC stars from Dufton et al. (2005). The values in parenthesis are those for which we have no objects in the spectral type bin but for which we could interpolate. The $T_{\rm eff}$ values are presented in units of K.
Table A.1: Absolute Abundances of NGC 3293, NGC 4755, NGC 2004 and NGC 330 stars. The abundances presented below are the mean absolute abundances of each species studied, using the initial atmospheric parameters from Tables 3 and 4. Numbers in the parentheses represent the number of lines of each species observed in the star, only 1 line was considered for C II, Mg II and Si IV, 2 lines for Si II and 3 for Si III. Uncertainties on the abundances account for both random and systematic errors as discussed in Sect. 5.1. Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex.
Table A.2: Absolute Abundances of the NGC 3293, NGC 4755, NGC 2004 and NGC 330 stars. The abundances presented below are the mean absolute abundances of each species studied, using the initial atmospheric parameters from Tables 3 and 4 but with the microturbulence corrected to obtain the mean Cluster silicon abundance in each star Uncertainties on the abundances account for both random and systematic errors as discussed in Sect. 5.1. Abundances are presented as [X] = 12 + $\log$ ([X/H]) in units of dex, and $\xi$ in km s^-1.
Table B.1: Iron equivalent widths and absolute abundances for the objects analysed in Paper IV. The last column contains the weighted mean abundance and uncertainties of the iron abundance in each star.
Table C.1: Equivalent widths and line by line absolute abundances of the NGC 3293 stars:#3, #4, #7. The first and second columns represent the ion and wavelength of the line. There are four columns per star the first represents the equivalent width of the line, the following three are abundance estimates from the lines and they show the results from the 3 steps in determining the abundances as described in Sect. 4. The energy levels and oscillator strenghts relating to the transitions for the metal lines are available online at http://star.pst.qub.ac.uk/~pld/line_identifications.html.
Table C.2: Equivalent widths and line by line absolute abundances of NGC 4755 for stars:#2, #3, #4. Columns are as for Table C.1.
Table C.3: Equivalent widths and line by line absolute abundances of NGC 2004 for stars #3, #5, and #7. Columns are as for Table C.1.
Table C.4: Equivalent Widths and line by line absolute abundances of NGC 330 for stars #2, #3, and #4. Columns are as for Table C.1.