All Tables

Table 1: Program Stars - observations are from either the 1m JKT (Lennon et al. 1992), 2.5 m INT or 4.2 m WHT (northern) or 1.5 m CTIO (southern). Two estimates of interstellar reddenings are given, based on intrinsic colours adopted from Schmidt-Kaler (1982) and from theoretical continuum fits to UV spectrophotometry and optical photometry (no spectrophotometry was available for HD 194279 or HD 148688). The majority of our targets are probable cluster/association members, whilst absolute magnitudes are adopted for the remainder, based on average values of Magellanic Cloud members from Fitzpatrick (1991), Parker (1993) and Massey et al. (1995), except that HD 190603 is set at M_V=-7.5 mag. References to cluster/association distances are: (a) Brown et al. (1994); (b) Blaha & Humphreys (1989); (c) Baume et al. 1999; (d) Baume et al (2003); (e) Garmany & Stencel (1992); (f) Humphreys (1978).
Table 2: Atomic models for early and mid B supergiants. For each ion F denotes full levels, S super levels, and T the number of bound-bound transitions considered. Most ions are common to all stars, except that high ionization stages are only included in early B supergiant models (shown in italics).
Table 3: Derived non-LTE stellar and wind parameters. Two values are listed for the mass-loss rate of HD 37128 since we fit the minimum and maximum H $\alpha$ profiles of Prinja et al. (2004).
Table 4: Comparison between our derived non-LTE line blanketed temperature scale (in kK) of Galactic early B Ia and Iab supergiants and the unblanketed temperature scale of McErlean et al. (1999), plus recent line blanketed Magellanic Cloud results from Trundle et al. (2004), Trundle & Lennon (2005). For each study the range in temperatures and number of stars studied is indicated. Values for hypergiants are flagged with $\ast$ , and are excluded from our current "mean'' temperature scale for Ia supergiants.
Table 5: Comparison between present results for selected B supergiants and those determined from (a) mid-IR free-free excess method of Barlow & Cohen (1977, BC77), and (b) Kudritzki et al. (1999, K99) following the H $\alpha$ fitting technique of Santolaya-Rey et al. (1997) plus the plane-parallel hydrostatically derived temperature scale from McErlean et al. (1999). For HD 30614 we compare the present results with both Puls et al. (1996, P96) and the recent line blanketed study of Repolust et al. (2004, R04), whilst we also include line blanketed results from Urbaneja (2004, U04) for HD 37128 and HD 38771. Wind velocities in parenthesis relate to adopted values.
Table 6: Individual and mean CNO abundances for Galactic B supergiants (given as $\log N(X)/N({\rm H})+12$ ), where X represents the appropriate element, versus Solar abundances (Asplund et al. 2005), to the nearest 0.05 dex. For all stars He/H = 0.2 by number was adopted. In addition, we show the mean non-LTE abundances obtained from two B1-2Ib supergiants from Gies & Lambert (1992, GL92), four B2Ia supergiant results from Lennon (1994, L94), plus luminosity class II-Ia Galactic A supergiants from Venn (1995, V95).