All Tables

Table 1: Log of the LBV observations. The signal-to-noise ( S/N) was calculated from the noise in flat regions of the continuum. The spectral resolution was calculated using the FWHM of lines in the arc calibration spectra taken at the time and position of the observed star. All observations, including the archive data, were done at the AAT except P Cyg which was done at the WHT. All data was taken using a 1200R grating, except HD 160529 on 18/9/02 which was done using a 600V grating.
Table 2: Log of the observations of the stars in the spectral atlas. Columns show the same as Table 1, except Col. 4 which shows the MK spectral type of each of the stars. All observations were done at the AAT, and all used a 1200R grating with the exception of HD 183143 which used a 600V grating. All stars were observed on 15/2/04 with the exception of HD 183143 and HD 32034 which were observed on 15/9/02 and 15/8/03 respectively.
Table 3: Effective temperature at observation as calculated from the BC and spectral characteristics methods (see text for details). The two estimates agree well for most of the objects, exceptions are explained below.
Table 4: The observed H $\alpha$ data. The first column denotes whether or not a line-effect was detected; the second column shows the contrast between the line-peak and the continuum to an accuracy of 0.1; the equivalent-widths and FWHM are measured to an accuracy of $\sim$ 5%. The continuum polarization was measured from featureless sections either side of the emission line. As the R 40 data from consecutive nights showed no variability, the data was combined to improve the S/N. The quoted uncertainties do not include the external errors, which we estimate to be 0.1-0.2% (see Sect. 2).