All Tables

Table 1: Log of observations.
Table 2: Relative line intensities of strong nebular UV lines, as measured from HST STIS long-slit spectra at off-star positions (southern nebular filaments). These values are used for correcting the IUE spectra for nebular contamination.
Table 3: Model atom summary: number of Non-LTE energy levels and line transitions.
Table 4: Parameters which do not vary with the epoch.
Table 5: Parameters of N 66 obtained by model fits to the observed spectra from the different epochs. $\Delta(\log L)$ is the logarithm of the luminosity, relative to $\log L/L_\odot = 4.78$ . Apart from the luminosity scaling, only three different models (A, B, C) are applied. The mass-loss rate is in the usual units, $M_{\odot}~ {\rm yr}^{-1}$ .
Table 6: Some properties of the final models (cf. Table 5).