All Tables

Table 1: Broad band JHK photometry for AFGL 2298; the data are from ¹Garcia-Lario et al. (1997), ²Ueta et al. (2001) and ³Pasquali & Comeron (2002).
Table 2: Line identifications and equivalent widths (EWs; given in Å) for the K band ( $\sim$ 2-2.35 $\mu$ m) spectra of AFGL 2298. Note that we have adopted the convention that emission lines are quoted as positive throughout the table. We estimate errors of $\pm$ 10 per cent for the UKIRT spectra and $\pm$ 20 per cent for the spectra from Campo Imperatore. Dates are given in month/year form for brevity; the exact dates of spectra are listed in Sect. 2.2. Note that within the observational uncertainties the EW measured from the 3 low resolution spectra taken between 2002 May-July are identical to one another (hence we only quote a mean value) while the values obtained from 2001 August (PC02) are identical to those obtained in 2001 June (and are also omitted for brevity).
Table 3: Line identification and equivalent widths (given in Å) between $\sim$ 1.1-1.8 $\mu$ m for AFGL 2298 between 2001 August (PC02) and 2002 May. We estimate errors to be $\pm$ 20 per cent of the quoted EW. Note that within the observational uncertainty no variability was apparent over the 3.5 month period between 2002 May-July.
Table 4: Stellar parameters and predicted broadband photometry of AFGL 2298 in 2001 June and 2002 August, derived from comparison to NLTE synthetic spectra (see Sect. 3 for details). Note that both $v_{\exp}$ and the H/He abundance ratio cannot be determined directly from the present dataset and hence were set to values appropiate to high luminosity mid-B supergiants; note that solar Fe & Mg abundances are assumed.