![The FORS2 optical spectrum of star B, formed from the combination of the single exposures obtained with the 600RI and 600z grisms, is shown in black. The spectrum has been shifted to zero velocity. The R- and I-band magnitudes have been converted to fluxes using the zero-points of Bessell, Castelli & Plez (1998) and are plotted. Regions affected by telluric absorption have been masked. The most prominent spectral lines are indicated. Two synthetic spectra by Munari et al. (2005) are shown which bracket the best-fitting model to the observed spectrum. Both model spectra have [M/H] = −1.0 and has been rotationally broadened by 83 km s−1 and convolved by a truncated Moffat profile representing the observational seeing and slit width. The top light-grey model spectrum has Teff = 4250 K and log g = 4.5 cgs, while the dark-grey model spectrum has Teff = 4000 K and log g = 4.0 cgs. The models have been reddened using the extinction law by Cardelli, Clayton & Mathis (1989) and E(B − V) = 0.04 and then scaled to match the observed spectrum. The model spectra are offset by 0.3 and 0.4 vertical units for clarity.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/460/2/10.1093_mnras_stw1134/2/stw1134fig5.jpeg?Expires=1750466745&Signature=INk3rUrEo6-rWs4cN9yna7mxjI4b4J8rLXm3Z6fZf7Is2dqvd68ofbyFq88ak6dhPbHeQ3AHMSbA3YZMMDTjcYlWDo27UfaVnCniohuEjhvSCoHK3NwJ2eHmwHJR5NlpiIMzIorke7obgj4FJPVaclhvixgbwgP59XT~Hl4mARqDQA-y-5N~2mr2TgMH7x9qczzz24Pip6H~U7LF1PDWyDGFZVGKR1wvlc2A1JF4Yw9NkzoRH6EXUlgUROiluTL0Ehk7R0oS8gKFafVKC4Ya9J4u2LHTHOO8HkqpNHuYqsyrY1GBVARJtyK6EsBrw4bmEgzMSKpJGkbMcxRvIvvMIg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
The FORS2 optical spectrum of star B, formed from the combination of the single exposures obtained with the 600RI and 600z grisms, is shown in black. The spectrum has been shifted to zero velocity. The R- and I-band magnitudes have been converted to fluxes using the zero-points of Bessell, Castelli & Plez (1998) and are plotted. Regions affected by telluric absorption have been masked. The most prominent spectral lines are indicated. Two synthetic spectra by Munari et al. (2005) are shown which bracket the best-fitting model to the observed spectrum. Both model spectra have [M/H] = −1.0 and has been rotationally broadened by 83 km s−1 and convolved by a truncated Moffat profile representing the observational seeing and slit width. The top light-grey model spectrum has Teff = 4250 K and log g = 4.5 cgs, while the dark-grey model spectrum has Teff = 4000 K and log g = 4.0 cgs. The models have been reddened using the extinction law by Cardelli, Clayton & Mathis (1989) and E(B − V) = 0.04 and then scaled to match the observed spectrum. The model spectra are offset by 0.3 and 0.4 vertical units for clarity.
