Left: Comparison between the SED from Bohlin & Gilliland (2004; IUE and HST observations supplemented by a slowly rotating model spectrum both below 127.5 nm and longward of 420 nm) and two rapidly rotating models for Vega’s SED, one viewed from an inclination of 5° (nearly pole on) and one viewed from an inclination of 90° (equator on), from an integration of two intensity maps via eq. (24) for these inclinations. Right: Comparison of the best‐fit brightness distributions for Vega with inclinations of 5° (top) and 90° (bottom). For the equator‐on view, the poles appear 10% fainter than the pole‐on view due to limb darkening.