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We present high-spectral-resolution, optical spectra of the Herbig Be starMWC 147, in which we spectrally resolve several emission lines, including the[O I] lines at 6300 and 6363\deg. Their highly symmetric, double-peaked lineprofiles indicate that the emission originates in a rotating circumstellardisk. We deconvolve the Doppler-broadened [O I] emission lines to obtain ameasure of emission as a function of distance from the central star. Theresulting radial surface brightness profiles are in agreement with a diskstructure consisting of a flat, inner, gaseous disk and a flared, outer, dustdisk. The transition between these components at 2 to 3 AU corresponds to theestimated dust sublimation radius. The width of the double-peaked Mg II line at4481\deg suggests that the inner disk extends to at least 0.10 AU, close to thecorotation radius.

An Inner Gaseous Disk around the Herbig Be Star MWC 147