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We present 0.3 arcsec resolution observations of the disk around GM Aurigaewith the Submillimeter Array (SMA) at a wavelength of 860 um and with thePlateau de Bure Interferometer at a wavelength of 1.3 mm. These observationsprobe the distribution of disk material on spatial scales commensurate with thesize of the inner hole predicted by models of the spectral energy distribution.The data clearly indicate a sharp decrease in millimeter optical depth at thedisk center, consistent with a deficit of material at distances less than ~20AU from the star. We refine the accretion disk model of Calvet et al. (2005)based on the unresolved spectral energy distribution (SED) and demonstrate thatit reproduces well the spatially resolved millimeter continuum data at bothavailable wavelengths. We also present complementary SMA observations of COJ=3-2 and J=2-1 emission from the disk at 2" resolution. The observed COmorphology is consistent with the continuum model prediction, with twosignificant deviations: (1) the emission displays a larger CO J=3-2/J=2-1 lineratio than predicted, which may indicate additional heating of gas in the upperdisk layers; and (2) the position angle of the kinematic rotation patterndiffers by 11 +/- 2 degrees from that measured at smaller scales from the dustcontinuum, which may indicate the presence of a warp. We note thatphotoevaporation, grain growth, and binarity are unlikely mechanisms forinducing the observed sharp decrease in opacity or surface density at the diskcenter. The inner hole plausibly results from the dynamical influence of aplanet on the disk material. Warping induced by a planet could also potentiallyexplain the difference in position angle between the continuum and CO datasets.

A Spatially Resolved Inner Hole in the Disk around GM Aurigae