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Clumpy structure in the debris disk around Vega has been previously reportedat millimeter wavelengths and attributed to concentrations of dust grainstrapped in resonances with an unseen planet. However, recent imaging at similarwavelengths with higher sensitivity has disputed the observed structure. Wepresent three new millimeter-wavelength observations that help to resolve thepuzzling and contradictory observations. We have observed the Vega system withthe Submillimeter Array (SMA) at a wavelength of 880 um and angular resolutionof 5"; with the Combined Array for Research in Millimeter-wave Astronomy(CARMA) at a wavelength of 1.3 mm and angular resolution of 5"; and with theGreen Bank Telescope (GBT) at a wavelength of 3.3 mm and angular resolution of10". Despite high sensitivity and short baselines, we do not detect the Vegadebris disk in either of the interferometric data sets (SMA and CARMA), whichshould be sensitive at high significance to clumpy structure based onpreviously reported observations. We obtain a marginal (3-sigma) detection ofdisk emission in the GBT data; the spatial distribution of the emission is notwell constrained. We analyze the observations in the context of severaldifferent models, demonstrating that the observations are consistent with asmooth, broad, axisymmetric disk with inner radius 20-100 AU and width >50 AU.The interferometric data require that at least half of the 860 um emissiondetected by previous single-dish observations with the James Clerk MaxwellTelescope be distributed axisymmetrically, ruling out strong contributions fromflux concentrations on spatial scales of <100 AU. These observations supportrecent results from the Plateau de Bure Interferometer indicating that previousdetections of clumpy structure in the Vega debris disk were spurious.

Confirming the Primarily Smooth Structure of the Vega Debris Disk at Millimeter Wavelengths