Cool Stars 14 - Submitted Abstract # 407
This version created on 1 November 2006

Multiple-Sized Dust Grains in Planetary Resonances in Vega Debris Disk


Thangsamy Velusamy, JPL 
Keith Grogan, JPL
Kenneth Marsh,  JPL


Vega debris disks with central clearing has been directly imaged
at 350 and 450 um using the CSO SHARC II camera with an angular
resolution of ~9 FWHM.. Vega  disk at 350 µm has a broad (50
detected), low surface brightness (<40 mJy/10 beam) disk with
an inner dust ring structure characterized by three  roughly
evenly-spaced peaks, quite different to the highly asymmetric 
morphology seen at 850 um . We use our CSO data and Spitzer data
at 70 um  combined with DISKFIT and dynamical modeling to
predict higher spatial  resolution images, observable by future
submm arrays with high enough dynamic  range, of the resonance
trappings in Vega disk and thereby test (and further  constrain)
the models for the suspected planetary systems. 

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