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We present the first results of a program to characterize the disk andenvelope structure of typical Class 0 protostars in nearby low-mass starforming regions. We use Spitzer IRS mid-infrared spectra, high resolution CARMA230 GHz continuum imaging, and 2-D radiative transfer models to constrain theenvelope structure, as well as the size and mass of the circum-protostellardisk in Serpens FIRS 1. The primary envelope parameters (centrifugal radius,outer radius, outflow opening angle, and inclination) are well constrained bythe spectral energy distribution (SED), including Spitzer IRAC and MIPSphotometry, IRS spectra, and 1.1 mm Bolocam photometry. These together with theexcellent uv-coverage (4.5-500 klam) of multiple antenna configurations withCARMA allow for a robust separation of the envelope and a resolved disk. TheSED of Serpens FIRS 1 is best fit by an envelope with the density profile of arotating, collapsing spheroid with an inner (centrifugal) radius ofapproximately 600 AU, and the millimeter data by a large resolved disk withMdisk~1.0 Msun and Rdisk~300 AU. These results suggest that large, massivedisks can be present early in the main accretion phase. Results for the larger,unbiased sample of Class~0 sources in the Perseus, Serpens, and Ophiuchusmolecular clouds are needed to determine if relatively massive disks aretypical in the Class 0 stage.

Disk and Envelope Structure in Class 0 Protostars: I. The Resolved Massive Disk in Serpens FIRS 1