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We present a CARMA 1.3 mm continuum survey toward 9 Class 0 protostars in thePerseus molecular cloud at $\sim$0.3$^{\prime\prime}$ (70 AU) resolution. Thisstudy approximately doubles the number of Class 0 protostars observed withspatial resolutions $<$ 100 AU at millimeter wavelengths, enabling the presenceof protostellar disks and proto-binary systems to be probed. We detectflattened structures with radii $>$ 100 AU around 2 sources (L1448 IRS2 andPer-emb-14) and these sources may be strong disk candidates.Marginally-resolved structures with position angles within 30$^{\circ}$ ofperpendicular to the outflow are found toward 3 protostars (L1448 IRS3C, IRAS03282+3035, and L1448C) and are considered disk candidates. Two others (L1448IRS3B and IRAS 03292+3039) have resolved structure, possibly indicative ofmassive inner envelopes or disks; L1448 IRS3B also has a companion separated by0.9$^{\prime\prime}$ ($\sim$210 AU). IC348-MMS does not have well-resolvedstructure and the candidate first hydrostatic core L1451-MMS is marginallyresolved on 1$^{\prime\prime}$ scales. The strong disk candidate sources werefollowed-up with C$^{18}$O ($J=2\rightarrow1$) observations, detecting velocitygradients consistent with rotation, but it is unclear if the rotation isKeplerian. We compare the observed visibility amplitudes to radiative transfermodels, finding that visibility amplitude ratios suggest a compact component(possibly a disk) is necessary for 5 of 9 Class 0 sources; envelopes alone mayexplain the other 4 systems. We conclude that there is evidence for theformation of large disks in the Class 0 phase with a range of radii and massesdependent upon their initial formation conditions.

A Sub-arcsecond Survey Toward Class 0 Protostars in Perseus: Searching for Signatures of Protostellar Disks