  We present continuum observations at 1.3 and 2.7 mm using the Combined Array
for Research in Millimeter-wave Astronomy (CARMA) toward six protoplanetary
disks in the Taurus molecular cloud: CI Tau, DL Tau, DO Tau, FT Tau, Haro 6-13,
and HL Tau. We constrain physical properties of the disks with Bayesian
inference using two disk models; flared power-law disk model and flared
accretion disk model. Comparing the physical properties, we find that the more
extended disks are less flared and that the dust opacity spectral index (beta)
is smaller in the less massive disks. In addition, disks with a steeper
mid-plane density gradient have a smaller beta, which suggests that grains grow
and radially move. Furthermore, we compare the two disk models quantitatively
and find that the accretion disk model provides a better fit overall. We also
discuss the possibilities of substructures on three extended protoplanetary
disks.
