  In this work we model the expected emission from the molecular line
C17O(J=3-2) in protoplanetary disks, modifying different physical parameters to
obtain distinctive observational signatures. Our aim is to determine the kind
of observations that will allow us to extract information about the physical
parameters of disks. With this purpose we perform a statistical analysis of
principal components and a multiple linear correlation on our set of results
from the models. We also present prospects for future molecular line
observations of protoplanetary disks using SMA and ALMA.
