  We present high-resolution spectra and spectroastrometric (SA) measurements
of fundamental rovibrational CO emission from nine nearby ($\lesssim$300 pc)
protoplanetary disks where large inner dust cavities have been observed. The
emission line profiles and SA signals are fit with a slab disk model that
allows the eccentricity of the disk and intensity of the emission to vary as
power laws. Six of the sources are well fit with our model, and three of these
sources show asymmetric line profiles that can be fit by adopting a non-zero
eccentricity. The three other sources have components in either their line
profile or SA signal that are not captured by our disk model. Two of these
sources (V892 Tau, CQ Tau) have multi-epoch observations that reveal
significant variability. CQ Tau and AB Aur have CO line profiles with
centrally-peaked components that are similar to line profiles that have been
interpreted as evidence of molecular gas arising from a wide-angle disk wind.
Alternatively, emission from a circumplanetary disk (CPD) could also account
for this component. The interpretations of these results can be clarified in
the future with additional epochs that will test the variability timescale of
these SA signals. We discuss the utility of using high-resolution spectroscopy
for probing the dynamics of gas in the disk and the scenarios that can give
rise to profiles that are not fit with a simple disk model.
