  Characterizing the spatial and velocity structure of molecular clouds is a
first step towards a better understanding of interstellar turbulence and its
link to star formation. We present observations and structure analysis results
for a large-scale (~ 7.10 deg^2) 13CO J = 2--1 and 12 CO J = 3--2 survey
towards the nearby Perseus molecular cloud observed with the KOSMA 3m
telescope. We study the spatial structure of line-integrated and velocity
channel maps, measuring the $\Delta$-variance as a function of size scale. We
determine the spectral index $\beta$ of the corresponding power spectrum and
study its variation across the cloud and across the lines. We find that the
spectra of all CO line-integrated maps of the whole complex show the same
index, $\beta$ ~ 3.1, for scales between about 0.2 and 3pc, independent of
isotopomer and rotational transition. A complementary 2MASS map of optical
extinction shows a noticeably smaller index of 2.6. In contrast to the overall
region, the CO maps of individual subregions show a significant variation of
$\beta$. The 12CO 3--2 data provide e.g. a spread of indices between 2.9 in
L1455 and 3.5 in NGC1333. In general, active star forming regions show a larger
power-law exponent. We find that the $\Delta$-variance spectra of individual
velocity channel maps are very sensitive to optical depth effects clearly
indicating self-absorption in the densest regions. When studying the dependence
of the channel-map spectra as a function of the velocity channel width, the
expected systematic increase of the spectral index with channel width is only
detected in the blue line wings.This could be explained by a filamentary,
pillar-like structure which is left at low velocities while the overall
molecular gas is swept up by a supernova shock wave.
