  We report the results of a 100 square degree survey of the Taurus Molecular
Cloud region in the J = 1-0 transition of 12CO and 13CO. The image of the cloud
in each velocity channel includes ~ 3 million Nyquist sampled pixels on a 20"
grid. The high sensitivity and large linear dynamic range of the maps in both
isotopologues reveal a very complex, highly structured cloud morphology. There
are large scale correlated structures evident in 13CO emission having very fine
dimensions, including filaments, cavities, and rings. The 12CO emission shows a
quite different structure, with particularly complex interfaces between regions
of greater and smaller column density defining the boundaries of the
largest-scale cloud structures. The axes of the striations seen in the 12CO
emission from relatively diffuse gas are aligned with the direction of the
magnetic field. Using a column density-dependent model for the CO fractional
abundance, we derive the mass of the region mapped to be 24,000 solar masses, a
factor of three greater than would be obtained with canonical CO abundance
restricted to the high column density regions. We determine that half the mass
of the cloud is in regions having column density below 2.1x10^{21} per square
cm. The distribution of young stars in the region covered is highly nonuniform,
with the probability of finding a star in a pixel with a specified column
density rising sharply for N(H2) = 6x10^{21} cm^{-2}. We determine a relatively
low star formation efficiency (mass of young stars/mass of molecular gas),
between 0.3 and 1.2 %, and an average star formation rate during the past 3 Myr
of 8x10^{-5} stars yr^{-1}.
