We present new observational data on the small-scale structure of the
Taurus molecular cloud 1 (TMC-1) in the regime of 0.02-0.04 pc and 0.0
4-0.6 M.. Our analysis is based on high-resolution, high-S/N, observat
ions of an 8' x 8' area centered on the ''cyanopolyyne peak'' in the s
outheastern part of the TMC-1 ridge. The observations were made in the
CCS 22 and 45 GHz transitions using NASA's Deep Space Network 70 m an
d 34 m telescopes at the Goldstone facility. The CCS emission in this
region originates in three narrow components centered on LSR velocitie
s of similar to 5.7, 5.9, and 6.1 km s(-1). These components each repr
esent a separate cylindrical feature elongated along the ridge. Among
the three velocity components we identified a total of 45 clumps with
a typical CCS column density of similar to a few x 10(13) cm(-2), an H
-2 density of similar to a few x 10(4) cm(-3), and a mass in the range
of 0.04-0.6 M.. The statistical properties of these small-scale clump
s are compared with those of the larger ''NH3 cores'' in cold clouds a
nd ''CS cores'' in the hotter Orion region. The CCS clumps in TMC-1 ar
e found to conform to Larson's scaling laws (relating observed line wi
dth to clump size) derived from the larger cores down to the small-sca
le regime (0.02 pc and 0.04 M.). These clumps represent a regime in wh
ich microturbulence is small, amounting to similar to 10% of the therm
al pressure inside a clump. Of the 45 clumps, only five appear to be g
ravitationally unstable to collapse. All unbound clumps have masses le
ss than 0.2 M., while bound clumps have masses in the range 0.15-0.6 M
.. The 6.1 km s(-1) velocity feature contains all the gravitationally
unstable clumps and is the most likely site for future star formation.