  We have conducted a survey of the CCS $J_N = 3_2-2_1$ line toward 11 dark
clouds and star-forming regions at 30 arcsec spatial resolution and 0.054 km/s
velocity resolution. CCS was only detected in quiescent clouds, not in active
star-forming regions. The CCS distribution shows remarkable clumpy structure,
and 25 clumps are identified in 7 clouds. Seven clumps with extremely narrow
nonthermal linewidths < 0.1 km/s are among the most quiescent clumps ever
found. The CCS clumps tend to exist around the higher density regions traced by
NH_3 emission or submillimeter continuum sources, and the distribution is not
spherically symmetric. Variation of the CCS abundance was suggested as an
indicator of the evolutionary status of star formation. However, we can only
find a weak correlation between N(CCS) and $n_{H_2,vir}$. The velocity
distributions of CCS clouds reveal that a systematic velocity pattern generally
exists. The most striking feature in our data is a ring structure in the
position-velocity diagram of L1544 with an well-resolved inner hole of 0.04 pc
x 0.13 km/s and an outer boundary of 0.16 pc x 0.55 km/s. This
position-velocity structure clearly indicates an edge-on disk or ring geometry,
and it can be interpreted as a collapsing disk with an infall velocity
$\gtrsim$ 0.1 km/s and a rotational velocity less than our velocity resolution.
Nonthermal linewidth distribution is generally coherent in CCS clouds, which
could be evidence for the termination of Larson's Law at small scales, $\sim$
0.1 pc.
