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 " spatial resolution and 0.054 km s(-
1) velocity resolution. CCS was detected only in quiescent clouds, not in a
ctive star-forming regions. The CCS distribution shows remarkable clumpy st
ructure, and 25 clumps are identified in seven clouds. Seven clumps with ex
tremely narrow nonthermal line widths (<0.1 km s(-1)) are among the most qu
iescent clumps ever found. The CCS clumps tend to exist around the higher d
ensity regions traced by NH3 emission or submillimeter continuum sources, a
nd the distribution is not spherically symmetric. Variation of the CCS abun
dance was suggested as an indicator of the evolutionary status of star form
ation. However, we can only find a weak correlation between N(CCS) and n(H2
,vir). The velocity distributions of CCS clouds reveal that a systematic ve
locity pattern generally exists. The most striking feature in our data is a
ring structure in the position-velocity diagram of L1544 with an well-reso
lved inner hole of 0.04 pc x 0.13 km s(-1) and an outer boundary of 0.16 pc
x 0.55 km s(-1). This position-velocity structure clearly indicates an edg
e-on disk or ring geometry, and it can be interpreted as a collapsing disk
with an infall velocity greater than or similar to 0.1 km s(-1) and a rotat
ional velocity less than our velocity resolution. Nonthermal line width dis
tribution is generally coherent in CCS clouds, which could be evidence for
the termination of Larson's Law at small scales, similar to 0.1 pc.