  We studied the distribution of dense gas in a filamentary molecular cloud
containing several dense clumps. The center of the filament is given by the
dense clump WB673. The clumps are high-mass and intermediate-mass star-forming
regions. We observed CS(2-1), 13CO(1-0), C18O(1-0) and methanol lines at 96GHz
toward WB673 with the Onsala Space Observatory 20-m telescope. We found CS(2-1)
emission in the inter-clump medium so the clumps are physically connected and
the whole cloud is indeed a filament. Its total mass is $10^4$ M$_{\odot}$ and
mass-to-length ratio is 360 M$_{\odot}$pc$^{-1}$ from 13CO(1-0) data.
Mass-to-length ratio for the dense gas is $3.4-34$ M$_{\odot}$pc$^{-1}$ from
CS(2-1) data. The PV-diagram of the filament is V-shaped. We estimated physical
conditions in the molecular gas using methanol lines. Location of the filament
on the sky between extended shells suggests that it could be a good example to
test theoretical models of formation of the filaments via multiple compression
of interstellar gas by supersonic waves.
