  A survey of radio recombination lines (RLs) in the Galactic plane ($l = $
332\deg $\to$ 89\deg) near 327 MHz made using the Ooty Radio Telescope (ORT)
has detected carbon RLs from all the positions in the longitude range 0\deg $<
l < $ 20\deg and from a few positions at other longitudes. The carbon RLs
detected in this survey originate from ``diffuse'' \CII regions. Comparison of
the \lv diagram and the radial distribution of carbon line emission with those
obtained from hydrogen RLs near 3 cm from \HII regions and ``intense'' \CO
emission indicates that the distribution of the diffuse \CII regions in the
inner Galaxy is similar to that of spiral arm components. Towards several
observed positions, the central velocities of the carbon RLs coincide with \HI
self-absorption features suggesting an association of diffuse \CII regions with
cool \HI. The observed widths of the lines from the two species are, however,
different. We discuss possible reasons for the difference in the line widths.
