  Yamamoto et al. (1987) reported the first detection of $c$-C$_3$H radical in
{TMC-1} through its transition $2_{1 2} \to 1_{1 1}$ at 91.5 GHz. Mangum and
Wootten (1990) detected $c$-C$_3$H through the transition $1_{1 0} \to 1_{1 1}$
at 14.8 GHz in 12 additional galactic objects. The column density of $c$-C$_3$H
in the objects was estimated to be about one order of magnitude lower than that
of the C$_3$H$_2$ which is ubiquitous in the galactic objects. The most
probable production mechanism of both the C$_3$H and C$_3$H$_2$ in dark clouds
is a common dissociation reaction of C$_3$H$_3^+$ ion (Adams & Smith, 1987).
Although the $c$-C$_3$H is 0.8 eV less stable than its isomer $l$-C$_3$H,
finding of comparable column densities of both the isomers in {TMC-1} supports
the idea of comparable formation of both the $c$-C$_3$H and $l$-C$_3$H in the
cosmic objects. Existence of a metaisomer in interstellar condition is a well
known phenomenon in astronomy.
  We propose that $c$-C$_3$H may be identified through the transition $3_{3 1}
\to 3_{3 0}$ at 3.4 GHz in absorption against the cosmic 2.7 K background in
dense cosmic objects when no strong source is present in the background. When
there is some strong source in the background of the object, peak of the
absorption line decreases with the increase of the strength of the background
source. However, at low densities, the intensity is found to increase. Hence,
in low density regions, a background source can help in detection of the line.
This absorption line may play an important role for identification of
$c$-C$_3$H in a large number of cosmic objects. Similar absorption features are
found for $c$-C$_3$D radical also.
