  We present the first observations of emission lines of CN(2-1),
HCO$^{+}$(3-2) and C$_{2}$H(3-2) in the Perseus cluster. We observed at two
positions: directly at the central galaxy, NGC 1275 and also at a position
about 20$''$ to the east where associated filamentary structure has been shown
to have strong CO emission. Clear detections in CN and HCO$^{+}$ transitions
and a weak detection of the C$_{2}$H transition were made towards NGC 1275,
while weak detections of CN and HCO$^{+}$ were made towards the eastern
filamentary structure. Crude estimates of the column densities and fractional
abundances (mostly upper limits) as functions of an unknown rotational
temperature were made to both sources. These observational data were compared
with the outputs of thermal/chemical models previously published by
\citet{Baye10c} in an attempt to constrain the heating mechanisms in cluster
gas. We find that models in which heating is dominated by cosmic rays can
account for the molecular observations. This conclusion is consistent with that
of \citet{Ferl09} in their study of gas traced by optical and infrared
radiation. The cosmic ray heating rate in the regions probed by molecular
emissions is required to be at least two orders of magnitude larger than that
in the Milky Way.
