  We model Carbon Recombination Line (CRL) emission from the Photo Dissociation
Region (PDR) surrounding the Ultra-Compact (UC) HII region W48A. Our modelling
shows that the inner regions ($A_V \sim 1$) of the CII layer in the PDR
contribute significantly to the CRL emission. The dependence of line ratios of
CRL emission with the density of the PDR and the far ultra-violet (FUV)
radiation incident on the region is explored over a large range of these
parameters that are typical for the environments of UCHII regions. We find that
by observing a suitable set of CRLs it is possible to constrain the density of
the PDR. If the neutral density in the PDR is high ($\gtrsim 10^7$ \cmthree)
CRL emission is bright at high frequencies ($\gtrsim 20$ GHz), and absorption
lines from such regions can be detected at low frequencies ($\lesssim 10$ GHz).
Modelling CRL observations towards W48A shows that the UCHII region is embedded
in a molecular cloud of density of about $4 \times$ 10$^7$ \cmthree.
