  The 23 GHz emission lines from the NH3 rotation inversion transitions are
widely used to investigate the kinematics and physical conditions in dense
molecular clouds. The line profile is composed of hyperfine components which
can be used to calculate the opacity of the gas (Ho & Townes 1983). If the
intrinsic linewidth of the gas exceeds one half of the separation of these
quadrupole hyperfine components (~5-10 km/s) these lines blend together and the
observed linewidths greatly overestimate the intrinsic linewidths. If
uncorrected, these artificially broad linewidths will lead to artificially high
opacities. We have observed this effect in our NH3 data from the central 10 pc
of the Galaxy where uncorrected NH3 (1,1) linewidths of ~30 km/s exaggerate the
intrinsic linewidths by more than a factor of two (Genzel & Townes 1987).
Models of the effect of blending on the line profile enable us to solve for the
intrinsic linewidth and opacity of NH3 using the observed linewidth and
intensity of two NH3 rotation inversion transitions. We present the result of
the application of this method to our Galactic Center data. We successfully
recover the intrinsic linewidth and opacity of the gas. Clouds close to the
nucleus in projected distance as well as those that are being impacted by Sgr A
East show the highest intrinsic linewidths. The cores of the ``southern
streamer'' (Ho et al. 1991; Coil & Ho 1999, 2000) and the ``50 km/s'' giant
molecular cloud have the highest opacities.
