  In this work we adopted a CLEAN-based method to determine the scatter time,
$\tau$, from archived pulsar profiles under both the thin screen and uniform
medium scattering models and to calculate the scatter time frequency scale
index $\alpha$ where $\tau\propto\nu^{\alpha}$. The value of $\alpha$ is
$-4.4$, if a Kolmogorov spectrum of the interstellar medium turbulence is
assumed. We deconvolved 1342 profiles from 347 pulsars over a broad range of
frequencies and dispersion measures. In our survey, in the majority of cases
the scattering effect was not significant compared to pulse profile widths. For
a subset of 21 pulsars scattering at the lowest frequencies was large enough to
be measured. Because reliable scatter time measurements were determined only
for the lowest frequency, we were limited to using upper limits on scatter
times at higher frequencies for the purpose of our scatter time frequency slope
estimation. We scaled the deconvolved scatter time to 1~GHz assuming
$\alpha=-4.4$ and considered our results in the context of other observations
which yielded a broad relation between scatter time and dispersion measure.
