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 $taupropto u^{alpha}$. 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.
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