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 .