  Broadband radio waves emitted from pulsars are distorted and delayed as they
propagate toward the Earth due to interactions with the free electrons that
compose the interstellar medium, with lower radio frequencies being more
impacted than higher frequencies. Multipath propagation in the interstellar
medium results in both later times of arrival for the lower frequencies and
causes the observed pulse to arrive with a broadened tail described via the
pulse broadening function. We employ the CLEAN deconvolution technique to
recover both the intrinsic pulse shape and pulse broadening function. This work
expands upon previous descriptions of CLEAN deconvolution used in pulse
broadening analyses by parameterizing the efficacy on simulated data and
developing a suite of tests to establish which of a set of figures of merit
lead to an automatic and consistent determination of the scattering timescale
and its uncertainty. We compare our algorithm to simulations performed on
cyclic spectroscopy estimates of the scattering timescale. We test our improved
algorithm on the highly scattered millisecond pulsar J1903+0327, showing the
scattering timescale to change over years, consistent with estimates of the
refractive timescale of the pulsar.
