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The scattering timescale is roughly related to the observing frequency, $\nu$, and distance between pulsar and observer, $D$, by  \begin{equation}  \tau_s \propto \frac{D^2}{\nu^\alpha}  \end{equation}  where $\alpha$ depends on the structure of turbulence in the ISM and is approximated as $\alpha \sim 4$.  The scattering timescale can also be expressed in terms of dispersion measure (DM). Here we will use the empirical model of \citet{Bhat_2004}, that relates $\tau_s$ to DM via  \begin{equation}  \log_{10} \tau_s(\nu,{\rm DM}) = -9.46 + 0.154 \log_{10} {\rm DM}+ 1.07 (\log_{10} {\rm DM})^2 - 3.86 \log_{10}{\nu},  \end{equation}  where $\tau_s$ is the scattering time in seconds and $\nu$ is the observing frequency in GHz. The scatter of measured values about this relationship has a standard deviation of several orders of magnitude. In the remainder of this document we take a conservative approach and assume that the scattering timescale is 4 orders of magnitude smaller than suggested by the above relation, i.e. the best-case scattering ($\tau_{s_{\rm best}}$) is given by  \begin{equation}  \label{eqn:best_case_scattering}  \log_{10} \tau_{s_{\rm best}}(\nu,{\rm DM}) = \log_{10} \tau_s(\nu,{\rm DM}) - 4.  \end{equation}  The point at which the scattering timescale exceeds the timescale implied by new versions of SKA1-SYS\_REQ-2961 and SKA1-SYS\_REQ-2962 (see above) ultimately determines the maximum DM for which the SKA1 pulsar timing instrumentation must support phase-coherent dispersion removal. Beyond this DM, the computational cost of coherent dedispersion can be decreased by trading time resolution for frequency resolution.