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\section{Maximum Temporal Resolutions for SKA1\_Mid and SKA1\_Low}  Figure \ref{fig:pulse_spectra} displays fluctuation power spectra derived from the long-term average profiles of the Parkes Pulsar Timing Array (PPTA) pulsars observed at 20 and 50 cm \cite{Dai_2015}. In these plots, the fluctuation power of each pulsar drops exponentially as a function of spin harmonic, eventually hitting a white noise floor. PSR~J0437$-$4715 and PSR~J2241$-$5236 are the worst case examples in which fluctuation power approaches the Nyquist limit where spin harmonics will be aliased.  These plots indicate that 1024 phase bins is sufficient to resolve all of the structure in the mean pulse profiles of most the  currently known MSPs. PSR~J0437$-$4715 and PSR~J2241$-$5236 are the worst case examples in which fluctuation power approaches the Nyquist limit where spin harmonics will be aliased. MSPs used for high-precision timing.  Greater telescope sensitivity increases the signal-to-noise ratio, causing more fluctuation power to rise out of the white noise floor; however, these plots indicate that the number of spin harmonics required to resolve all significant power is proportional only to the logarithm of the S/N; i.e. to first order, the maximum harmonic, 
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