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The use of pulsars as astrophysical clocks for gravitational wave experimentsdemands the highest possible timing precision. Pulse times of arrival (TOAs)are limited by stochastic processes that occur in the pulsar itself, along theline of sight through the interstellar medium, and in the measurement process.On timescales of seconds to hours, the TOA variance exceeds that fromtemplate-fitting errors due to additive noise. We assess contributions to thetotal variance from two additional effects: amplitude and phase jitterintrinsic to single pulses and changes in the interstellar impulse responsefrom scattering. The three effects have different dependencies on time,frequency, and pulse signal-to-noise ratio. We use data on 37 pulsars from theNorth American Nanohertz Observatory for Gravitational Waves to assess theindividual contributions to the overall intraday noise budget for each pulsar.We detect jitter in 22 pulsars and estimate the average value of RMS jitter inour pulsars to be $\sim 1\%$ of pulse phase. We examine how jitter evolves as afunction of frequency and find evidence for evolution. Finally, we compare ourmeasurements with previous noise parameter estimates and discuss methods toimprove gravitational wave detection pipelines.

The NANOGrav Nine-Year Data Set: Noise Budget for Pulsar Arrival Times on Intraday Timescales