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Low-frequency gravitational-wave experiments require the highest timingprecision from an array of the most stable millisecond pulsars. Several knownsources of noise on short timescales in single radio-pulsar observations arewell described by a simple model of three components: template-fitting from afinite signal-to-noise ratio, pulse phase/amplitude jitter from single-pulsestochasticity, and scintillation errors from short-timescale interstellarscattering variations. Currently template-fitting errors dominate, but as radiotelescopes push towards higher signal-to-noise ratios, jitter becomes the nextdominant term for most millisecond pulsars. Understanding the statistics ofjitter becomes crucial for properly characterizing arrival-time uncertainties.We characterize the radio-frequency dependence of jitter using data on 48pulsars in the North American Nanohertz Observatory for Gravitational Waves(NANOGrav) timing program. We detect significant jitter in 43 of the pulsarsand test several functional forms for its frequency dependence; we findsignificant frequency dependence for 30 pulsars. We find moderate correlationsof rms jitter with pulse width (R = 0.62) and number of profile components (R =0.40); the single-pulse rms jitter is typically ~1% of pulse phase. The averagefrequency dependence for all pulsars using a power-law model has index -0.42.We investigate the jitter variations for the interpulse of PSR~B1937+21 andfind no significant deviations from the main pulse rms jitter. We also test thetime-variation of jitter in two pulsars and find that systematics likely biasthe results for high-precision pulsars. Pulsar timing array analyses mustproperly model jitter as a significant component of the noise within thedetector.

The NANOGrav 12.5-Year Data Set: The Frequency Dependence of Pulse Jitter in Precision Millisecond Pulsars