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We have searched for planetary companions around 800 pulsars monitored at theJodrell Bank Observatory, with both circular and eccentric orbits of periodsbetween $20$ days and $17$ years and inclination-dependent planetary massesfrom $10^{-4}$ to $100\,\mathrm{M}_{\oplus}$. Using a Bayesian framework, wesimultaneously model pulsar timing parameters and a stationary noise processwith a power-law power spectral density. We put limits on the projected massesof any planetary companions, which reach as low as 1/100th of the mass of theMoon ($\sim 10^{-4}\,\mathrm{M}_{\oplus}$). We find that two-thirds of ourpulsars are highly unlikely to host any companions above$2-8\,\mathrm{M}_{\oplus}$. Our results imply that fewer than $0.5\%$ ofpulsars could host terrestrial planets as large as those known to orbit PSRB1257$+$12 ($\sim4\,\mathrm{M}_{\oplus}$); however, the smaller planet in thissystem ($\sim0.02\,\mathrm{M}_{\oplus}$) would be undetectable in $95\%$ of oursample, hidden by both instrumental and intrinsic noise processes, although itis not clear if such tiny planets could exist in isolation. We detectsignificant periodicities in 15 pulsars, however we find that intrinsicquasi-periodic magnetospheric effects can mimic the influence of a planet, andfor the majority of these cases we believe this to be the origin of thedetected periodicity. Notably, we find that the highly periodic oscillations inPSR B0144$+$59 are correlated with changes in the pulse profile and thereforecan be attributed to magnetospheric effects. We believe the most plausiblecandidate for planetary companions in our sample is PSR J2007$+$3120.

A search for planetary companions around 800 pulsars from the Jodrell Bank pulsar timing programme