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We present a new model for the distribution of free electrons in the Galaxy,the Magellanic Clouds and the intergalactic medium (IGM) that can be used toestimate distances to real or simulated pulsars and fast radio bursts (FRBs)based on their dispersion measure (DM). The Galactic model has an extendedthick disk representing the so-called warm interstellar medium, a thin diskrepresenting the Galactic molecular ring, spiral arms based on a recent fit toGalactic HII regions, a Galactic Center disk and seven local features includingthe Gum Nebula, Galactic Loop I and the Local Bubble. An offset of the Sun fromthe Galactic plane and a warp of the outer Galactic disk are included in themodel. Parameters of the Galactic model are determined by fitting to 189pulsars with independently determined distances and DMs. Simple models are usedfor the Magellanic Clouds and the IGM. Galactic model distances are within theuncertainty range for 86 of the 189 independently determined distances andwithin 20\% of the nearest limit for a further 38 pulsars. We estimate that95\% of predicted Galactic pulsar distances will have a relative error of lessthan a factor of 0.9. The predictions of YMW16 are compared to those of theTC93 and NE2001 models showing that YMW16 performs significantly better on allmeasures. Timescales for pulse broadening due to interstellar scattering areestimated for (real or simulated) Galactic and Magellanic Cloud pulsars andFRBs.

A New Electron Density Model for Estimation of Pulsar and FRB Distances