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Pulsar timing arrays (PTAs) are placing increasingly stringent constraints onthe strain amplitude of continuous gravitational waves emitted by supermassiveblack hole binaries on subparsec scales. In this paper, we incorporateindependent information about the dynamical masses $M_{bh}$ of supermassiveblack holes in specific galaxies at known distances and use this additionalinformation to further constrain whether or not those galaxies could host adetectable supermassive black hole binary. We estimate the strain amplitudesfrom individual binaries as a function of binary mass ratio for two samples ofnearby galaxies: (1) those with direct dynamical measurements of $M_{bh}$ inthe literature, and (2) the 116 most massive early-type galaxies (and thuslikely hosts of the most massive black holes) within 108 Mpc from the MASSIVESurvey. Our exploratory analysis shows that the current PTA upper limits oncontinuous waves (as a function of angular position in the sky) can alreadyconstrain the mass ratios of hypothetical black hole binaries in many galaxiesin our samples. The constraints are stronger for galaxies with larger $M_{bh}$and at smaller distances. For the black holes with $M_{bh} \gtrsim 5\times 10^9M_\odot$ at the centers of NGC 1600, NGC 4889, NGC 4486 (M87) and NGC 4649(M60), any binary companion in orbit within the PTA frequency bands would haveto have a mass ratio of a few percent or less.

Constraints on Individual Supermassive Black Hole Binaries from Pulsar Timing Array Limits on Continuous Gravitational Waves