Using Gravitational Wave Pulsar Observations to measure electron column density

For binaries whose sky position, orientation, and chirp mass ${\cal M}_{c}$ are known, the observed gravitational wave amplitude of the binary system is a direct measure of the distance to the binary. In a similar spirit, the distance to radio pulsars can be inferred from pulsar observations from the dispersion measure, the integrated column density of electrons along the line of sight to a pulsar that causes an observational broadening of a radio pulse. This talk considers a multi-messenger observation of galactic binary systems that contain a pulsar component detectable in the electromagnetic spectrum, and a detectable gravitational wave signal, and demonstrates how the two independent distance measures can be used to measure the electron column density along the line of sight to the pulsar.