2011MNRAS.414...50D

Pulsar timing arrays (PTAs) act to detect gravitational waves by observing the small, correlated effect the waves have on pulse arrival times at the Earth. This effect has conventionally been evaluated assuming the gravitational wave phase fronts are planar across the array, an assumption that is valid only for sources at distances R ≫ 2πL²/λ, where L is physical extent of the array and λ is the radiation wavelength. In the case of PTAs, the array size is of the order of the pulsar–Earth distance (kpc) and λ is of the order of parsec. Correspondingly, for point gravitational wave sources closer than ∼100 Mpc, the PTA response is sensitive to the source parallax across the pulsar–Earth baseline. Here, we evaluate the PTA response to gravitational wave point sources including the important wavefront curvature effects. Taking the wavefront curvature into account, the relative amplitude and phase of the timing residuals associated with a collection of pulsars allow us to measure the distance to, and the sky position of, the source. Early-type stars observed in the ESO UVES Paranal Observatory Project – III. Sub-parsec and au-scale structure in the interstellar medium