VLBI pulsar astrometry

Details VLBI pulsar astrometry VLBI pulsar astrometry

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..404c&link_type=abstract

Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at

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Interleaved VLBI phase-delay observations of two sources that lie near each other on the plane of the sky can determine their relative positions with sub-milliarcsecond uncertainties. A series of such observations, well spread throughout the seasons, of a pulsar and extragalactic reference sources can yield the position, proper motion, and parallax of the pulsar, the latter providing a model-independent distance. Such results can find applications in, among others, two broad areas: (i) the properties of the free-electron density distribution in the solar neighborhood: e.g., checks on models of ne, calibrations for scattering-based distance scales, and perhaps characterization of plasma turbulence in the ISM; and (ii) the kinematics and evolution of the pulsars themselves: e.g., whether useful links may be established between individual pulsars and putative progenitors (especially in light of recent Hipparcos astrometry), and estimation of bounds on the decay timescales of pulsars' magnetic fields via comparison of their spin-down and derived kinetic ages. We will present an overview of and illustrative results from our ongoing VLBI pulsar astrometry program.

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