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D. A. Hemberger, D. R. Stinebring (Oberlin)
High precision timing of pulsars -- important for a range of studies including the search for gravitational waves from black hole binaries -- is seriously limited by interstellar scattering. Pulsars are strongest at lower radio frequencies, but scattering effects are most severe there. Coherent correction for pulsar dispersion is now done routinely in high precision timing programs. Correction for basic scattering effects is uncommon, however. We explore the need for and efficacy of a post-detection correction technique based on the centroid of the scattering tail. Unlike previous efforts at time domain techniques, we derive information about the scattering tail centroid from the secondary spectrum of the scintillation pattern. We report on the time variability and accuracy to be expected for this technique for a range of scattering measures.
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.