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Measuring the Size of the Vela Pulsar’s Radio Emission Region

Published online by Cambridge University Press:  12 April 2016

C.R. Gwinn
Affiliation:
Physics Department, UC Santa Barbara, Santa Barbara, California, USA
J.E. Reynolds
Affiliation:
Australia Telescope National Facility, Epping, New South Wales, Australia
D.L. Jauncey
Affiliation:
Australia Telescope National Facility, Epping, New South Wales, Australia
H. Hirabayashi
Affiliation:
Institute of Space and Astronautical Science, Sagamihara, Kanagawa, Japan
H. Kobayashi
Affiliation:
Institute of Space and Astronautical Science, Sagamihara, Kanagawa, Japan
Y. Murata
Affiliation:
Institute of Space and Astronautical Science, Sagamihara, Kanagawa, Japan
P.G. Edwards
Affiliation:
Institute of Space and Astronautical Science, Sagamihara, Kanagawa, Japan
B. Carlson
Affiliation:
Dominion Radio Astronomy Observatory, Hertzberg Institute of Astrophysics, National Research Council of Canada, Penticton, British Columbia, Canada
S. Dougherty
Affiliation:
Dominion Radio Astronomy Observatory, Hertzberg Institute of Astrophysics, National Research Council of Canada, Penticton, British Columbia, Canada
D. Del Rizzo
Affiliation:
Dominion Radio Astronomy Observatory, Hertzberg Institute of Astrophysics, National Research Council of Canada, Penticton, British Columbia, Canada
M.C. Britton
Affiliation:
Swinburne Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia
RM. McCulloch
Affiliation:
Physics Department, University of Tasmania, Hobart, Tasmania, Australia
J.E.J. Lovell
Affiliation:
Physics Department, University of Tasmania, Hobart, Tasmania, Australia

Abstract

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We describe the expected distribution of intensity for a scintillating source of finite size observed through a scattering medium, including systematic and instrumental effects. We describe measurements of the size of the Vela pulsar, using this technique.

Type
Part 3. Studies of Radio Emission
Copyright
Copyright © Astronomical Society of the Pacific 2000

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