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Exoplanet detection from Dome C, Antarctica: opportunities and challenges

Published online by Cambridge University Press:  02 May 2006

J. S. Lawrence ,
M. C. B. Ashley ,
M. G. Burton  and
J. W. V. Storey
J. S. Lawrence
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW, 2052, Australia email: jl@phys.unsw.edu.au
M. C. B. Ashley
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW, 2052, Australia email: jl@phys.unsw.edu.au
M. G. Burton
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW, 2052, Australia email: jl@phys.unsw.edu.au
J. W. V. Storey
Affiliation:
School of Physics, University of New South Wales, Sydney, NSW, 2052, Australia email: jl@phys.unsw.edu.au
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Abstract

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Many methods have been proposed for the detection of exoplanets. The minimum detectable planetary size and mass, and the maximum distance from us at which exoplanets are observable, are determined by both technological and environmental constraints. The unique atmospheric conditions found at Dome C offer significant advantages. Using what is now known about the turbulence profile of the atmosphere above Antarctic plateau sites, we explore the potential these sites offer for detecting exoplanets around nearby stars using various methods.

Keywords

planetary systemstelescopesinstrumentation: adaptive opticsatmospheric effectstechniques: high angular resolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Colloquium C200: Direct Imaging of Exoplanets: Science & Techniques , October 2005 , pp. 297 - 300
Copyright
© 2006 International Astronomical Union