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The Potential of Differential Astrometric Interferometry from the High Antarctic Plateau

Published online by Cambridge University Press:  05 March 2013

James P. Lloyd ,
Ben R. Oppenheimer  and
James R. Graham
James P. Lloyd*
Affiliation:
Department of Astronomy, University of California, Berkeley, USA
Ben R. Oppenheimer
Affiliation:
Department of Astrophysics, American Museum of Natural History, New York, USA
James R. Graham
Affiliation:
Department of Astronomy, University of California, Berkeley, USA
*
jpl@astron.berkeley.edu
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Abstract

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The low infrared background and high atmospheric transparency are the principal advantages of Antarctic Plateau sites for astronomy. However, the poor seeing (between 1 and 3 as) negates much of the sensitivity improvements that the Antarctic atmosphere offers, compared to mid-latitude sites such as Mauna Kea or Cerro Paranal. The seeing at mid-latitude sites, though smaller in amplitude, is dominated by turbulence at altitudes of 10–20 km. Over the Antarctic Plateau, virtually no high altitude turbulence is present in the winter. The mean square error for an astrometric measurement with a dual-beam, differential astrometric interferometer in the very narrow angle regime is proportional to the integral of h2C2N(h). Therefore, sites at which the turbulence occurs only at low altitudes offer large gains in astrometric precision. We show that a modest interferometer at the South Pole can achieve 10 μ as differential astrometry 300 times faster than a comparable interferometer at a good mid-latitude site, in median conditions. Science programs that would benefit from such an instrument include planet detection and orbit determination, and astrometric observation of stars microlensed by dark matter candidates.

Keywords

instrumentation: interferometerstechniques: interferometricastrometryextrasolar planetsGalaxy: halo, stellar content
Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 19 , Issue 3 , 2002 , pp. 318 - 322
Copyright
Copyright © Astronomical Society of Australia 2002

References

Alcock, C., et al. 2000, ApJ, 542, 281 Google Scholar
Boden, A. F., Shao, M., & van Buren, D. 1998, ApJ, 502, 538 Google Scholar
Colavita, M. M. 1994, A&A, 283, 1027 Google Scholar
Colavita, M. M., et al. 1999, ApJ, 510, 505 Google Scholar
Gillingham, P. 1993, in Optics in Astronomy: 32nd Herstmonceux Conference, ed. J. V. Wall (Cambridge: Cambridge University Press), 244 Google Scholar
Greenwood, D. P. 1977, J. Opt. Soc. Am., 67, 390 CrossRefGoogle Scholar
Hardy, J. W., ed. 1998, Adaptive Optics for Astronomical Telescopes (New York: Oxford University Press)Google Scholar
Marks, R. D., Vernin, J., Azouit, M., Briggs, J. W., Burton, M. G., Ashley, M. C. B., & Manigault, J. F. 1996, A&AS, 118, 385 Google Scholar
Marks, R. D., Vernin, J., Azouit, M., Manigault, J. F., & Clevelin, C. 1999, A&AS, 134, 161 Google Scholar
Oppenheimer, B. R., Hambly, N. C., Digby, A. P., Hodgkin, S. T., & Saumon, D. 2001, Science, 292, 698 CrossRefGoogle Scholar
Roddier, F., Cowie, L., Graves, J. E., Songaila, A., & McKenna, D. 1990, Proc. SPIE, 1236, 485 Google Scholar
Roggeman, M. C., & Welsh, B. 1996, Imaging Through Turbulence (CRC Press)Google Scholar
Shao, M., & Colavita, M. M. 1992, A&A, 262, 353 Google Scholar
Udalski, A., Kubiak, M., & Szymanski, M. 1997, Acta Astronom., 47, 319 Google Scholar