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Title:
High-Precision Limb-Darkening Measurement of a K3 Giant Using Microlensing
Authors:
Fields, Dale L.; Albrow, M. D.; An, J.; Beaulieu, J.-P.; Caldwell, J. A. R.; DePoy, D. L.; Dominik, M.; Gaudi, B. S.; Gould, A.; Greenhill, J.; Hill, K.; Jørgensen, U. G.; Kane, S.; Martin, R.; Menzies, J.; Pogge, R. W.; Pollard, K. R.; Sackett, P. D.; Sahu, K. C.; Vermaak, P.; Watson, R.; Williams, A.; Glicenstein, J.-F.; Hauschildt, P. H.
Affiliation:
AA(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; .), AB(Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand.; Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AC(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; .; Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 OHA, UK.), AD(Institut d'Astrophysique de Paris, INSU-CNRS, 98 bis Boulevard Arago, F 75014 Paris, France.), AE(South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa.), AF(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; .), AG(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK.), AH(School of Natural Sciences, Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540.; Hubble Fellow.), AI(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; .), AJ(Physics Department, University of Tasmania, G.P.O. 252C, Hobart, Tasmania 7001, Australia.), AK(Physics Department, University of Tasmania, G.P.O. 252C, Hobart, Tasmania 7001, Australia.), AL(Astronomical Observatory, Niels Bohr Institute, Juliane Maries Vej 30, 2100 Copenhagen, Denmark.), AM(School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK.), AN(Perth Observatory, Walnut Road, Bickley, Western Australia 6076, Australia.), AO(South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa.), AP(Department of Astronomy, Ohio State University, 140 West 18th Avenue, Columbus, OH 43210; .), AQ(Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand.), AR(Research School of Astronomy and Astrophysics, Australian National University, Mount Stromlo, Weston ACT 2611, Australia.), AS(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218.), AT(South African Astronomical Observatory, P.O. Box 9, Observatory 7935, South Africa.), AU(Physics Department, University of Tasmania, G.P.O. 252C, Hobart, Tasmania 7001, Australia.), AV(Perth Observatory, Walnut Road, Bickley, Western Australia 6076, Australia.), AW(DAPNIA-SPP, CE-Saclay, F-91191 Gif-sur-Yvette, France.), AX(Universität Hamburg, Hamburger Sternwarte, Gojenbergsweg 112, D-21029 Hamburg, Germany.)
Publication:
The Astrophysical Journal, Volume 596, Issue 2, pp. 1305-1319. (ApJ Homepage)
Publication Date:
10/2003
Origin:
UCP
ApJ Keywords:
Cosmology: Gravitational Lensing, Stars: Atmospheres
DOI:
10.1086/378196
Bibliographic Code:
2003ApJ...596.1305F

Abstract

We obtain high-precision limb-darkening measurements in five bands (V, VE, IE, I, and H) for the K3 III (Teff=4200 K, [Fe/H]=+0.3, logg=2.3) source of the Galactic bulge microlensing event EROS BLG-2000-5. These measurements are inconsistent with the predictions of atmospheric models at higher than 10 σ. While the disagreement is present in all bands, it is most apparent in I, IE, and VE, in part because the data are better and in part because the intrinsic disagreement is stronger. We find that when limb-darkening profiles are normalized to have unit total flux, the I-band models for a broad range of temperatures all cross each other at a common point. The solar profile also passes through this point. However, the profile as measured by microlensing does not. We hypothesize that the models have incorporated some aspect of solar physics that is not shared by giant atmospheres.
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