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Title:
Determination of stellar shape in microlensing event MOA 2002-BLG-33
Authors:
Rattenbury, N. J.; Abe, F.; Bennett, D. P.; Bond, I. A.; Calitz, J. J.; Claret, A.; Cook, K. H.; Furuta, Y.; Gal-Yam, A.; Glicenstein, J.-F.; Hearnshaw, J. B.; Hauschildt, P. H.; Kilmartin, P. M.; Kurata, Y.; Masuda, K.; Maoz, D.; Matsubara, Y.; Meintjes, P. J.; Moniez, M.; Muraki, Y.; Noda, S.; Ofek, E. O.; Okajima, K.; Philpott, L.; Rhie, S. H.; Sako, T.; Sullivan, D. J.; Sumi, T.; Terndrup, D. M.; Tristram, P. J.; Wood, J.; Yanagisawa, T.; Yock, P. C. M.
Affiliation:
AA(Jodrell Bank Observatory, Macclesfield, Cheshire SK11 9DL, UK ), AB(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AC(Department of Physics, Notre Dame University, Notre Dame, IN 46556, USA), AD(Institute of Information and Mathematical Sciences, Massey University, Auckland, New Zealand), AE(Department of Physics, University of the Free State, Bloemfontein, South Africa), AF(Instituto de Astrofísica de Andalucía, CSIC, Apartado 3004, 18080 Granada, Spain), AG(Institute for Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, CA 94563, USA), AH(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AI(Hubble Fellow, Caltech Astronomy, MS 105-24, California Institute of Technology, 1200 E. California Bl., Pasadena, California), AJ(CEA, DSM, DAPNIA, Centre d'Études de Saclay, 91191 Gif-sur-Yvette Cedex, France), AK(Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand), AL(Universität Hamburg, Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany), AM(Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand), AN(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AO(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AP(School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel), AQ(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AR(Department of Physics, University of the Free State, Bloemfontein, South Africa), AS(Laboratoire de l'Accélérateur Lineaire, IN2P3 CNRS, Université de Paris-Sud, 91405 Orsay Cedex, France), AT(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AU(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AV(School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel), AW(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), AX(Faculty of Science, University of Auckland, Private Bag 92019, Auckland, New Zealand), AY(Department of Physics, Notre Dame University, Notre Dame, IN 46556, USA), AZ(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), BA(School of Chemical and Physical Sciences, Victoria University, PO Box 600, Wellington, New Zealand), BB(Department of Astrophysical Sciences, Princeton University, Princeton NJ 08544, USA), BC(Department of Astronomy, Ohio State University, Columbus OH 43210, USA), BD(Department of Physics and Astronomy, University of Canterbury, Private Bag 4800, Christchurch, New Zealand), BE(Faculty of Science, University of Auckland, Private Bag 92019, Auckland, New Zealand), BF(Solar Terrestrial Environment Laboratory, Nagoya University, Nagoya 464-8601, Japan), BG(Faculty of Science, University of Auckland, Private Bag 92019, Auckland, New Zealand)
Publication:
Astronomy and Astrophysics, Volume 439, Issue 2, August IV 2005, pp.645-650 (A&A Homepage)
Publication Date:
08/2005
Origin:
EDP Sciences
Keywords:
gravitational lensing, stars: atmospheres, stars: rotation
DOI:
10.1051/0004-6361:20052858
Bibliographic Code:
2005A&A...439..645R

Abstract

We report a measurement of the shape of the source star in microlensing event MOA 2002-BLG-33. The lens for this event was a close binary whose centre-of-mass passed almost directly in front of the source star. At this time, the source star was closely bounded on all sides by a caustic of the lens. This allowed the oblateness of the source star to be constrained. We found that a/b = 1.02+0.04-0.02 where a and b are its semi-major and semi-minor axes respectively. The angular resolution of this measurement is approximately 0.04 μ{arcsec}. We also report HST images of the event that confirm a previous identification of the source star as an F8-G2 turn-off main-sequence star.
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