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Bachelet, E; Fouque, P; Han, C; Gould, A; Albrow, M D; Beaulieu, J-P; Bertin, E; Bond, I A; Christie, G W; Heyrovsky, D; Novati, S Calchi; Dreizler, S; Finet, F; Glitrup, M; Grundahl, F; Harpsoee, K; Hessman, F V; Hinse, T C; Hundertmark, M; Liebig, C; Horne, K; Maier, G; Mancini, L; Rahvar, S; Ricci, D; Scarpetta, G; Skottfelt, J; Southworth, J; Surdej, J; Zimmer, F; Joergensen, U G; Maoz, D; Mathiasen, M; Matsunaga, N; McCormick, J; Menzies, J; Nataf, D; Natusch, T; Oi, N; Renon, N; Tsapras, Y; Udalski, A; Yee, J C; Batista, V; Bennett, D P; Brillant, S; Caldwell, J A R; Cassan, A; Cole, A; Cook, K H; et. al
Astronomy and astrophysics (Berlin), 11/2012, Volume: 547Journal Article
MOA 2009-BLG-411 was detected on August 5, 2009 by the MOA-Collaboration. Thanks to observations by all the collaborations, this event was well monitored. The authors first decided to characterize the source star properties by using a more refined method than the classical one: they measure the interstellar absorption along the line of sight in five different passbands. Secondly, they model the lightcurve by using the standard technique: make grids to look for local minima and refine the results by using a downhill method. Finally, they use a Galactic model to estimate the physical properties of the lens components. They find that the source star is a giant G star with radius 9 R. The grid search gives two local minima, which correspond to the theoretical degeneracy ... . They find that the lens is composed of a brown dwarf secondary of mass M sub( s) =0.05 M orbiting a primary M-star of mass M super( p) = 0.18 M. (ProQuest: ... denotes formulae/symbols omitted.)
