MOA-2010-BLG-311:a planetary candidate below the threshold of reliable detection
- Yee, J. C.
- Hung, L. -W.
- Bond, I. A.
- Allen, W.
- Monard, L. A. G.
- Albrow, M. D.
- Fouque, P.
- Dominik, M.
- Tsapras, Y.
- Udalski, A.
- Gould, A.
- Zellem, R.
- Bos, M.
- Christie, G. W.
- DePoy, D. L.
- Dong, Subo
- Drummond, J.
- Gaudi, B. S.
- Gorbikov, E.
- Han, C.
- Kaspi, S.
- Klein, N.
- Lee, C. -U.
- Maoz, D.
- McCormick, J.
- Moorhouse, D.
- Natusch, T.
- Nola, M.
- Park, B. -G.
- Pogge, R. W.
- Polishook, D.
- Shporer, A.
- Shvartzvald, Y.
- Skowron, J.
- Thornley, G.
- Abe, F.
- Bennett, D. P.
- Botzler, C. S.
- Chote, P.
- Freeman, M.
- Fukui, A.
- Furusawa, K.
- Harris, P.
- Itow, Y.
- Ling, C. H.
- Masuda, K.
- Matsubara, Y.
- Miyake, N.
- Ohnishi, K.
- Rattenbury, N. J.
- Saito, To.
- Sullivan, D. J.
- Sumi, T.
- Suzuki, D.
- Sweatman, W. L.
- Tristram, P. J.
- Wada, K.
- Yock, P. C. M.
- Szymanski, M. K.
- Soszynski, I.
- Kubiak, M.
- Poleski, R.
- Ulaczyk, K.
- Pietrzynski, G.
- Wyrzykowski, L.
- Bachelet, E.
- Batista, V.
- Beatty, T. G.
- Beaulieu, J. -P.
- Bennett, C. S.
- Bowens-Rubin, R.
- Brillant, S.
- Caldwell, J. A. R.
- Cassan, A.
- Cole, A. A.
- Corrales, E.
- Coutures, C.
- Dieters, S.
- Prester, D. Dominis
- Donatowicz, J.
- Greenhill, J.
- Henderson, C. B.
- Kubas, D.
- Marquette, J. -B.
- Martin, R.
- Menzies, J. W.
- Shappee, B.
- Williams, A.
- Wouters, D.
- van Saders, J.
- Zub, M.
- Street, R. A.
- Horne, K.
- Bramich, D. M.
- Steele, I. A.
- Alsubai, K. A.
- Bozza, V.
- Browne, P.
- Burgdorf, M. J.
- Calchi Novati, S.
- Dodds, P.
- Finet, F.
- Gerner, T.
- Hardis, S.
- Harpsoe, K.
- Hessman, F. V.
- Hinse, T. C.
- Hundertmark, M.
- Jorgensen, U. G.
- Kains, N.
- Kerins, E.
- Liebig, C.
- Mancini, L.
- Mathiasen, M.
- Penny, M. T.
- Proft, S.
- Rahvar, S.
- Ricci, D.
- Sahu, K. C.
- Scarpetta, G.
- Schaefer, S.
- Schoenebeck, F.
- Snodgrass, C.
- Southworth, J.
- Surdej, J.
- Wambsganss, J.
DOIAbstract
We analyze MOA-2010-BLG-311, a high magnification (Amax > 600) microlensing event with complete data coverage over the peak, making it very sensitive to planetary signals. We fit this event with both a point lens and a two-body lens model and find that the two-body lens model is a better fit but with only Δχ2 ~ 80. The preferred mass ratio between the lens star and its companion is q = 10−3.7 ± 0.1, placing the candidate companion in the planetary regime. Despite the formal significance of the planet, we show that because of systematics in the data the evidence for a planetary companion to the lens is too tenuous to claim a secure detection. When combined with analyses of other high-magnification events, this event helps empirically defi...
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