February
2011
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2011ApJ...728..120M
Authors
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Miyake, N.
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Sumi, T.
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Dong, Subo
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Street, R.
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Mancini, L.
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Gould, A.
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Bennett, D. P.
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Tsapras, Y.
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Yee, J. C.
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Albrow, M. D.
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Bond, I. A.
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Fouqué, P.
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Browne, P.
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Han, C.
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Snodgrass, C.
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Finet, F.
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Furusawa, K.
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Harpsøe, K.
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Allen, W.
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Hundertmark, M.
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Freeman, M.
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Suzuki, D.
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Abe, F.
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Botzler, C. S.
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Douchin, D.
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Fukui, A.
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Hayashi, F.
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Hearnshaw, J. B.
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Hosaka, S.
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Itow, Y.
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Kamiya, K.
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Kilmartin, P. M.
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Korpela, A.
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Lin, W.
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Ling, C. H.
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Makita, S.
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Masuda, K.
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Matsubara, Y.
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Muraki, Y.
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Nagayama, T.
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Nishimoto, K.
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Ohnishi, K.
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Perrott, Y. C.
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Rattenbury, N.
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Saito, To.
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Skuljan, L.
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Sullivan, D. J.
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Sweatman, W. L.
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Tristram, P. J.
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Wada, K.
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Yock, P. C. M.
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MOA Collaboration
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Bolt, G.
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Bos, M.
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Christie, G. W.
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DePoy, D. L.
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Drummond, J.
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Gal-Yam, A.
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Gaudi, B. S.
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Gorbikov, E.
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Higgins, D.
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Hwang, K. -H.
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Janczak, J.
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Kaspi, S.
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Lee, C. -U.
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Koo, J. -R.
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Kozłowski, S.
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Lee, Y.
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Mallia, F.
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Maury, A.
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Maoz, D.
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McCormick, J.
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Monard, L. A. G.
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Moorhouse, D.
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Muñoz, J. A.
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Natusch, T.
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Ofek, E. O.
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Pogge, R. W.
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Polishook, D.
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Santallo, R.
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Shporer, A.
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Spector, O.
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Thornley, G.
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μFUN Collaboration
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Allan, A.
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Bramich, D. M.
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Horne, K.
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Kains, N.
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Steele, I.
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RoboNet Collaboration
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Bozza, V.
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Burgdorf, M. J.
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Calchi Novati, S.
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Dominik, M.
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Dreizler, S.
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Glitrup, M.
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Hessman, F. V.
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Hinse, T. C.
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Jørgensen, U. G.
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Liebig, C.
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Maier, G.
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Mathiasen, M.
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Rahvar, S.
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Ricci, D.
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Scarpetta, G.
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Skottfelt, J.
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Southworth, J.
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Surdej, J.
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Wambsganss, J.
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Zimmer, F.
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MiNDSTEp Consortium
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Batista, V.
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Beaulieu, J. P.
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Brillant, S.
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Cassan, A.
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Cole, A.
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Corrales, E.
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Coutures, Ch.
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Dieters, S.
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Greenhill, J.
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Kubas, D.
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Menzies, J.
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PLANET Collaboration
Abstract
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We report the gravitational microlensing discovery of a sub-Saturn mass planet, MOA-2009-BLG-319Lb, orbiting a K- or M-dwarf star in the inner Galactic disk or Galactic bulge. The high-cadence observations of the MOA-II survey discovered this microlensing event and enabled its identification as a high-magnification event approximately 24 hr prior to peak magnification. As a result, the planetary signal at the peak of this light curve was observed by 20 different telescopes, which is the largest number of telescopes to contribute to a planetary discovery to date. The microlensing model for this event indicates a planet-star mass ratio of q = (3.95 ± 0.02) × 10-4 and a separation of d = 0.97537 ± 0.00007 in units of the Einstein radius. A Bayesian analysis based on the measured Einstein radius crossing time, t E, and angular Einstein radius, θE, along with a standard Galactic model indicates a host star mass of M L = 0.38+0.34 -0.18 M sun and a planet mass of M p = 50+44 -24 M ⊕, which is half the mass of Saturn. This analysis also yields a planet-star three-dimensional separation of a = 2.4+1.2 -0.6 AU and a distance to the planetary system of D L = 6.1+1.1 -1.2 kpc. This separation is ~2 times the distance of the snow line, a separation similar to most of the other planets discovered by microlensing.
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