MOA 2010-BLG-477Lb: Constraining the mass of a microlensing planet from microlensing parallax, orbital motion, and detection of blended light
- Bachelet E.
- Shin I. -G.
- Han C.
- Fouque P.
- Gould A.
- Menzies J. W.
- Beaulieu J. -P.
- Bennett D. P.
- Bond I. A.
- Dong S.
- Heyrovsk D.
- Marquette J. -B.
- Marshall J.
- Skowron J.
- Street R. A.
- Sumi T.
- Udalski A.
- Abe L.
- Agabi K.
- Albrow M. D.
- Allen W.
- Bertin E.
- Bos M.
- Bramich D. M.
- Chavez J.
- Christie G. W.
- Cole A. A.
- Crouzet N.
- Dieters S.
- Dominik M.
- Drummond J.
- Greenhill J.
- Guillot T.
- Henderson C. B.
- Hessman F. V.
- Horne K.
- Hundertmark M.
- Johnson J. A.
- Jorgensen U. G.
- Kandori R.
- Liebig C.
- Mekarnia D.
- McCormick J.
- Moorhouse D.
- Nagayama T.
- Nataf D.
- Natusch T.
- Nishiyama S.
- Rivet J. -P.
- Sahu K. C.
- Shvartzvald Y.
- Thornley G.
- Tomczak A. R.
- Tsapras Y.
- Yee J. C.
- Batista V.
- Bennett C. S.
- Brillant S.
- Caldwell J. A. R.
- Cassan A.
- Corrales E.
- Coutures C.
- Dominis Prester D.
- Donatowicz J.
- Kubas D.
- Martin R.
- Williams A.
- Zub M.
- Andrade De Almeida L.
- Depoy D. L.
- Gaudi B. S.
- Hung L. -W.
- Jablonski F.
- Kaspi S.
- Klein N.
- Lee C. -U.
- Lee Y.
- Koo J. -R.
- Maoz D.
- Munoz J. A.
- Pogge R. W.
- Polishook D.
- Shporer A.
- Abe F.
- Botzler C. S.
- Chote P.
- Freeman M.
- Fukui A.
- Furusawa K.
- Harris P.
- Itow Y.
- Kobara S.
- Ling C. H.
- Masuda K.
- Matsubara Y.
- Miyake N.
- Ohmori K.
- Ohnishi K.
- Rattenbury N. J.
- Saito T.
- Sullivan D. J.
- 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.
- Kains N.
- Snodgrass C.
- Steele I. A.
- Alsubai K. A.
- Bozza V.
- Browne P.
- Burgdorf M. J.
- Calchi Novati S.
- Dodds P.
- Dreizler S.
- Finet F.
- Gerner T.
- Hardis S.
- Harpsoe K.
- Hinse T. C.
- Kerins E.
- Mancini L.
- Mathiasen M.
- Penny M. T.
- Proft S.
- Rahvar S.
- Ricci D.
- Scarpetta G.
- Schafer S.
- Schonebeck F.
- Southworth J.
- Surdej J.
- Wambsganss J.
DOIAbstract
Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of planet formation. In this paper, we report the discovery of a giant planet detected from the analysis of the light curve of a high-magnification microlensing event MOA 2010-BLG-477. The measured planet-star mass ratio is q = (2.181 ± 0.004) × 10-3 and the projected separation is s = 1.1228 ± 0.0006 in units of the Einstein radius. The angular Einstein radius is unusually large θE = 1.38 ± 0.11 mas. Combining this measurement with constraints on the "microlens parallax" and the lens flux, we can onl...
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