A sub-Saturn mass planet, MOA-2009-BLG-319Lb
- Miyake N.
- Sumi T.
- Dong S.
- Street R.
- Mancini L.
- Gould A.
- Bennett D. P.
- Tsapras Y.
- Yee J. C.
- Albrow M. D.
- Bond I. A.
- Fouque P.
- Browne P.
- Han C.
- Snodgrass C.
- Finet F.
- Furusawa K.
- Harpsoe K.
- Allen W.
- Hundertmark M.
- Freeman M.
- Suzuk D.
- Abe F.
- Botzler C. S.
- Douchin D.
- Fukui A.
- Hayashi F.
- Hearnshaw J. B.
- Hosaka S.
- Itow Y.
- Kamiya K.
- Kilmartin P. M.
- Korpela A.
- Lin W.
- Ling C. H.
- Makita S.
- Masuda K.
- Matsubara Y.
- Muraki Y.
- Nagayama T.
- Nishimoto K.
- Ohnishi K.
- Perrott Y. C.
- Rattenbury N.
- Saito To.
- Skuljan L.
- Sullivan D. J.
- Sweatman W. L.
- Tristram P. J.
- Wada K.
- Yock P. C. M.
- Bolt G.
- Bos M.
- Christie G. W.
- Depoy D. L.
- Drummond J.
- Gal-Yam A.
- Gaudi B. S.
- Gorbikov E.
- Higgins D.
- Hwang K. -H.
- Janczak J.
- Kaspi S.
- Lee C. -U.
- Koo J. -R.
- Kozllowski S.
- Lee Y.
- Mallia F.
- Maury A.
- Maoz D.
- McCormick J.
- Monard L. A. G.
- Moorhouse D.
- Munoz J. A.
- Natusch T.
- Ofek E. O.
- Pogge R. W.
- Polishook D.
- Santallo R.
- Shporer A.
- Spector O.
- Thornley G.
- Allan A.
- Bramich D. M.
- Horne K.
- Kains N.
- Steele I.
- Bozza V.
- Burgdorf M. J.
- Calchi Novati S.
- Dominik M.
- Dreizler S.
- Glitrup M.
- Hessman F. V.
- Hinse T. C.
- Jorgensen U. G.
- Liebig C.
- Maier G.
- Mathiasen M.
- Rahvar S.
- Ricci D.
- Scarpetta G.
- Skottfelt J.
- Southworth J.
- Surdej J.
- Wambsganss J.
- Zimmer F.
- Batista V.
- Beaulieu J. P.
- Brillant S.
- Cassan A.
- Cole A.
- Corrales E.
- Coutures Ch.
- Dieters S.
- Greenhill J.
- Kubas D.
- Menzies J.
DOIAbstract
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 Bay...
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