J/A+A/529/A102ivo://CDS.VizieR/J/A+A/529/A102doi:10.26093/cds/vizier.35290102CDSBatista V.Gould A.Dieters S.Dong SuboBond I.Beaulieu J.P.,Maoz D.Monard B.Christie G.W.McCormick J.Albrow M.D.Horne K.,Tsapras Y.Burgdorf M.J.Calchi Novati S.Skottfelt J.Caldwell J.,Kozlowski S.Kubas D.Gaudi B.S.Han C.Bennett1 D.P.An J.,Abe F.Botzler C.S.Douchin D.Freeman M.Fukui A.Furusawa K.,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.Miyake N.,Muraki Y.Nagaya M.Nishimoto K.Ohnishi K.Okumura T.Perrott Y.C.,Rattenbury N.Saito To.Sullivan D.J.Sumi T.Sweatman W.L.,Tristram P.J.von Seggern E.Yock P.C.M. (The MOA Collaboration),Brillant S.Calitz J.J.Cassan A.Cole A.Cook K.Coutures C.,Dominis Prester D.Donatowicz J.Greenhill J.Hoffman M.Jablonski F.,Kane S.R.Kains N.Marquette J.-B.Martin R.Martioli E.Meintjes P.,Menzies J.Pedretti E.Pollard K.Sahu K.C.Vinter C.Wambsganss J.,Watson R.Williams A.Zub M. (The PLANET Collaboration),Allen W.Bolt G.Bos M.DePoy D.L.Drummond J.Eastman J.D.,Gal-Yam A.Gorbikov E.Higgins D.Janczak J.Kaspi S.Lee C.-U.,Mallia F.Maury A.Monard L.A.G.Moorhouse D.Morgan N.Natusch T.,Ofek E.O.Park B.-G.Pogge R.W.Polishook D.Santallo R.Shporer A.,Spector O.Thornley G.Yee J.C. (The {mu} Collaboration),Bozza V.Browne P.Dominik M.Dreizler S.Finet F.Glitrup M.,Grundah F.Harpsoe K.Hessman F.V.Hinse T.C.Hundertmark M.,Jorgensen U.G.Liebig C.Maier G.Mancini L.Mathiasen M.Rahvar S.,Ricci D.Scarpetta G.Southworth J.Surdej J.Zimmer F.,(The MiNDSTEp Consortium),Allan A.Bramich D.M.Snodgrass C.Steele I.A.Street R.A.(The RoboNet Collaboration)2017-06-28T06:57:52Z2011-04-13T14:24:25ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frmultiple-starssolar-system-planetsapparent-magnitudeWe report the discovery of a planet with a high planet-to-star mass ratio in the microlensing event MOA-2009-BLG-387, which exhibited pronounced deviations over a 12-day interval, one of the longest for any planetary event. The host is an M dwarf, with a mass in the range 0.07M_{sun}_<M_host_<0.49M_{sum}_ at 90% confidence. The planet-star mass ratio q=0.0132+/-0.003 has been measured extremely well, so at the best-estimated host mass, the planet mass is m_p_=2.6 Jupiter masses for the median host mass, M=0.19M_{sun}_.2011A&A...529A.102Bhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/529/A102CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/529/A102https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/529/A102http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/529/A102https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/529/A102https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/529/A102http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/529/A102GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/529/A102/photI-band light curvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintObsObservatory code (1)meta.code;instr.obstycharHJD'Date (HJD'=HJD-2450000)dtime.epochdoubleImagI magnitudemagphot.mag;em.opt.Ifloate_Imag? Error bar on Imagmagstat.error;phot.mag;em.opt.Ifloatnullableres1residuals 1 (2)magstat.fit.residualfloatres2residuals 2 (2)magstat.fit.residualfloatres3residuals 3 (2)magstat.fit.residualfloat