J/AJ/160/148ivo://CDS.VizieR/J/AJ/160/148doi:10.26093/cds/vizier.51600148CDSJung Y.K.Gould A.Udalski A.Sumi T.Yee J.C.Han C.Albrow M.D.,Chung S.-J.Hwang K.-H.Ryu Y.-H.Shin I.-G.Shvartzvald Y.Zhu W.,Zang W.Cha S.-M.Kim D.-J.Kim H.-W.Kim S.-L.Lee C.-U.Lee D.-J.,Lee Y.Park B.-G.Pogge R.W.Mroz P.Szymanski M.K.Skowron J.,Poleski R.Soszynski I.Pietrukowicz P.Kozlowski S.Ulaczyk K.,Rybicki K.A.Iwanek P.Wrona M.Abe F.Barry R.Bennett D.P.,Bond I.A.Bhattacharya A.Donachie M.Fukui A.Hirao Y.Itow Y.,Kondo I.Koshimoto N.Li M.C.A.Matsubara Y.Miyazaki S.Muraki Y.,Nagakane M.Ranc C.Rattenbury N.J.Suematsu H.Sullivan D.J.,Suzuki D.Tristram P.J.Yonehara A.2021-12-06T23:26:20Z2020-12-01T07:17:00ZCDS support team

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

cds-question@unistra.frexoplanetsgravitational-lensinginfrared-photometryvisible-astronomyphotometryWe report the discovery of a planet in the microlensing event OGLE-2018-BLG-1269 with a planet-host mass ratio q~6x10^-4^, i.e., 0.6 times smaller than the Jupiter/Sun mass ratio. Combined with the Gaia parallax and proper motion, a strong one-dimensional constraint on the microlens parallax vector allows us to significantly reduce the uncertainties of lens physical parameters. A Bayesian analysis that ignores any information about light from the host yields that the planet is a cold giant (M_2_=0.69_-0.22_^+0.44^M_J_) orbiting a Sun-like star (M_1_=1.13_-0.35_^+0.72^M_{sun}_) at a distance of D_L_=2.56_-0.62_^+0.92^kpc. The projected planet-host separation is a_{perp}_=4.61_-1.17_^+1.70^au. Using Gaia astrometry, we show that the blended light lies <~12mas from the host and therefore must be either the host star or a stellar companion to the host. An isochrone analysis favors the former possibility at >99.6%. The host is therefore a subgiant. For host metallicities in the range of 0.0<=[Fe/H]<=+0.3, the host and planet masses are then in the range of 1.16<=M_1_/M_{sun}_<=1.38 and 0.74<=M_2_/M_J_<=0.89, respectively. Low host metallicities are excluded. The brightness and proximity of the lens make the event a strong candidate for spectroscopic follow-up both to test the microlensing solution and to further characterize the system.2020AJ....160..148Jhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/160/148CatalogResearchIsServedByTAP VizieR generic servicerelated-toI/337 : Gaia DR1 (Gaia Collaboration, 2016)I/345 : Gaia DR2 (Gaia Collaboration, 2018)J/AcA/50/421 : OGLE-II DIA BUL_SC1 field (Wozniak, 2000)J/A+A/428/587 : Cepheids BVRIJHK dereddened magnitudes (Kervella+, 2004)J/A+A/529/A102 : MOA-2007-BLG-387Lb light curve I band (Batista+, 2011)J/ApJ/756/52 : R-band light curve of QSO J0158-4325 images (Morgan+, 2012)J/A+A/549/A147 : Abundances of microlensed bulge dwarf stars.V. (Bensby+, 2013)J/A+A/616/A183 : R-band light curves of PG 1115+080 (Bonvin+, 2018)J/AJ/159/98 : I LC of the microlensing event KMT-2016-BLG-1836 (Yang+, 2020)J/AJ/159/116 : I-band light curves of OGLE-2015-BLG-1771Lb (Zhang+, 2020)J/AJ/159/256 : Light curve of OGLE-2018-BLG-0677 (Herrera-Martin+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/160/148https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/160/148http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/160/148https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/160/148https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/160/148http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/160/148GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/AJ/160/148/figure1Combined table from original tablesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintHJDHeliocentric Julian Date, HJD-2450000dtime.epochdoubleInstInstrument usedmeta.id;instrcharmagObserved magnitudemagphot.magdoublee_magUncertainty in magmagstat.error;phot.magdouble