J/AJ/162/203ivo://CDS.VizieR/J/AJ/162/203doi:10.26093/cds/vizier.51620203CDSHanHan C.Udalski A.Lee C.-U.Kim D.Ryu Y.-H.Albrow M.D.ChungS.-J.Gould A.Hwang K.-H.Kil Jung Y.Kim H.-W.Shin I.-G.,Shvartzvald Y.Yee J.C.Zang W.Cha S.-M.Kim D.-J.Kim S.-L.LeeD.-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.RybickiK.A.Iwanek P.Wrona M.Gromadzki M.2022-05-18T12:44:58Z2022-01-25T12:16:18ZCDS support team

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

cds-question@unistra.frgravitational-lensingexoplanetsinfrared-photometryvisible-astronomyphotometryWe analyze the microlensing event OGLE-2019-BLG-0304, whose light curve exhibits two distinctive features: a deviation in the peak region and a second bump appearing ~61days after the main peak. Although a binary-lens model can explain the overall features, it leaves subtle but noticeable residuals in the peak region. We find that the residuals can be explained by the presence of either a planetary companion located close to the primary of the binary lens (3L1S model) or an additional close companion to the source (2L2S model). Although the 3L1S model is favored over the 2L2S model, with {Delta}{chi}2~8, securely resolving the degeneracy between the two models is difficult with the currently available photometric data. According to the 3L1S interpretation, the lens is a planetary system, in which a planet with a mass 0.51_-0.23_^+0.51^M_J_ is in an S-type orbit around a binary composed of stars with masses 0.27_-0.12_^+0.27^M{odot} and 0.10_-0.04_^+0.10^M{odot}. According to the 2L2S interpretation, however, the source is composed of G- and K-type giant stars and the lens is composed of a low-mass M dwarf and a brown dwarf with masses 0.12_-0.05_^+0.12^M{odot} and 0.045_-.019_^+0.045^M{odot}, respectively. The event illustrates the need for thorough model testing in the interpretation of lensing events with complex features in light curves.2021AJ....162..203Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/162/203CatalogResearchIsServedByTAP VizieR generic servicerelated-toII/213 : OGLE Galactic Bulge periodic variables (Udalski+ 1996)I/345 : Gaia DR2 (Gaia Collaboration, 2018)J/AJ/137/3181 : HW Vir differential VR light curves (Lee+, 2009)J/A+A/549/A147 : Abundances of microlensed bulge dwarf stars. V (Bensby+, 2013)J/AJ/159/256 : Light curve of OGLE-2018-BLG-0677 (Herrera-Martin+, 2020)J/AJ/159/116 : I-band light curves of OGLE-2015-BLG-1771Lb (Zhang+, 2020)J/A+A/649/A90 : KMT-2018-BLG-1025Lb I light curve (Han+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/162/203https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/162/203http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/162/203https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/162/203https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/162/203http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/162/203GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/AJ/162/203/fig1Light curve of the microlensing event OGLE-2019-BLG-0304recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintInstInstrument used (1)instr.setupcharHJD[7415/8779] Heliocentric Julian Date; HJD-2450000dtime.epochdoubleImag[13.7/18.3] Apparent I band magnitudemagphot.mag;em.opt.Ifloate_Imag[0.002/0.07] Uncertainty in Imagmagstat.error;phot.magfloat