J/AJ/162/17ivo://CDS.VizieR/J/AJ/162/17doi:10.26093/cds/vizier.51620017CDSKim Y.H.Chung S.-J.Yee J.C.Udalski A.Bond I.A.Jung Y.K.,Gould A.Albrow M.D.Han C.Hwang K.-H.Ryu Y.-H.Shin I.-G.,Shvartzvald Y.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.,(the Kmtnet Collaboration)Poleski R.Mroz P.Skowron J.,Szymanski M.K.Soszynski I.Pietrukowicz P.Kozlowski S.Ulaczyk K.,Rybicki K.A.Iwanek P.Wrona M.Gromadzki M.(the Ogle Collaboration),Abe F.Barry R.Bennett D.P.Bhattacharya A.Donachie M.Fujii H.,Fukui A.Itow Y.Hirao Y.Kirikawa R.Kondo I.Koshimoto N.,Matsubara Y.Muraki Y.Miyazaki S.Ranc C.Rattenbury N.J.Satoh Y.,Shoji H.Sumi T.Suzuki D.Tristram P.J.Tanaka Y.Yamawaki T.,Yonehara A.(the Moa Collaboration)2022-03-16T12:13:06Z2021-11-22T06:49:56ZCDS support team

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

cds-question@unistra.frgravitational-lensinginfrared-photometryvisible-astronomyphotometryWe show that the perturbation at the peak of the light curve of microlensing event KMT-2019-BLG-0371 is explained by a model with a mass ratio between the host star and planet of q~0.08. Due to the short event duration (t_E_~6.5days), the secondary object in this system could potentially be a massive giant planet. A Bayesian analysis shows that the system most likely consists of a host star with a mass M_h_=0.09_-0.05_^+0.14^Msun and a massive giant planet with a mass M_p_=7.70_-3.90_^+11.34^M_Jup_. However, the interpretation of the secondary as a planet (i.e., as having M_p_<13M_Jup_) rests entirely on the Bayesian analysis. Motivated by this event, we conduct an investigation to determine which constraints meaningfully affect Bayesian analyses for microlensing events. We find that the masses inferred from such a Bayesian analysis are determined almost entirely by the measured value of {theta}_E_ and are relatively insensitive to other factors such as the direction of the event (l, b), the lens-source relative proper motion {mu}_rel_, or the specific Galactic model prior.2021AJ....162...17Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/162/17CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/549/A147 : Abundances of microlensed bulge dwarf stars V. (Bensby+, 2013)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)J/AJ/159/261 : LC of microlensing event OGLE-2012-BLG-0838 (Poleski+, 2020)J/AJ/160/148 : RI LC microlensing event OGLE-2018-BLG-1269Lb (Jung+, 2020)J/AJ/160/255 : KMTNet & OGLE I photometry of KMT-2019-BLG-0842 (Jung+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/162/17https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/162/17http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/162/17https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/162/17https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/162/17http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/162/17GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/AJ/162/17/fig1Light curve of KMT-2019-BLG-0371recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTelTelescope identifier; KMTNet, MOA or OGLEmeta.id;instr.telcharFiltFilter used; R or Iinstr.setup;instr.filtercharHJD[7435/8931] Heliocentric Julian Date; HJD-2450000dtime.epochdoubleindexedmag[14.66/21.51] Apparent magnitude in Filtermagphot.magdoublee_mag[0.009/3.2] Uncertainty in magmagstat.error;phot.magdouble