J/AJ/167/154ivo://CDS.VizieR/J/AJ/167/154doi:10.26093/cds/vizier.51670154CDSKirikawa R.Sumi T.Bennett D.P.Suzuki D.Koshimoto N.Miyazaki S.,Bond I.A.Udalski A.Rattenbury N.J. (The Leading Authors)Abe F.,Barry R.Bhattacharya A.Fujii H.Fukui A.Hamada R.Hirao Y.,Ishitani Silva S.Itow Y.Matsubara Y.Muraki Y.Olmschenk G.Ranc C.,Satoh Y.K.Tomoyoshi M.Tristram P.J.Vandorou A.Yama H.,Yamashita K. (The MOA Collaboration)Mroz P.Poleski R.Skowron J.,Szymanski M.K.Soszynski I.Pietrukowicz P.Kozlowski S.Ulaczyk K.,Mroz M.J. (The OGLE Collaboration)2024-11-06T20:19:34Z2024-06-04T07:34:01ZCDS support team

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

cds-question@unistra.frexoplanetslate-type-starsinfrared-photometryvisible-astronomyphotometryWe present the analysis of the microlensing event OGLE-2014-BLG-0221, a planetary candidate event discovered in 2014. The photometric light curve is best described by a binary-lens single-source model. Our light-curve modeling finds two degenerate models, with event timescales of tE~70days and ~110days. These timescales are relatively long, indicating that the discovered system would possess a substantial mass. The two models are similar in their planetary parameters with a Jupiter mass ratio of q~10^-3^ and a separation of s~1.1. Bayesian inference is used to estimate the physical parameters of the lens, revealing that the shorter timescale model predicts 65% and 25% probabilities of a late-type star and white dwarf host, respectively, while the longer timescale model favors a black hole host with a probability ranging from 60% to 95%, under the assumption that stars and stellar remnants have equal probabilities of hosting companions with planetary mass ratios. If the lens is a remnant, this would be the second planet found by microlensing around a stellar remnant. The current separation between the source and lens stars is 41-139mas depending on the models. This indicates the event is now ready for high-angular-resolution follow-up observations to rule out either of the models. If precise astrometric measurements are conducted in multiple bands, the centroid shift due to the color difference between the source and lens would be detected in the luminous lens scenario.2024AJ....167..154Khttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/167/154CatalogResearchIsServedByTAP VizieR generic servicerelated-toII/323 : OGLE-III Bulge Photometric Catalog (Szymanski+ 2011)J/ApJS/101/117 : UBVRIJHKLMNQ photometry in Taurus-Auriga (Kenyon+ 1995)J/A+A/529/A75 : Limb-darkening coefficients (Claret+, 2011)J/A+A/533/A134 : Abundances of microlensed stars in the Bulge (Bensby+, 2011)J/A+A/587/A61 : BlackCAT, stellar-mass BH X-ray trans. (Corral-Santana+, 2016)J/ApJS/244/29 : Microlensing events toward the Galactic bulge (Mroz+, 2019)J/AJ/161/54 : VRI photometry of MOA 2009-BLG-319 (Terry+, 2021)J/A+A/664/A159 : Radial velocities of Galactic SB1s (Mahy+, 2022)J/other/NatAs/6.1085 : Light curve for VFTS 243 (Shenar+, 2022)J/AJ/166/6 : GaiaDR34373465352415301632 abundances (Chakrabarti+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/167/154https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/167/154http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/167/154https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/167/154https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/167/154http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/167/154GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticalInfrareddefaultJ/AJ/167/154/fig1The light curve of OGLE-2014-BLG-0221recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFiltFilter used; I, MOA_Red or Vinstr.setup;instr.filtercharHJD[5266/8743] Heliocentric Julian Date, JD-2450000dtime.epochdoubleindexedFlux[-2858/8418] Observed fluxphot.flux.density;em.optfloate_Flux[1/1752] Uncertainty in Fluxstat.error;phot.fluxfloat