J/AJ/154/210ivo://CDS.VizieR/J/AJ/154/210doi:10.26093/cds/vizier.51540210CDSZhu W.Udalski A.Novati S.C.Chung S.-J.Jung Y.K.Ryu Y.-H.,Shin I.-G.Gould A.Lee C.-U.Albrow M.D.Yee J.C.Han C.,Hwang K.-H.Cha S.-M.Kim D.-J.Kim H.-W.Kim S.-L.Kim Y.-H.Lee Y.,Park B.-G.Pogge R.W.(the KMTNet Collaboration)Poleski R.Mroz P.,Pietrukowicz P.Skowron J.Szymanski M.K.KozLowski S.Ulaczyk K.,Pawlak M.(the OGLE Collaboration)Beichman C.Bryden G.Carey S.,Fausnaugh M.Gaudi B.S.Henderson C.B.Shvartzvald Y.Wibking B.2019-10-01T08:00:12Z2018-08-14T08:18:16ZCDS support team

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

cds-question@unistra.frmilky-way-galaxygravitational-lensingexoplanetsephemeridesinfrared-photometryvisible-astronomyphotometryWe analyze an ensemble of microlensing events from the 2015 Spitzer microlensing campaign, all of which were densely monitored by ground-based high-cadence survey teams. The simultaneous observations from Spitzer and the ground yield measurements of the microlensing parallax vector {pi}_E_, from which compact constraints on the microlens properties are derived, including ~<25% uncertainties on the lens mass and distance. With the current sample, we demonstrate that the majority of microlenses are indeed in the mass range of M dwarfs. The planet sensitivities of all 41 events in the sample are calculated, from which we provide constraints on the planet distribution function. In particular, assuming a planet distribution function that is uniform in log q, where q is the planet-to-star mass ratio, we find a 95% upper limit on the fraction of stars that host typical microlensing planets of 49%, which is consistent with previous studies. Based on this planet-free sample, we develop the methodology to statistically study the Galactic distribution of planets using microlensing parallax measurements. Under the assumption that the planet distributions are the same in the bulge as in the disk, we predict that ~1/3 of all planet detections from the microlensing campaigns with Spitzer should be in the bulge. This prediction will be tested with a much larger sample, and deviations from it can be used to constrain the abundance of planets in the bulge relative to the disk.2017AJ....154..210Zhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/154/210CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toII/213 : OGLE Galactic Bulge periodic variables (Udalski+ 1996)J/AcA/50/1 : OGLE microlensing events in Galactic Bulge (Udalski+, 2000)J/A+A/466/157 : Bulge Microlensing Events (Soto+, 2007)J/ApJ/778/150 : Microlensing events toward the Bulge from MOA-IIJ/ApJS/216/12 : OGLE-III Galactic bulge microlensing eventsJ/MNRAS/458/3012 : OGLE-III Parallax microlensing events (Wyrzykowski+, 2016)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/154/210https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/154/210http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/154/210https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/154/210https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/154/210http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/154/210GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/154/210/table1 (Summary of the 50 events in our sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/154/210/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/154/210/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/154/210/table1?GETtext/xml+votable180.050000true269.21783306-29.283250.0055555555555555565/7205 6/28730 28731 28734 28735 28778 28817 28819 28829 28865 28866 28867 28868 28870 28872https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/154/210?format=asciiInfraredOpticaldefaultJ/AJ/154/210/table1Summary of the 50 events in our samplerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintOGLE[11/1533] OGLE identifier (OGLE-2015-BLG-NNNN)meta.id;meta.mainintRAJ2000Right Ascension in decimal degrees (J2000)degpos.eq.ra;meta.mainDEJ2000Declination in decimal degrees (J2000)degpos.eq.dec;meta.mainGLON[] Galactic longitudedegpos.galactic.lonGLATGalactic latitudedegpos.galactic.latdoubleObs.Date1Subjective selection date (YYYY-MM-DDThh:mm) (1)time.epochcharObs.Date2Objective selection date (1)time.epochnullableFieldOGLE-IV field identifier (BLGNNN)meta.id;obs.fieldcharo_Field[3/30] Cadence of Field; per dayd**-1meta.numberintHJD1[7183.32/7213.65] Heliocentric Julian Date of Spitzer observation start (HJD-2450000.0)dtime.start;obsfloatHJD2[7198.41/7223.07] Heliocentric Julian Date of Spitzer observation end (HJD-2450000.0)dtime.end;obsfloatSNum[17/131] Number of Spitzer observationsmeta.numberintSimbadSimbad column added by the CDSmeta.ref.urlcharJ/AJ/154/210/table2Best-fit parameters and associated uncertainties for the 50 eventse_u0[0.0003/0.12] Uncertainty in u0stat.errorfloate_piEE[0.0017/0.4] Uncertainty in piEEmasstat.errorfloate_I-3.6[0.011/0.6] Uncertainty in I-3.6magstat.errorfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintOGLE[11/1533] OGLE identifier (OGLE-2015-BLG-NNNN)meta.id;meta.mainintSolSolution type (see Equation 9)meta.notecharDelchi2[0/80.8] Difference between given solution and best solution (1)stat.fit.paramfloatt0[7125.53/7236.56] Heliocentric Julian Date of peak time (HJD-2450000.0)dtime.epoch;stat.maxdoublee_t0[0.003/0.5] Uncertainty in t0dstat.errorfloatu0[-0.9943/0.9941] Impact parametersrc.impactParamfloattE[4.39/116] Einstein timescaledtime.scalefloate_tE[0.06/18] Uncertainty in tEdstat.errorfloatpiEN[-1.77/3.2] North component of microlensing parallax {pi}_E,N_maspos.parallaxfloate_piEN[0.0017/0.4] Uncertainty in piENmasstat.errorfloatpiEE[-1.5/0.34] East component of microlensing parallax {pi}_E,E_maspos.parallaxfloatImag[15.132/20.407] Total baseline OGLE-IV I band magnitude (2)magphot.mag;em.opt.IfloatBlend[-0.15/0.956]? Blending fraction in I band (3)stat.fit.paramfloatnullablee_Blend[0.003/0.3]? Uncertainty in Blendstat.errorfloatnullableI-3.6[0.83/10.5] The (I-3.6{mu}m) colormagphot.color;em.IR;em.IRfloat