J/A+A/617/A135ivo://CDS.VizieR/J/A+A/617/A135doi:10.26093/cds/vizier.36170135CDSMustill A.-J.Davies M.-B.Lindegren L.2018-11-05T10:52:51Z2018-10-02T08:49:03ZCDS support team

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

cds-question@unistra.frgravitational-lensingastrometryvisible-astronomytrigonometric-parallaxnarrow-band-photometryproper-motionsGaia DR2 offers unparalleled precision on stars' parallaxes and proper motions. This allows the prediction of microlensing events for which the lens stars (and any planets they possess) are nearby and may be well studied and characterised. We identify a number of potential microlensing events that will occur before the year 2035.5, 20 years from the Gaia DR2 reference epoch. We query Gaia DR2 for potential lenses within 100pc, extract parallaxes and proper motions of the lenses and background sources, and identify potential lensing events. We estimate the lens masses from Priam effective temperatures, and use these to calculate peak magnifications and the size of the Einstein radii relative to the lens stars' habitable zones. We identify 7 future events with a probability >10% of an alignment within one Einstein radius. Of particular interest is DR2 5918299904067162240 (WISE J175839.20-583931.6), magnitude G=14.9, which will lens a G=13.9 background star in early 2030, with a median 23% net magnification. Other pairs are typically fainter, hampering characterisation of the lens (if the lens is faint) or the ability to accurately measure the magnification (if the source is much fainter than the lens). Of timely interest is DR2 4116504399886241792 (2MASS J17392440-2327071), which will lens a background star in July 2020, albeit with weak net magnification (0.03%). Median magnifications for the other 5 high-probability events range from 0.3% to 5.3%. The Einstein radii for these lenses are 1-10 times the radius of the habitable zone, allowing these lensing events to pick out cold planets around the ice line, and filling a gap between transit and current microlensing detections of planets around very low-mass stars. We provide a catalogue of the predicted events to aid future characterisation efforts. Current limitations include a lack of many high-proper motion objects in Gaia DR2 and often large uncertainties on the proper motions of the background sources (or only 2-parameter solutions). Both of these deficiencies will be rectified with Gaia DR3 in 2020. Further characterisation of the lenses is also warranted to better constrain their masses and predict the photometric magnifications.2018A&A...617A.135Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/617/A135CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/617/A135https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/617/A135http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/617/A135https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/617/A135https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/617/A135http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/617/A135GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/617/A135/mlens (Microlens source-lens pairs)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/617/A135/mlens?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/617/A135/mlens?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/617/A135/mlens?GETtext/xml+votable180.050000true347.83911420839868.983450230934610.0055555555555555566/824 2262 14430 14514 14586 15738 20851 23735 24338 28870 29215 29232 29249 30564 32773 33711 36884 37180 37215 38450 39287 39883 41215 41350 41539 41929 41946 42052 47347 488151.9867573869263685e-19 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/617/A135?format=asciiOpticaldefaultJ/A+A/617/A135/mlensMicrolens source-lens pairsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintLensGaia DR2 id of lens star (DR2id_lens)meta.id;meta.mainGmaglGaia DR2 G magnitude of lens (Gmag_lens)magphot.mag;em.optfloatRAlGaia DR2 right ascension of lens (ICRS, at epoch 2015.5) (RAdeg_lens)degpos.eq.ra;meta.mainDElGaia DR2 declination of lens (ICRS, at epoch 2015.5) (DEdeg_lens)degpos.eq.dec;meta.mainpmRAl? Gaia DR2 proper motion in RA of lens (pmRA_lens)mas/yrpos.pm;pos.eq.radoublenullablepmDEl? Gaia DR2 proper motion in Dec of lens (pmDE_lens)mas/yrpos.pm;pos.eq.decdoublenullableplxl? Gaia DR2 parallax of lens (plx_lens)maspos.parallax.trigfloatnullableb_Teffl? Priam Teff of lens (16th percentile) (Teff_lens_low)Kphys.temperature.effectiveintnullableTeffl? Priam Teff of lens (50th percentile) (Teff_lens)Kphys.temperature.effectiveintnullableB_Teffl? Priam Teff of lens (84th percentile) (Teff_lens_high)Kphys.temperature.effectiveintnullablebMasslLens mass from Teff_lens_low (M_lens_low)solMassphys.massfloatMasslLens mass from Teff_lens (M_lens)solMassphys.massfloatBMasslLens mass from Teff_lens_high (M_lens_high)solMassphys.massfloatbLumlLens luminosity from Teff_lens_low (L_lens_low)solLumphys.luminositydoubleLumlLens luminosity from Teff_lens (L_lens)solLumphys.luminositydoubleBLumlLens luminosity from Teff_lens_high (L_lens_high)solLumphys.luminositydoublebRHZHabitable zone radius from Teff_lens_low (RHZ_low)AUphys.size.radiusdoubleRHZHabitable zone radius from Teff_lens (RHZ)AUphys.size.radiusdoubleBRHZHabitable zone radius from Teff_lens_high (RHZ_high)AUphys.size.radiusdoublebREasAngular Einstein radius from Teff_lens_low (RE_as_low)arcsecphys.angSizedoubleREasAngular Einstein radius from Teff_lens (RE_as)arcsecphys.angSizedoubleBREasAngular Einstein radius from Teff_lens_high (RE_as_high)arcsecphys.angSizedoublebREauPhysical Einstein radius from Teff_lens_low (RE_au_low)AUphys.size.radiusdoubleREauPhysical Einstein radius from Teff_lens (RE_au)AUphys.size.radiusdoubleBREauPhysical Einstein radius from Teff_lens_high (RE_au_high)AUphys.size.radiusdoubleSourceGaia DR2 id of source star (DR2id_source)meta.id.parentGmagGaia DR2 G magnitude of source (Gmag_source)magphot.mag;em.optfloatRAsdegGaia DR2 right ascension of source (ICRS, at epoch 2015.5) (RAdeg_source)degpos.eq.raDEsdegGaia DR2 declination of source (ICRS, at epoch 2015.5) (DEdeg_source)degpos.eq.decpmRAsGaia DR2 proper motion in RA of source (pmRA_source)mas/yrpos.pm;pos.eq.rafloatpmDEsGaia DR2 proper motion in Dec of source (pmDE_source)mas/yrpos.pm;pos.eq.decfloatplxsGaia DR2 parallax of source (plx_source)maspos.parallax.trigfloatprob1REProbability of alignment within one Einstein radius (prob_1RE)%statfloatb_DminClosest approach (16th percentile) (Dmin_low)arcsecpos.angDistancefloatDminClosest approach (50th percentile) (Dmin)arcsecpos.angDistancefloatB_DminClosest approach (84th percentile) (Dmin_high)arcsecpos.angDistancefloatb_maxmagMaximum magnification ignoring dilution (16th percentile) (max_mag_low)phot.mag;arith.ratiodoublemaxmagMaximum magnification ignoring dilution (50th percentile) (max_mag)phot.mag;arith.ratiodoubleB_maxmagMaximum magnification ignoring dilution (84th percentile) (max_mag_high)phot.mag;arith.ratiodoubleb_maxmagnetMaximum magnification including dilution (16th percentile) (max_mag_net_low)phot.mag;arith.ratiodoublemaxmagnetMaximum magnification including dilution (50th percentile) (max_mag_net)phot.mag;arith.ratiodoubleB_maxmagnetMaximum magnification including dilution (84th percentile) (max_mag_net_high)phot.mag;arith.ratiodoubleb_TmaxTime of maximum magnification (16th percentile) (Tmax_low)time.epoch;stat.error;stat.minnullableTmaxTime of maximum magnification (50th percentile) (Tmax)time.epochnullableB_TmaxTime of maximum magnification (84th percentile) (Tmax_high)time.epoch;stat.error;stat.maxnullableb_durTime undiluted magnification exceeds 10^-2^ (16th percentile) (duration_low)dtime.intervalfloatdurTime undiluted magnification exceeds 10^-2^ (50th percentile) (duration)dtime.intervalfloatB_durTime undiluted magnification exceeds 10^-2^ (84th percentile) (duration_high)dtime.intervalfloatb_durnetTime diluted magnification exceeds 10^-4^ (16th percentile) (duration_net_low)dtime.intervalfloatdurnetTime diluted magnification exceeds 10^-4^ (50th percentile) (duration_net)dtime.intervalfloatB_durnetTime diluted magnification exceeds 10^-4^ (84th percentile) (duration_net_high)dtime.intervalfloatb_SolelongSolar elongation at peak magnification (16th percentile) (Sol_elong_low)degpos.angDistance;stat.maxfloatSolelongSolar elongation at peak magnification (50th percentile) (Sol_elong)degpos.angDistance;stat.maxfloatB_SolelongSolar elongation at peak magnification (84th percentile) (Sol_elong_high)degpos.angDistance;stat.maxfloat_RA.icrsRight ascension (ICRS) at Epoch=J2000, proper motions taken into accountdegpos.eq.ranullableindexed_DE.icrsDeclination (ICRS) at Epoch=J2000, proper motions taken into accountdegpos.eq.decnullableindexed