J/AJ/156/286ivo://CDS.VizieR/J/AJ/156/286doi:10.26093/cds/vizier.51560286CDSStone J.M.Skemer A.J.Hinz P.M.Bonavita M.Kratter K.M.Maire A.-L.,Defrere D.Bailey V.P.Spalding E.Leisenring J.M.Desidera S.,Bonnefoy M.Biller B.Woodward C.E.Henning T.Skrutskie M.F.,Eisner J.A.Crepp J.R.Patience J.Weigelt G.De Rosa R.J.,Schlieder J.Brandner W.Apai D.Su K.Ertel S.Ward-Duong K.,Morzinski K.M.Schertl D.Hofmann K.-H.Close L.M.Brems S.S.,Fortney J.J.Oza A.Buenzli E.Bass B.2020-01-31T15:52:22Z2019-05-09T07:46:59ZCDS support team

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

cds-question@unistra.frmultiple-starsinterferometrystellar-distanceinfrared-photometrystellar-spectral-typesstellar-agesstellar-masseschemical-abundancesstellar-radiisurveysWe present the results of the largest L' (3.8 {mu}m) direct imaging survey for exoplanets to date, the Large Binocular Telescope Interferometer Exozodi Exoplanet Common Hunt (LEECH). We observed 98 stars with spectral types from B to M. Cool planets emit a larger share of their flux in L' compared to shorter wavelengths, affording LEECH an advantage in detecting low-mass, old, and cold-start giant planets. We emphasize proximity over youth in our target selection, probing physical separations smaller than other direct imaging surveys. For FGK stars, LEECH outperforms many previous studies, placing tighter constraints on the hot-start planet occurrence frequency interior to ~20 au. For less luminous, cold-start planets, LEECH provides the best constraints on giant-planet frequency interior to ~20 au around FGK stars. Direct imaging survey results depend sensitively on both the choice of evolutionary model (e.g., hot- or cold-start) and assumptions (explicit or implicit) about the shape of the underlying planet distribution, in particular its radial extent. Artificially low limits on the planet occurrence frequency can be derived when the shape of the planet distribution is assumed to extend to very large separations, well beyond typical protoplanetary dust-disk radii (~<50 au), and when hot-start models are used exclusively. We place a conservative upper limit on the planet occurrence frequency using cold-start models and planetary population distributions that do not extend beyond typical protoplanetary dust-disk radii. We find that ~<90% of FGK systems can host a 7-10 M_Jup_ planet from 5 to 50 au. This limit leaves open the possibility that planets in this range are common.2018AJ....156..286Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/156/286CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/ApJ/687/1264 : Age estimation for solar-type dwarfs (Mamajek+, 2008)J/PASP/122/162 : Direct imaging of exoplanets (Beichman+, 2010)J/ApJ/768/2 : Spitzer and Herschel observations of debris disksJ/A+A/591/A84 : Search for UMa group companions (Ammler-von Eiff+, 2016)J/AJ/156/137 : Wide-orbit Exoplanet search with IR Direct imaginghttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/156/286https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/156/286http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/156/286https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/156/286https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/156/286http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/156/286GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/156/286/table2 (Target summary)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/156/286/table2?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/156/286/table2?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/156/286/table2?GETtext/xml+votable180.050000true1.6529.021390.0055555555555555566/155 350 666 689 1397 1704 1875 2340 4871 5074 5108 5311 5631 6082 6385 6420 7205 7221 7227 7332 7763 8496 8687 8717 8788 8790 9310 10096 10149 10457 10568 10695 10741 10783 11109 11126 11145 11165 11193 11202 11204 11225 11500 11917 11946 12676 13313 14144 14208 14777 14906 15144 15583 17486 17907 17953 18210 19329 20328 20439 21060 21386 22334 22773 22822 23140 23230 23342 23408 23502 23774 23826 23895 24151 24480 27163 27374 27574 27735 27884 27909 28341 28352 28605 30229 30543 30655 31399 31448 31849 31929 32061 32496 36664 36697 44833 485894.925240337479573e-20 6.203309766548433e-20https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/156/286?format=asciiInfrareddefaultJ/AJ/156/286/table2Target summaryNameTarget namemeta.id;meta.maincharprimaryrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintn_NameNote on Name (1)meta.notecharONameOther namemeta.idmoreindicates data in other tables for this starmeta.ref.urlcharRAJ2000Hour of Right Ascension (J2000)pos.eq.ra;meta.mainDEJ2000Degree of Declination (J2000)pos.eq.dec;meta.mainDist[3.2/78.25] Distancepcpos.distance;pos.heliocentricfloatVmag[0.03/10.17] V band magnitudemagphot.mag;em.opt.VfloatKmag[0.13/6.88]? K band magnitudemagphot.mag;em.IR.KfloatnullableSpTypeSpectral typesrc.spTypecharLmag[0.13/6.77] L' band magnitude (2)magphot.mag;em.IR.3-4umfloatAge[10/1650] Age (3)Myrtime.ageintMass[0.4/4.07] Stellar mass (4)solMassphys.massfloatSublistTarget sublist (5)meta.codecharSimbadSimbad column added by the CDSmeta.ref.urlcharJ/AJ/156/286/table3Best-fit age, mass, and metallicity for observed stars in the Field-B/A sublistrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharAge[50/1646] Best-fit ageMyrtime.age;meta.modelledintb_Age16-84[14/1249] Lower value of age in the interval between 16% and 84% in the cumulative distribution function of the posterior probability distributionMyrtime.age;stat.minintB_Age16-84[81/1723] Upper value of age in the interval between 16% and 84% in the cumulative distribution function of the posterior probability distributionMyrtime.age;stat.maxintb_Age2.5-97.5[7/1045] Lower value of age in the interval between 2.5% and 97.5% in the cumulative distribution function of the posterior probability distributionMyrtime.age;stat.minintB_Age2.5-97.5[124/5477] Upper value of age in the interval between 2.5% and 97.5% in the cumulative distribution function of the posterior probability distributionMyrtime.age;stat.maxintMass[1.5/4.5] Best-fit masssolMassphys.mass;meta.modelledfloatb_Mass16-84[1.4/4.4] Lower value of mass in the interval between 16% and 84% in the cumulative distribution function of the posterior probability distributionsolMassphys.mass;stat.minfloatB_Mass16-84[1.5/4.5] Upper value of mass in the interval between 16% and 84% in the cumulative distribution function of the posterior probability distributionsolMassphys.mass;stat.maxfloatb_Mass2.5-97.5[1.4/4.3] Lower value of mass in the interval between 2.5% and 97.5% in the cumulative distribution function of the posterior probability distributionsolMassphys.mass;stat.minfloatB_Mass2.5-97.5[1.5/4.5] Upper value of mass in the interval between 2.5% and 97.5% in the cumulative distribution function of the posterior probability distributionsolMassphys.mass;stat.maxfloatlogZ[-0.26/0.04] Best-fit metallicity log_10_(Z/Z_{sun}_)log(Sun)phys.abund.Z;meta.modelledfloatb_logZ16-84[-0.27/-0.11] Lower value of metallicity in the interval between 16% and 84% in the cumulative distribution function of the posterior probability distributionlog(Sun)phys.abund.Z;stat.minfloatB_logZ16-84[-0.13/0.09] Upper value of metallicity in the interval between 16% and 84% in the cumulative distribution function of the posterior probability distributionlog(Sun)phys.abund.Z;stat.maxfloatb_logZ2.5-97.5[-0.3/-0.17] Lower value of metallicity in the interval between 2.5% and 97.5% in the cumulative distribution function of the posterior probability distributionlog(Sun)phys.abund.Z;stat.minfloatB_logZ2.5-97.5[-0.04/0.19] Upper value of metallicity in the interval between 2.5% and 97.5% in the cumulative distribution function of the posterior probability distributionlog(Sun)phys.abund.Z;stat.maxfloatJ/AJ/156/286/table4LEECH observing logNameStar namemeta.id;meta.maincharDateObservation datetime.epoch;obsnullableSeeing[0.6/2.1] Mean seeing (1)arcsecinstr.obsty.seeing;stat.meanfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordinte_Seeing[0/0.7]? Standard deviation of the seeing (1)arcsecstat.error;instr.obsty.seeingfloatnullableTint-l[10/4794]? Exposure time with the left side of LBTstime.duration;obs.exposureintnullableRot-l[0/169]? Rotation angle with the left side of LBTdeginstr.paramintnullableTint-r[105/6675]? Exposure time with the right side of LBTstime.duration;obs.exposureintnullableRot-r[3/170]? Rotation angle with the right side of LBTdeginstr.paramintnullableJ/AJ/156/286/table6Summary of binary system parametersNameStar namemeta.id;meta.maincharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintn_Name[d] Note on Name (1)meta.notecharM1[0.85/3.48] Mass of the primarysolMassphys.massfloatM2[0.3/2.7]? Mass of the secondarysolMassphys.massfloatnullableM2/M1[0.09/1] Mass ratio (2)phys.massfloatSep[0.003/8]? Separationarcsecpos.angDistancefloatnullablee[0/0.92]? Eccentricitysrc.orbital.eccentricityfloatnullableacrit-cs[5.9/109.7]? Circumstellar critical radius a_crit_^cs^ (3)AUphys.size.radiusfloatnullableacrit-cb[0.06/972] Circumbinary critical radius a_crit_^cb^ (4)AUphys.size.radiusfloatPer[4.02/1202.2]? Perioddtime.periodfloatnullabler_acritReference for a_crit_meta.ref;pos.framecharBibcodeBibcode of the referencemeta.bib.bibcodechar