J/A+A/603/A3ivo://CDS.VizieR/J/A+A/603/A3doi:10.26093/cds/vizier.36030003CDSVigan A.Bonavita M.Biller B.Forgan D.Rice K.Chauvin G.,Desidera S.Meunier J.-C.Delorme P.Schlieder J. E.Bonnefoy M.,Carson J.Covino E.Hagelberg J.Henning T.Janson M.Lagrange A.-M.,Quanz S. P.Zurlo A.Beuzit J.-L.Boccaletti A.Buenzli E.Feldt M.,Girard J. H. V.Gratton R.Kasper M.Le Coroller H.Mesa D.Messina S.,Meyer M.Montagnier G.Mordasini C.Mouillet D.Moutou C.Reggiani M.,Segransan D.Thalmann C.2017-09-04T08:06:45Z2017-08-21T10:20:31ZCDS support team

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

cds-question@unistra.froptical-observationcatalogsstellar-agesstellar-distanceUnderstanding the formation and evolution of giant planets (>1M_Jup_) at wide orbital separation (>5AU) is one of the goals of direct imaging. Over the past 15 years, many surveys have placed strong constraints on the occurrence rate of wide-orbit giants, mostly based on non-detections, but very few have tried to make a direct link with planet formation theories. In the present work, we combine the results of our previously published VLT/NaCo large program with the results of 12 past imaging surveys to constitute a statistical sample of 199 FGK stars within 100 pc, including three stars with sub-stellar companions. Using Monte Carlo simulations and assuming linear flat distributions for the mass and semi-major axis of planets, we estimate the sub-stellar companion frequency to be within 0.75-5.70% at the 68% confidence level (CL) within 20-300AU and 0.5-75M_Jup_, which is compatible with previously published results. We also compare our results with the predictions of state-of-the-art population synthesis models based on the gravitational instability (GI) formation scenario with and without scattering. We estimate that in both the scattered and non-scattered populations, we would be able to detect more than 30% of companions in the 1-75M_Jup_ range (95% CL). With the three sub-stellar detections in our sample, we estimate the fraction of stars that host a planetary system formed by GI to be within 1.0-8.6% (95% CL). We also conclude that even though GI is not common, it predicts a mass distribution of wide-orbit massive companions that is much closer to what is observed than what the core accretion scenario predicts. Finally, we associate the present paper with the release of the Direct Imaging Virtual Archive (DIVA), a public database that aims at gathering the results of past, present, and future direct imaging surveys.2017A&A...603A...3Vhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/603/A3CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/A+A/573/A126 : VLT/NaCo Large program I. Sample (Desidera+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/603/A3https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/603/A3http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/603/A3https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/603/A3https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/603/A3http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/603/A3GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/603/A3/tablea1 (Full NaCo-LP (table A.1))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/603/A3/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/603/A3/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/603/A3/tablea1?GETtext/xml+votable180.050000true1.46875-41.75305560.0055555555555555566/765 814 819 871 940 1603 1762 1875 2101 2574 2966 3786 3922 4190 4591 4674 4871 5088 5322 5413 7763 7854 8357 8424 8985 8995 10089 10741 10826 10914 11015 11126 11226 12228 12388 12592 12770 13243 13301 13487 13674 14208 15887 16134 16220 16393 16426 16606 16853 16930 17016 17274 17425 17552 17605 17887 19509 19598 20166 20327-20328 20332 20544 20657 21060 21118 21217 21418 21424 21726 21953 21956 22146 23143 23369 23895 24239 24633 25015 25056 25224 25793 25948 25998 26651 26924 26997 27006 27374 27395 27462 27973 28041 28122 28784 28849 29569 29718 29993 31425 31998 32147 32520 32617 32844 32937 33100 33312 33500 33508 33548 33694 33838 34074 34146 34164 34203 34244-34245 34423 34436 34683 34733 34757 34825 34829 34886 34905 34909 34930 35497 35802 36261 36308 36664 36697 36713 37414 37419 37607 37616 38061 38137 38151 38765 38910 38950 39044 39123 39579 39735 40242 40717 41158 41528 41565 41647 41960 42493 42555 42601 42751 42815 43014 43209 43432 43533 43639 44324 44377 44792 45072 45253 45351 45384 45388 45538 45564 45621 45927 46383 46520 46640 46925 46987 46997 47101 47205 47287 47598 47626 48045 48163 48559 48651https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/603/A3?format=asciiOpticaldefaultJ/A+A/603/A3/tablea1Full NaCo-LP (table A.1)SimbadNameSimbad column added by the CDSmeta.idcharSpTypeMK spectral typesrc.spTypecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintTargetStar namemeta.id;meta.maincharRAJ2000Right ascension (J2000.0)pos.eq.ra;meta.mainDEJ2000Declination (J2000.0)pos.eq.dec;meta.mainSurveysPrevious direct imaging surveys (1)meta.bibcharMGName of the moving group or association (2)meta.id.parentcharAgeOptimal ageMyrtime.ageintb_AgeMinimum ageMyrtime.age;stat.minintB_AgeMaximum ageMyrtime.age;stat.maxintDistDistance of the starpcpos.distance;pos.heliocentricfloat[Fe/H]? Metalicityphys.abund.FefloatnullableMassStellar masssolMassphys.massfloat