J/A+A/669/A145ivo://CDS.VizieR/J/A+A/669/A145doi:10.26093/cds/vizier.36690145CDSCugno G.Pearce T.D.Launhardt R.Bonse M.J.Ma J.Henning T.,Quirrenbach A.Segransan D.Matthews E.C.Quanz S.P.Kennedy G.M.,Muller A.Reffert S.Rickman E.L.2024-11-06T20:02:09Z2023-01-26T07:56:55ZCDS support team

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

cds-question@unistra.frmultiple-starsyoung-stellar-objectsphotometryvisible-astronomyWe present the statistical analysis of a subsample of 45 young stars surrounded by protoplanetary disks (PPD). This is the largest imaging survey uniquely focused on PPDs to date. Our goal is to search for young forming companions embedded in the disk material and to constrain their occurrence rate in relation to the formation mechanism. We used Principal Component Analysis based Point Spread Function subtraction techniques to reveal young companions forming in the disks. We calculated detection limits for our datasets and adopted a black-body model to derive temperature upper limits of potential forming planets. We then used Monte Carlo simulations to constrain the population of forming gas giant companions and compare our results to different types of formation scenarios. Our data revealed a new binary system (HD38120) and a recently identified triple system with a brown dwarf companion orbiting a binary system (HD101412), in addition to 12 known companions. Furthermore, we detected signals from 17 disks, two of which (HD72106 and TCrA) were imaged for the first time. We reached median detection limits of L=15.4mag at 2.0", which were used to investigate the temperature of potentially embedded forming companions. We constrained the occurrence of forming planets with semi-major axis a in [20-500] au and Teff in [600-3000], in line with the statistical results obtained for more evolved systems from other direct imaging surveys. These values are obtained under the assumption that extinction from circumstellar and circumplanetary material does not affect the companion signal, but we show the potential impact these factors might have on the detectability of forming objects.2023A&A...669A.145Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/669/A145CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/669/A145https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/669/A145http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/669/A145https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/669/A145https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/669/A145http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/669/A145GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/669/A145/sources (List of studied sources)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/669/A145/sources?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/669/A145/sources?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/669/A145/sources?GETtext/xml+votable180.050000true241.0902083-21.50791670.0055555555555555566/1113 1168-1169 21418 21439 21480 21541 22854 23549 24277 24279 24281 28746 28762 28921 29193 29207 30741 31259 32065 36956 37186 37916 37978 38382 39163 39290 41472 42429 42595 42598 42611 42614 42644 42704 42931 42941 42981 43415 44317 44361-44362 47828https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/669/A145?format=asciiOpticaldefaultJ/A+A/669/A145/sourcesList of studied sourcesSimbadSimbad column added by the CDSmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameStar namemeta.id;meta.maincharRAJ2000Right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Declination (J2000)pos.eq.dec;meta.mainCCShow the contrast curvesmeta.ref.urlcharFileName1Name of the file with contrast curve in subdirectory ccmeta.id;meta.filecharFileName2Name of the fits datacube with residuals in L' in subdirectory fitsmeta.id;meta.fitschar