J/A+A/610/A24ivo://CDS.VizieR/J/A+A/610/A24doi:10.26093/cds/vizier.36100024CDSFedele D.Tazzari M.Booth R.Testi L.Clarke C.J.Pascucci I.,Kospal A.Semenov D.Bruderer S.Henning T.Teague R.2018-08-07T06:12:40Z2018-02-20T08:21:40ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsexoplanetsradio-continuum-emissionThis paper presents new high angular resolution ALMA 1.3mm dust continuum observations of the protoplanetary system AS 209 in the Ophiuchus star forming region. The dust continuum emission is characterized by a main central core and two prominent rings at r=75au and r=130au intervaled by two gaps at at r=62au and r=103au. The two gaps have different widths and depths, with the inner one being narrower and shallower. We determined the surface density of the millimeter dust grains using the 3D radiative transfer disk code dali. According to our fiducial model the inner gap is partially filled with millimeter grains while the outer gap is largely devoid of dust. The inferred surface density is compared to 3D hydrodynamical simulations (FARGO-3D) of planet-disk interaction. The outer dust gap is consistent with the presence of a giant planet (M_planet_~0.8M_Saturn_); the planet is responsible for the gap opening and for the pile-up of dust at the outer edge of the planet orbit. The simulations also show that the same planet could be the origin of the inner gap at r=62au. The relative position of the two dust gaps is close to the 2:1 resonance and we have investigated the possibility of a second planet inside the inner gap. The resulting surface density (including location, width and depth of the two dust gaps) are in agreement with the observations. The properties of the inner gap pose a strong constraint to the mass of the inner planet (M_planet_<0.1M_J_). In both scenarios (single or pair of planets), the hydrodynamical simulations suggest a very low disk viscosity ({alpha}<10^-4^). Given the young age of the system (0.5-1Myr), this result implies that the formation of giant planets occurs on a timescale of <~1Myr.2018A&A...610A..24Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/610/A24CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/610/A24https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/610/A24http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/610/A24https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/610/A24https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/610/A24http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/610/A24GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/610/A24/list (Information on fits image)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/610/A24/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/610/A24/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/610/A24/list?GETtext/xml+votable180.050000true252.31372-14.369170.005555555555555556Associated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/610/A246/30741https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/610/A24?format=asciiRadiodefaultJ/A+A/610/A24/listInformation on fits imagerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRAJ2000Right Ascension of center (J2000)degpos.eq.ra;meta.mainDEJ2000Declination of center (J2000)degpos.eq.dec;meta.mainNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintObs.DateObservation date (YYYY-MM-DDThh:mm:ss.ssssss)time.epoch;obscharFreqObserved frequencyGHzem.freqfloatsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory fitsmeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitscharAssocDataAssociated Data web pagemeta.bib.pagechar