J/A+A/591/A108ivo://CDS.VizieR/J/A+A/591/A108doi:10.26093/cds/vizier.35910108CDSOlofsson J.Samland M.Avenhaus H.Caceres C.Henning T.Moor A.,Milli J.Canovas H.Quanz S. P.Schreiber M. R.Augereau J.-C.,Bayo A.Bazzon A.Beuzit J.-L.Boccaletti A.Buenzli E.Casassus S.,Chauvin G.Dominik C.Desidera S.Feldt M.Gratton R.Janson M.,Lagrange A.-M.Langlois M.Lannier J.Maire A.-L.Mesa D.Pinte C.,Rouan D.Salter G.Thalmann C.Vigan A.2016-06-22T08:43:00Z2016-06-22T09:37:51ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsgalaxy-classification-systemspolarimetryDebris disks offer valuable insights into the latest stages of circumstellar disk evolution, and can possibly help us to trace the outcomes of planetary formation processes. In the age range 10 to 100Myr, most of the gas is expected to have been removed from the system, giant planets (if any) must have already been formed, and the formation of terrestrial planets may be on-going. Pluto-sized planetesimals, and their debris released in a collisional cascade, are under their mutual gravitational influence, which may result into non-axisymmetric structures in the debris disk. Here we present new VLT/SPHERE and ALMA observations of the debris disk around the 40Myr-old solar-type star HD61005. We resolve the disk at unprecedented resolution both in the near-infrared (in scattered and polarized light) and at millimeter wavelengths. We perform a detailed modeling of these observations, including the spectral energy distribution. Thanks to the new observations, we propose a solution for both the radial and azimuthal distribution of the dust grains in the debris disk. We find that the disk has a moderate eccentricity and that the dust density is two times larger at the pericenter compared to the apocenter. With no giant planets detected in our observations, we investigate alternative explanations besides planet-disk interactions to interpret the inferred disk morphology. We postulate that the morphology of the disk could be the consequence of a massive collision between 1000km-sized bodies at 61 au. If this interpretation holds, it would put stringent constraints on the formation of massive planetesimals at large distances from the star.2016A&A...591A.108Ohttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/591/A108CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/591/A108https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/591/A108http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/591/A108https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/591/A108https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/591/A108http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/591/A108GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/591/A108/list (List of images in the fits file)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/591/A108/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/591/A108/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/591/A108/list?GETtext/xml+votable180.050000true113.94775-32.203890.0055555555555555566/39735https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/591/A108?format=asciiOpticaldefaultJ/A+A/591/A108/listList of images in the fits filerecnoRecord 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.mainscaleScale of the imagearcsec/pixinstr.scaledoubleNxNumber of pixels along X-axismeta.numberintNyNumber of pixels along Y-axismeta.numberintlambdaWavelength for observed bandumem.wlfloatsizeSize of FITS fileKibytephys.size;meta.fitsintHDU[1/6] Image HDU number in the fits filemeta.id;meta.mainintFileNameName of FITS filemeta.id;meta.fitscharTitleTitle of the imagemeta.titlechar