J/A+A/619/A161ivo://CDS.VizieR/J/A+A/619/A161doi:10.26093/cds/vizier.36190161CDSCazzoletti P.van Dishoeck E. F.Pinilla P.Tazzari M.Facchini S.,van der Marel N.Benisty M.Garufi A.Perez L.2019-02-21T05:41:49Z2018-11-23T09:17:26ZCDS support team

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

cds-question@unistra.fryoung-stellar-objectsmultiple-starsmillimeter-astronomysubmillimeter-astronomySpiral arms, rings and large scale asymmetries are structures observed in high resolution observations of protoplanetary disks, and it appears that some of the disks showing spiral arms in scattered light also show asymmetries in millimeter-sized dust. HD 135344B is one of these disks. Planets are invoked as the origin of these structures, but no planet has been observed so far and up per limits are becoming more stringent with time. We want to investigate the nature of the asymmetric structure in the HD 135344B disk in order to understand the origin of the spirals and of the asymmetry seen in this disk. Ultimately, we aim at understanding whether or not one or more planets are needed to explain such structures. We present new ALMA sub-0.1" resolution observations at optically thin wavelengths (lambda=2.8mm and 1.9mm) of the HD 135344B disk. The high spatial resolution allows us to unambiguously characterize the mm-dust morphology of the disk. The low optical depth of continuum emission probes the bulk of the dust content of the vortex. Moreover, we combine the new observations with archival data at shorter wavelengths to perform a multi-wavelength analysis and to obtain information about the dust distribution and properties inside the observed asymmetry. We resolve the asymmetric disk into a symmetric ring + asymmetric crescent, and observe that: (1) the spectral index strongly decreases at the center of the vortex, consistent with the presence of large grains; (2) for the first time, an azimuthal shift of the peak of the vortex with wavelength is observed; (3) the azimuthal width of the vortex decreases at longer wavelengths, as expected for dust traps. These features allow to confirm the nature of the asymmetry as a vortex. Finally, under the assumption of optically thin emission, a lower limit to the total mass of the vortex is 0.3M_Jupiter_. Considering the uncertainties involved in this estimate, it is possible that the actual mass of the vortex is higher and possibly within the required values (~4M_Jupiter_) to launch spiral arms similar to those observed in scattered light. If this is the case, no outer planet is needed to explain the morphology.2018A&A...619A.161Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/619/A161CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/619/A161https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/619/A161http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/619/A161https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/619/A161https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/619/A161http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/619/A161GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/619/A161/list (List of fits images)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/619/A161/list?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/619/A161/list?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/619/A161/list?GETtext/xml+votable180.050000true228.95175-37.15460.005555555555555556Associated datahttps://cdsarc.cds.unistra.fr/assocdata/?obs_collection=J/A+A/619/A1616/44049https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/619/A161?format=asciiMillimeterdefaultJ/A+A/619/A161/listList of fits imagesrecnoRecord 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.dateObvervation date (YYYY/MM/DDThh:mm:ss.ssssss)stime.epochnullableFreqObserved frequencyGHzem.freqfloatsizeSize of FITS fileKibytephys.size;meta.fitsintFileNameName of FITS file, in subdirectory imagemeta.id;meta.fitscharTitleTitle of the FITS filemeta.title;meta.fitschar