dc.contributor.author Cazzoletti, P dc.contributor.author Van Dishoeck, EF dc.contributor.author Pinilla, P dc.contributor.author Tazzari, M dc.contributor.author Facchini, S dc.contributor.author Van Der Marel, N dc.contributor.author Benisty, M dc.contributor.author Garufi, A dc.contributor.author Pérez, LM dc.date.accessioned 2018-12-12T00:30:50Z dc.date.available 2018-12-12T00:30:50Z dc.date.issued 2018 dc.identifier.issn 0004-6361 dc.identifier.uri https://www.repository.cam.ac.uk/handle/1810/286694 dc.description.abstract Spiral 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. We 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 in Band 3 and 4. The high spatial resolution allows us to characterize the mm-dust morphology of the disk. The low optical depth of continuum emission probes the bulk of the dust in vortex. Moreover, we combine the new observations with archival data to perform a multi-wavelength analysis and to obtain information about the dust distribution and properties inside the 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 a lower limit to the total mass of the vortex is $0.3 M_{\rm Jupiter}$. 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 ($\sim 4\,\rm M_{\rm Jupiter}$) to launch spiral arms similar to those observed in scattered light. dc.description.sponsorship P.P. acknowledges support by NASA through Hubble Fellowship grant HST-HF2-51380.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. M.B. acknowledges funding from ANR of France under contract number ANR-16-CE31-0013 (Planet Forming disks). M.T. has been supported by the DISCSIM project, grant agreement 341137 funded by the European Research Council under ERC-2013-ADG. Astrochemistry in Leiden is supported by the European Union A-ERC grant 291141 CHEMPLAN, by the Netherlands Research School for Astronomy (NOVA), and by a Royal Netherlands Academy of Arts and Sciences (KNAW) professor prize. dc.publisher EDP Sciences dc.subject protoplanetary disks dc.subject planet-disk interactions dc.subject stars: individual: HD 135344B dc.subject planets and satellites: formation dc.subject instabilities dc.title Evidence for a massive dust-trapping vortex connected to spirals: Multi-wavelength analysis of the HD 135344B protoplanetary disk dc.type Article prism.publicationDate 2018 prism.publicationName Astronomy and Astrophysics prism.volume 619 dc.identifier.doi 10.17863/CAM.34001 dcterms.dateAccepted 2018-09-11 rioxxterms.versionofrecord 10.1051/0004-6361/201834006 rioxxterms.version AM rioxxterms.licenseref.uri http://www.rioxx.net/licenses/all-rights-reserved rioxxterms.licenseref.startdate 2018-11-01 dc.contributor.orcid Tazzari, Marco [0000-0003-3590-5814] dc.identifier.eissn 1432-0746 dc.publisher.url http://dx.doi.org/10.1051/0004-6361/201834006 rioxxterms.type Journal Article/Review pubs.funder-project-id European Research Council (341137) cam.issuedOnline 2018-11-21
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