Avenhaus, H.Quanz, S.P.Garufi, A.Perez, S.Casassus, S.Pinte, C.Bertrang, G.H.-M.Caceres, C.Benisty, M.Dominik, C.2019-11-282019-11-282018-08Astrophysical Journal, 863(1), art. no. 44.0004-637XDOI: 10.3847/1538-4357/aab846http://repositorio.unab.cl/xmlui/handle/ria/10882Indexación: Scopus.SPHERE is an instrument designed and built by a consortium consisting of IPAG (Grenoble, France), MPIA (Heidelberg, Germany), LAM (Marseille, France), LESIA (Paris, France), Laboratoire Lagrange (Nice, France), INAF– Osservatorio di Padova (Italy), Observatoire de Gen‘eve (Switzerland), ETH Zurich (Switzerland), NOVA (Netherlands), ONERA (France), and ASTRON (Netherlands), in collaboration with ESO. SPHERE also received funding from the European Commission Sixth and Seventh Framework Programmes as part of the Optical Infrared Coordination Network for Astronomy (OPTICON) under grant number RII3-Ct-2004-001566 for FP6 (20042008), grant number 226604 for FP7 (20092012), and grant number 312430 for FP7 (20132016).HA acknowledges support from the Millennium Science Initiative (Chilean Ministry of Economy) through grant RC130007 and further financial support by FONDECYT, grant 3150643. Part of this work has been carried out within the framework of the National Centre for Competence in Research PlanetS, supported by the Swiss National Science Foundation. HA, SPQ, and HMS acknowledge the financial support of the SNSF. GH-MB acknowledges financial support from CON-ICYT through FONDECYT grant 3170657. CC acknowledges support from project CONICYT PAI/Concurso Nacional Insercion en la Academia, convocatoria 2015, folio 79150049, and financial support from ICM Nucleo Milenio de Formacion Planetaria, NPF. MB acknowledges funding from ANR of France under contract number ANR-16-CE31-0013 (Planet Forming Disks). CP acknowledges funding from the Australian Research Council (ARC) under Future Fellowship number FT170100040. SC and SP acknowledge financial support from CONICYT FONDECYT grant 1171624. Financial support was provided by Millennium Nucleus RC130007 (Chilean Ministry of Economy). SP acknowledges CONICYT-Gemini grant 32130007.This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has furthermore made use of data from the European Space Agency (ESA) mission Gaia (http://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC; http://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.We present the first part of our Disks ARound T Tauri Stars with SPHERE (DARTTS-S) survey: observations of eight T Tauri stars that were selected based on their strong (sub)millimeter excesses using SPHERE/IRDIS polarimetric differential imaging in the J and H bands. All observations successfully detect the disks, which appear vastly different in size, from ≈80 au in scattered light to >400 au, and display total polarized disk fluxes between 0.06% and 0.89% of the stellar flux. For five of these disks, we are able to determine the three-dimensional structure and the flaring of the disk surface, which appears to be relatively consistent across the different disks, with flaring exponents α between ≈1.1 and ≈1.6. We also confirm literature results with regard to the inclination and position angle of several of our disks and are able to determine which side is the near side of the disk in most cases. While there is a clear trend of disk mass with stellar ages (≈1 to >10 Myr), no correlations of disk structures with age were found. There are also no correlations with either stellar mass or submillimeter flux. We do not detect significant differences between the J and H bands. However, we note that while a high fraction (7/8) of the disks in our sample show ring-shaped substructures, none of them display spirals, in contrast to the disks around more massive Herbig Ae/Be stars, where spiral features are common. © 2018. The American Astronomical Society. All rights reserved.enDisk interactionsPlanetProtoplanetary disksStars: formationStars: pre-main sequenceArtículo