Abstract

Contributed Talk - Splinter PlanetFormation

The MATISSE view of the inner region of the RY Tau protoplanetary disk

J. S. Martin1 , J. Kobus1 , J. Varga2 , A. Matter3 , S. Wolf1 , M. Abello3 , F. Allouche3 , J.-C. Augereau4 , P. Berio3 , F. Bettonvil5 , R. van Boekel6 , P. A. Boley6 , P. Cruzalèbes3 , W. C. Danchi7 , J. Drevon3 , C. Dominik8 , V. Fleury3 , V. Gámez Rosas9 , A. Glindemann9 , L. N. A. van Haastere11 , M. Heininger10 , Th. Henning6 , K.-H. Hofmann10 , M. Hogerheijde8, 11 , M. Houllé3 , J. W. Isbell12 , W. Jaffe11 , L. Labadie13 , S. Lagarde3 , J. H. Leftley14 , M. Lehmitz6 , M. Letessier4 , B. Lopez3 , F. Lykou2 , J. Ma4 , A. Meilland3 , F. Millour3 , C. Paladini15 , E. Pantin16 , R. G. Petrov3 , P. Priolet4 , S. Robbe-Dubois3 , D. Schertl9 , M. Scheuck6 , J. Scigliuto3 , G. Weigelt10 , J. Woillez9 , and MATISSE Collaboration
1 Institut für Theoretische Physik und Astrophysik, Christian-Albrechts-Universität zu Kiel, Leibnizstraße 15, 24118 Kiel, Germany; 2 Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, HUN-REN, Konkoly Thege Miklós út 15-17., H-1121 Budapest, Hungary; 3 Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Boulevard de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France; 4 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France; 5 NOVA Optical IR Instrumentation Group at ASTRON, The Netherlands; 6 Max-Planck-Institut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany; 7 NASA Goddard Space Flight Center, Astrophysics Division, Greenbelt, MD, 20771, USA 8 Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1090 GE Amsterdam, The Netherlands; 9 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany; 10 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany; 11 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlands; 12 Steward Observatory, Department of Astronomy, University of Arizona, Tucson, AZ 85721, USA; 13 Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, Cologne, 50937, Germany; 14 School of Physics & Astronomy, University of Southampton, University Road, Southampton SO17 1BJ, UK; 15 European Southern Observatory, Alonso de Córdova, 3107 Vitacura, Santiago, Chile; 16 AIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, F-91191 Gif-sur-Yvette, France

The T-Tauri type young stellar object RY Tau exhibits a dust depleted inner cavity characteristic of a transition disk. We constrain the spatial distribution and mineralogy of dust in the RY Tau protoplanetary disk in the inner few astronomical units using spectrally resolved interferometric observations in the L, M, and N bands obtained with VLTI/MATISSE. Employing a 2D temperature gradient model we estimate the orientation of the inner disk finding no evidence of significant misalignment between the inner and outer disk of RY Tau. Successively, we analyze the chemical composition of silicates depending on spatial region in the disk and identify several silicate species commonly found in protoplanetary disks. Additionally, a depletion of amorphous dust grains toward the central protostar is observed. Monte Carlo radiative transfer simulations show that hot dust close to the protostar and in the line of sight to the observer, either in the uppermost disk layers of a strongly flared disk or in a dusty envelope, is necessary to model the observations. The shadow cast by a dense innermost disk midplane on the dust further out explains the observed closure phases in the L band and to some extent in the M band. However, the closure phases in the N band are underestimated by our model, hinting at an additional asymmetry in the flux density distribution not visible at shorter wavelengths.