Volume 625, May 2019
|Number of page(s)||32|
|Section||Catalogs and data|
|Published online||14 May 2019|
Consistent dust and gas models for protoplanetary disks
IV. A panchromatic view of protoplanetary disks⋆
Department of Astrophysics, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
2 SUPA School of Physics & Astronomy, University of St. Andrews, North Haugh, KY16 9SS St. Andrews, UK
3 Centre for Exoplanet Science, University of St. Andrews, St. Andrews, UK
4 Instituut voor Sterrenkunde, K.U. Leuven, Celestijnenlaan 200D, 3001 Leuven, Belgium
5 Univ. Grenoble Alpes, CNRS, IPAG, 38000 Grenoble, France
6 Kapteyn Astronomical Institute, University of Groningen, Postbus 800, 9700 AV Groningen, The Netherlands
7 Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, University Road, Belfast BT7 1NN, UK
8 IRAP, Université de Toulouse, CNRS, UPS, Toulouse, France
9 Astronomical institute Anton Pannekoek, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands
10 School of Physics and Astronomy, Cardiff University, 4 The Parade, Cardiff CF24 3AA, UK
11 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
12 SRON Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands
13 UMI-FCA, CNRS/INSU France (UMI 3386), and Departamento de Astronomica, Universidad de Chile, Santiago, Chile
14 Monash Centre for Astrophysics (MoCA) and School of Physics and Astronomy, Monash University, Clayton, VIC 3800, Australia
15 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany
Accepted: 22 February 2019
Context. Consistent modeling of protoplanetary disks requires the simultaneous solution of both continuum and line radiative transfer, heating and cooling balance between dust and gas and, of course, chemistry. Such models depend on panchromatic observations that can provide a complete description of the physical and chemical properties and energy balance of protoplanetary systems. Along these lines, we present a homogeneous, panchromatic collection of data on a sample of 85 T Tauri and Herbig Ae objects for which data cover a range from X-rays to centimeter wavelengths. Datasets consist of photometric measurements, spectra, along with results from the data analysis such as line fluxes from atomic and molecular transitions. Additional properties resulting from modeling of the sources such as disk mass and shape parameters, dust size, and polycyclic aromatic hydrocarbon (PAH) properties are also provided for completeness.
Aim. The purpose of this data collection is to provide a solid base that can enable consistent modeling of the properties of protoplanetary disks. To this end, we performed an unbiased collection of publicly available data that were combined to homogeneous datasets adopting consistent criteria. Targets were selected based on both their properties and the availability of data.
Methods. Data from more than 50 different telescopes and facilities were retrieved and combined in homogeneous datasets directly from public data archives or after being extracted from more than 100 published articles. X-ray data for a subset of 56 sources represent an exception as they were reduced from scratch and are presented here for the first time.
Results. Compiled datasets, along with a subset of continuum and emission-line models are stored in a dedicated database and distributed through a publicly accessible online system. All datasets contain metadata descriptors that allow us to track them back to their original resources. The graphical user interface of the online system allows the user to visually inspect individual objects but also compare between datasets and models. It also offers to the user the possibility to download any of the stored data and metadata for further processing.
Key words: stars: formation / circumstellar matter / stars: variables: T Tauri / Herbig Ae/Be / accretion / accretion disks / astronomical databases: miscellaneous
A copy of the X-ray data is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/625/A66
© ESO 2019
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