The potential of combining MATISSE and ALMA observations: Constraining the structure of the innermost region in protoplanetary discs
arXiv:1901.04342 · doi:10.1051/0004-6361/201833784
Abstract
In order to study the initial conditions of planet formation, it is crucial to obtain spatially resolved multi-wavelength observations of the innermost region of protoplanetary discs. We evaluate the advantage of combining observations with MATISSE/VLTI and ALMA to constrain the radial and vertical structure of the dust in the innermost region of circumstellar discs in nearby star-forming regions. Based on a disc model with a parameterized dust density distribution, we apply 3D radiative-transfer simulations to obtain ideal intensity maps. These are used to derive the corresponding wavelength-dependent visibilities we would obtain with MATISSE as well as ALMA maps simulated with CASA. Within the considered parameter space, we find that constraining the dust density structure in the innermost au around the central star is challenging with MATISSE alone, whereas ALMA observations with reasonable integration times allow us to derive significant constraints on the disc surface density. However, we find that the estimation of the different disc parameters can be considerably improved by combining MATISSE and ALMA observations. For example, combining a 30-minute ALMA observation (at 310 GHz with an angular resolution of 0.03) for MATISSE observations in the L and M bands (with visibility accuracies of about ) allows the radial density slope and the dust surface density profile to be constrained to within and , respectively. For an accuracy of even the disc flaring can be constrained to within . To constrain the scale height to within au, M band accuracies of are required. While ALMA is sensitive to the number of large dust grains settled to the disc midplane we find that the impact of the surface density distribution of the large grains on the observed quantities is small.
arXiv comment12 pages, 12 figures, 1 table, accepted by A&A
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