The DSHARP survey evidenced the ubiquity of substructure in the mm dust distribution of large, bright protoplanetary discs. Intriguingly, these data sets have yet higher resolution information that is not recovered in a CLEAN image. We first show that the intrinsic performance of the CLEAN algorithm is resolution-limited. Then analysing all 20 DSHARP sources using the 1D, super-resolution code FRANKenstein (FRANK), we accurately fit the 1D visibilities to a mean factor of 4.3 longer baseline than the Fourier transform of the CLEAN images and a factor of 3.0 longer baseline than the transform of the CLEAN component models. This yields a higher resolution brightness profile for each source, identifying new substructure interior to 30 au in multiple discs; resolving known gaps to be deeper, wider, and more structured; and known rings to be narrower and brighter. Across the survey, high contrast gaps are an average wider and deeper in the FRANK profiles relative to CLEAN, and high contrast rings are an average narrower. Categorizing the FRANK brightness profiles into trends, we find that the relative scarcity of features interior to 30 au in the survey's CLEAN images is an artefact of resolving power, rather than an intrinsic rarity of inner disc (or compact disc) substructure. Finally the rings in the FRANK profiles are narrower than the previously inferred deconvolved widths, indicating smaller alpha/St ratios in the local gas disc.

A super-resolution analysis of the DSHARP survey: Substructure is common in the inner 30 au / J. Jennings, R. A Booth, M. Tazzari, C. J Clarke, G.P. Rosotti. - In: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY. - ISSN 0035-8711. - 509:2(2022 Jan), pp. 2780-2799. [10.1093/mnras/stab3185]

A super-resolution analysis of the DSHARP survey: Substructure is common in the inner 30 au

G.P. Rosotti
Ultimo
2022

Abstract

The DSHARP survey evidenced the ubiquity of substructure in the mm dust distribution of large, bright protoplanetary discs. Intriguingly, these data sets have yet higher resolution information that is not recovered in a CLEAN image. We first show that the intrinsic performance of the CLEAN algorithm is resolution-limited. Then analysing all 20 DSHARP sources using the 1D, super-resolution code FRANKenstein (FRANK), we accurately fit the 1D visibilities to a mean factor of 4.3 longer baseline than the Fourier transform of the CLEAN images and a factor of 3.0 longer baseline than the transform of the CLEAN component models. This yields a higher resolution brightness profile for each source, identifying new substructure interior to 30 au in multiple discs; resolving known gaps to be deeper, wider, and more structured; and known rings to be narrower and brighter. Across the survey, high contrast gaps are an average wider and deeper in the FRANK profiles relative to CLEAN, and high contrast rings are an average narrower. Categorizing the FRANK brightness profiles into trends, we find that the relative scarcity of features interior to 30 au in the survey's CLEAN images is an artefact of resolving power, rather than an intrinsic rarity of inner disc (or compact disc) substructure. Finally the rings in the FRANK profiles are narrower than the previously inferred deconvolved widths, indicating smaller alpha/St ratios in the local gas disc.
methods: data analysis; techniques: interferometric; radio continuum: planetary systems; submillimetre: general; submillimetre: planetary systems
Settore FIS/05 - Astronomia e Astrofisica
   Dust and gas in planet forming discs (DUSTBUSTER)
   DUSTBUSTER
   EUROPEAN COMMISSION
   H2020
   823823
gen-2022
3-nov-2021
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2434/952813
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