A super-resolution analysis of the DSHARP survey: Substructure is common in the inner 30 au
Jeff Jennings, Richard A. Booth, Marco Tazzari, Cathie J. Clarke, Giovanni P. Rosotti
备注：
Revised version, accepted to MNRAS. Changes: added CLEAN .model profiles to Sec.3 and 4, quantified gaps/rings in frank profiles in Sec.5 and Table 3, expanded analysis of alpha/St in Sec.5.3.1. All frank fits are now available at https://zenodo.org/record/5587841
The DSHARP survey evidenced the ubiquity of substructure in the mm dust distribution of large, bright protoplanetary discs. Intriguingly, these datasets 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 analyzing 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 14% wider and 44% deeper in the frank profiles relative to CLEAN, and high contrast rings are an average 26% 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 artifact 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.
The Disk Substructures at High Angular Resolution Project (DSHARP) VI: Dust trapping in thin-ringed protoplanetary disks
ALMA观测到的大部分原行星盘在连续体中显示出多个定义明确且近乎完美的圆环，在许多情况下具有显著的峰谷对比度。DSHARP活动表明，这些环中有几个在径向范围内非常狭窄。在本文中，我们测试的假设，这些尘埃环是由尘埃捕获在径向压力颠簸，如果得到证实，把约束的物理尘埃捕获机制。我们在1D模型分析这个过程，假设轴对称。通过与观测数据的比较，我们发现所有的星环都与尘埃捕获相一致。基于一个合理的尘埃温度模型，我们发现几个环比压力标度的高度更窄，为尘埃捕获提供了强有力的证据。环具有在0.2和0.5之间的范围内的峰值吸收光学深度。储存在每个环中的尘埃质量大约是地球质量的几十倍，尽管由于尘埃不透明度的不确定性，仍然存在许多模糊性。尘埃环的密度足以潜在地触发流动的不稳定性，但我们的分析无法证明这种机制实际上在起作用。然而，我们的结果表明，本文所< 5e-4 and very large grains a_grain >研究的所有环的数据都可以排除非常低的α_turb < > 0.1 cm的组合。
The Disk Substructures at High Angular Resolution Project (DSHARP): X. Multiple rings, a misaligned inner disk, and a bright arc in the disk around the T Tauri star HD 143006
The Disk Substructures at High Angular Resolution Project (DSHARP): III. Spiral Structures in the Millimeter Continuum of the Elias 27, IM Lup, and WaOph 6 Disks
Axisymmetric Modeling of DSHARP Dusty Disks: Asymmetric Structures and Inner-Disk Dispersal
College of Science, Ibaraki University（茨城大学理学部）；Tsung-Dao Lee Institute, Shanghai Jiao Tong University（上海交通大学李政道研究所）；RIKEN Cluster for Pioneering Research（理化学院先锋研究集群）；Division of Liberal Arts, Kogakuin University（工学院大学人文学部）；National Astronomical Observatory of Japan（日本国立天文台）
The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): Constraints on disk turbulence, fragmentation velocity, and inner pebble fluxes
University College London（伦敦大学学院）；Universidad de Chile（智利大学）；European Southern Observatory（欧洲南方天文台）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理研究所）；Max-Planck-Institut fur Astronomie (MPIA)（马克斯·普朗克天文学研究所）；Universidad Técnica Federico Santa María（费德里科·圣玛丽亚技术大学）；Università degli Studi di Milano（米兰大学）
The ALMA survey to Resolve exoKuiper belt Substructures (ARKS). X. Interpreting the peculiar dust rings around HD 131835
Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences（孔科利天文台，匈牙利研究与创新学院天文学与地球科学研究中心）；Millennium Nucleus on Young Exoplanets and their Moons (YEMS)（年轻系外行星及其卫星千年核心）；Center for Interdisciplinary Research in Astrophysics Space Exploration (CIRAS), Universidad de Santiago, Chile（智利圣地亚哥大学跨学科天体物理空间探索研究中心）；Departamento de Astrofísica, Universidad de La Laguna, La Laguna, E-38200, Tenerife, Spain（拉帕尔马大学天体物理系）；Institute of Physics and Astronomy, ELTE Eötvös Loránd University, Pázmány Péter sétány 1/A, 1117 Budapest, Hungary（罗兰大学物理与天文学研究所）；Max-Planck-Insitut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany（马克斯·普朗克天文学研究所）；Institute of Physics Belgrade, University of Belgrade, Pregrevica 118, 11080 Belgrade, Serbia（贝尔格莱德大学物理研究所）；Institut für Astrophysik, Universität Wien, Türkensch（维也纳大学天体物理研究所）
Multi-frequency analysis of the ALMA and VLA high resolution continuum observations of the substructured disc around CI Tau. Preference for sub-mm-sized low-porosity amorphous carbon grains
The Ophiuchus DIsk Survey Employing ALMA (ODISEA): A Unified Evolutionary Sequence of Planet-Driven Substructures Explaining the Diversity of Disk Morphologies
