TY - JOUR
T1 - exoALMA. IV. Substructures, asymmetries, and the faint outer disk in continuum emission
AU - Curone, Pietro
AU - Facchini, Stefano
AU - Andrews, Sean M.
AU - Testi, Leonardo
AU - Benisty, Myriam
AU - Czekala, Ian
AU - Huang, Jane
AU - Ilee, John D.
AU - Isella, Andrea
AU - Lodato, Giuseppe
AU - Loomis, Ryan A.
AU - Stadler, Jochen
AU - Winter, Andrew J.
AU - Bae, Jaehan
AU - Barraza-Alfaro, Marcelo
AU - Cataldi, Gianni
AU - Cuello, Nicolás
AU - Fasano, Daniele
AU - Flock, Mario
AU - Fukagawa, Misato
AU - Galloway-Sprietsma, Maria
AU - Garg, Himanshi
AU - Hall, Cassandra
AU - Izquierdo, Andrés F.
AU - Kanagawa, Kazuhiro
AU - Lesur, Geoffroy
AU - Longarini, Cristiano
AU - Menard, Francois
AU - Orihara, Ryuta
AU - Pinte, Christophe
AU - Price, Daniel J.
AU - Rosotti, Giovanni
AU - Teague, Richard
AU - Wafflard-Fernandez, Gaylor
AU - Wilner, David J.
AU - Wölfer, Lisa
AU - Yen, Hsi-Wei
AU - Yoshida, Tomohiro C.
AU - Zawadzki, Brianna
N1 - Funding: P.C. acknowledges support by the Italian Ministero dell’Istruzione, Università e Ricerca through the grant Progetti Premiali 2012-iALMA (CUP C52I13000140001) and by the ANID BASAL project FB210003. S.F. is funded by the European Union (ERC, UNVEIL, 101076613), and acknowledges financial contribution from PRIN-MUR 2022YP5ACE. J.B. acknowledges support from NASA XRP grant No. 80NSSC23K1312. M.B., D.F., J.S, and A.W. have received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (PROTOPLANETS, grant agreement No. 101002188). M.F. has received funding from the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (grant agreement No. 757957). M.F. is supported by a grant-in-aid from the Japan Society for the Promotion of Science (KAKENHI: No. JP22H01274). C.H. acknowledges support from NSF AAG grant No. 2407679. J.D.I. acknowledges support from an STFC Ernest Rutherford Fellowship (ST/W004119/1) and a University Academic Fellowship from the University of Leeds. A.I. acknowledges support from the National Aeronautics and Space Administration under grant No. 80NSSC18K0828. Support for A.F.I. was provided by NASA through the NASA Hubble Fellowship grant No. HST-HF2-51532.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. G.L. has received funding from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (Grant agreement no. 815559 (MHDiscs)). G.L. and C.L. have received funding from the European Union's Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS). C.L. acknowledges support from the UK Science and Technology Research Council (STFC) via the consolidated grant ST/W000997/1. C.P. acknowledges Australian Research Council funding via FT170100040, DP18010423, DP220103767, and DP240103290. D.P. acknowledges Australian Research Council funding via DP18010423, DP220103767, and DP240103290. G.R. acknowledges funding from the Fondazione Cariplo, grant No. 2022-1217, and the European Research Council (ERC) under the European Union’s Horizon Europe Research & Innovation Programme under grant agreement No. 101039651 (DiscEvol). F.M. received funding from the European Research Council (ERC) under the European Union’s Horizon Europe research and innovation program (grant agreement No. 101053020, project Dust2Planets). N.C. has received funding from the European Research Council (ERC) under the European Union Horizon Europe research and innovation program (grant agreement No. 101042275, project Stellar-MADE). L.T. acknowledges funding from Progetti Premiali 2012 iALMA (CUP C52I13000140001), Deutsche Forschungs-gemeinschaft (German Research Foundation) reference No. 325594231 FOR 2634/1 TE 1024/1-1, European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant No. 823823 (DUSTBUSTERS), and the ERC via the ERC Synergy grant ECOGAL (grant No. 855130). T.C.Y. acknowledges support by Grant-in-Aid for JSPS Fellows JP23KJ1008. H.-W.Y. acknowledges support from the National Science and Technology Council (NSTC) in Taiwan through grant NSTC 113-2112-M-001-035- and from the Academia Sinica Career Development Award (AS-CDA-111-M03). G.W.F. acknowledges support from the European Research Council (ERC) under the European Union Horizon 2020 research and innovation program (grant agreement No. 815559 (MHDiscs)). G.W.F. was granted access to the HPC resources of IDRIS under the allocation A0120402231 made by GENCI. Support for B.Z. was provided by The Brinson Foundation.
PY - 2025/5/1
Y1 - 2025/5/1
N2 - The exoALMA Large Program targeted a sample of 15 disks to study gas dynamics within these systems, and these observations simultaneously produced continuum data at 0.9 mm (331.6 GHz) with exceptional surface brightness sensitivity at high angular resolution. To provide a robust characterization of the observed substructures, we performed a visibility space analysis of the continuum emission from the exoALMA data, characterizing axisymmetric substructures and nonaxisymmetric residuals obtained by subtracting an axisymmetric model from the observed data. We defined a nonaxisymmetry index and found that the most asymmetric disks predominantly show an inner cavity and consistently present higher values of mass accretion rate and near-infrared excess. This suggests a connection between outer disk dust substructures and inner disk properties. The depth of the data allowed us to describe the azimuthally averaged continuum emission in the outer disk, revealing that larger disks (both in dust and gas) in our sample tend to be gradually tapered compared to the sharper outer edge of more compact sources. Additionally, the data quality revealed peculiar features in various sources, such as shadows, inner disk offsets, tentative external substructures, and a possible dust cavity wall.
AB - The exoALMA Large Program targeted a sample of 15 disks to study gas dynamics within these systems, and these observations simultaneously produced continuum data at 0.9 mm (331.6 GHz) with exceptional surface brightness sensitivity at high angular resolution. To provide a robust characterization of the observed substructures, we performed a visibility space analysis of the continuum emission from the exoALMA data, characterizing axisymmetric substructures and nonaxisymmetric residuals obtained by subtracting an axisymmetric model from the observed data. We defined a nonaxisymmetry index and found that the most asymmetric disks predominantly show an inner cavity and consistently present higher values of mass accretion rate and near-infrared excess. This suggests a connection between outer disk dust substructures and inner disk properties. The depth of the data allowed us to describe the azimuthally averaged continuum emission in the outer disk, revealing that larger disks (both in dust and gas) in our sample tend to be gradually tapered compared to the sharper outer edge of more compact sources. Additionally, the data quality revealed peculiar features in various sources, such as shadows, inner disk offsets, tentative external substructures, and a possible dust cavity wall.
KW - Protoplanetary disks
KW - Dust continuum emission
KW - Planet formation
KW - Radio interferometry
U2 - 10.3847/2041-8213/adc438
DO - 10.3847/2041-8213/adc438
M3 - Article
SN - 2041-8205
VL - 984
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L9
ER -