TY - JOUR
T1 - exoALMA. I. Science goals, project design, and data products
AU - Teague, Richard
AU - Benisty, Myriam
AU - Facchini, Stefano
AU - Fukagawa, Misato
AU - Pinte, Christophe
AU - Andrews, Sean M.
AU - Bae, Jaehan
AU - Barraza-Alfaro, Marcelo
AU - Cataldi, Gianni
AU - Cuello, Nicolás
AU - Curone, Pietro
AU - Czekala, Ian
AU - Fasano, Daniele
AU - Flock, Mario
AU - Galloway-Sprietsma, Maria
AU - Garg, Himanshi
AU - Hall, Cassandra
AU - Hammond, Iain
AU - Hilder, Thomas
AU - Huang, Jane
AU - Ilee, John D.
AU - Izquierdo, Andrés F.
AU - Kanagawa, Kazuhiro
AU - Lesur, Geoffroy
AU - Lodato, Giuseppe
AU - Longarini, Cristiano
AU - Loomis, Ryan A.
AU - Masset, Frédéric
AU - Menard, Francois
AU - Orihara, Ryuta
AU - Price, Daniel J.
AU - Rosotti, Giovanni
AU - Stadler, Jochen
AU - Testi, Leonardo
AU - Yen, Hsi-Wei
AU - Wafflard-Fernandez, Gaylor
AU - Wilner, David J.
AU - Winter, Andrew J.
AU - Wölfer, Lisa
AU - Yoshida, Tomohiro C.
AU - Zawadzki, Brianna
N1 - Funding: J.B. acknowledges support from NASA XRP grant No. 80NSSC23K1312. M.B., D.F., and J.S. 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). P.C. and L.T. acknowledge 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. 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). S.F. is funded by the European Union (ERC, UNVEIL, 101076613), and acknowledges financial contribution from PRIN-MUR 2022YP5ACE. 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. I.H., C.H., and T.H. are supported by an Australian Government Research Training Program (RTP) Scholarship. J.D.I. acknowledges support from an STFC Ernest Rutherford Fellowship (ST/W004119/1) and a University Academic Fellowship from the University of Leeds. Support for AFI 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 Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS). C.L. has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 823823 (DUSTBUSTERS) and by 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). H.-W.Y. acknowledges support from 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. T.C.Y. acknowledges support by Grant-in-Aid for JSPS Fellows JP23KJ1008. Support for B.Z. was provided by The Brinson Foundation. This work was partly supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation)—Ref No. 325594231 FOR 2634/2 TE 1024/2-1, and by the DFG Cluster of Excellence Origins (https://www.origins-cluster.de/). This project has received funding from the European Research Council (ERC) via the ERC Synergy Grant ECOGAL (grant 855130).
PY - 2025/5/1
Y1 - 2025/5/1
N2 - Planet formation is a hugely dynamic process requiring the transport, concentration, and assimilation of gas and dust to form the first planetesimals and cores. With access to observations with extremely high spatial and spectral resolution at unprecedented sensitivities, it is now possible to probe the planet-forming environment in detail. To this end, the exoALMA Large Program targeted 15 large protoplanetary disks, ranging between ∼1″ and ∼7″ in radius, and mapped the gas and dust distributions. 12CO J = 3–2, 13CO J = 3–2, and CS J = 7–6 molecular emission was imaged at high angular (∼0.″15) and spectral (∼100 m s−1) resolution, achieving a surface brightness temperature sensitivity of ∼1.5 K over a single channel, while the 330 GHz continuum emission was imaged at 90 mas resolution and achieved a point source sensitivity of ∼40 μJy beam−1. These observations constitute some of the deepest observations of protoplanetary disks to date. Extensive substructure was found in all but one disk, traced by both dust continuum and molecular line emission. In addition, the molecular emission allowed for the velocity structure of the disks to be mapped with excellent precision (uncertainties of the order of 10 m s−1), revealing a variety of kinematic perturbations across all sources. From this sample it is clear that, when observed in detail, all disks appear to exhibit physical and dynamical substructure indicative of ongoing dynamical processing due to young, embedded planets, large-scale (magneto)hydrodynamical instabilities or winds.
AB - Planet formation is a hugely dynamic process requiring the transport, concentration, and assimilation of gas and dust to form the first planetesimals and cores. With access to observations with extremely high spatial and spectral resolution at unprecedented sensitivities, it is now possible to probe the planet-forming environment in detail. To this end, the exoALMA Large Program targeted 15 large protoplanetary disks, ranging between ∼1″ and ∼7″ in radius, and mapped the gas and dust distributions. 12CO J = 3–2, 13CO J = 3–2, and CS J = 7–6 molecular emission was imaged at high angular (∼0.″15) and spectral (∼100 m s−1) resolution, achieving a surface brightness temperature sensitivity of ∼1.5 K over a single channel, while the 330 GHz continuum emission was imaged at 90 mas resolution and achieved a point source sensitivity of ∼40 μJy beam−1. These observations constitute some of the deepest observations of protoplanetary disks to date. Extensive substructure was found in all but one disk, traced by both dust continuum and molecular line emission. In addition, the molecular emission allowed for the velocity structure of the disks to be mapped with excellent precision (uncertainties of the order of 10 m s−1), revealing a variety of kinematic perturbations across all sources. From this sample it is clear that, when observed in detail, all disks appear to exhibit physical and dynamical substructure indicative of ongoing dynamical processing due to young, embedded planets, large-scale (magneto)hydrodynamical instabilities or winds.
KW - Protoplanetary disks
UR - https://www.scopus.com/pages/publications/105003937648
U2 - 10.3847/2041-8213/adc43b
DO - 10.3847/2041-8213/adc43b
M3 - Article
AN - SCOPUS:105003937648
SN - 2041-8205
VL - 984
JO - Astrophysical Journal Letters
JF - Astrophysical Journal Letters
IS - 1
M1 - L6
ER -