exoALMA. I. Science Goals, Project Design, and Data Products
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...
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2025-01-01
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| author | Richard Teague Myriam Benisty Stefano Facchini Misato Fukagawa Christophe Pinte Sean M. Andrews Jaehan Bae Marcelo Barraza-Alfaro Gianni Cataldi Nicolás Cuello Pietro Curone Ian Czekala Daniele Fasano Mario Flock Maria Galloway-Sprietsma Himanshi Garg Cassandra Hall Iain Hammond Thomas Hilder Jane Huang John D. Ilee Andrés F. Izquierdo Kazuhiro Kanagawa Geoffroy Lesur Giuseppe Lodato Cristiano Longarini Ryan A. Loomis Frédéric Masset Francois Menard Ryuta Orihara Daniel J. Price Giovanni Rosotti Jochen Stadler Leonardo Testi Hsi-Wei Yen Gaylor Wafflard-Fernandez David J. Wilner Andrew J. Winter Lisa Wölfer Tomohiro C. Yoshida Brianna Zawadzki |
| author_facet | Richard Teague Myriam Benisty Stefano Facchini Misato Fukagawa Christophe Pinte Sean M. Andrews Jaehan Bae Marcelo Barraza-Alfaro Gianni Cataldi Nicolás Cuello Pietro Curone Ian Czekala Daniele Fasano Mario Flock Maria Galloway-Sprietsma Himanshi Garg Cassandra Hall Iain Hammond Thomas Hilder Jane Huang John D. Ilee Andrés F. Izquierdo Kazuhiro Kanagawa Geoffroy Lesur Giuseppe Lodato Cristiano Longarini Ryan A. Loomis Frédéric Masset Francois Menard Ryuta Orihara Daniel J. Price Giovanni Rosotti Jochen Stadler Leonardo Testi Hsi-Wei Yen Gaylor Wafflard-Fernandez David J. Wilner Andrew J. Winter Lisa Wölfer Tomohiro C. Yoshida Brianna Zawadzki |
| author_sort | Richard Teague |
| collection | DOAJ |
| description | 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. ^12 CO J = 3–2, ^13 CO J = 3–2, and CS J = 7–6 molecular emission was imaged at high angular ( $\sim 0\mathop{.}\limits^{^{\prime\prime} }15$ ) 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 μ Jy 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. |
| format | Article |
| id | doaj-art-a388ac4f43ad469c92dfa9afcb02b1eb |
| institution | DOAJ |
| issn | 2041-8205 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Letters |
| spelling | doaj-art-a388ac4f43ad469c92dfa9afcb02b1eb2025-08-20T03:19:02ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019841L610.3847/2041-8213/adc43bexoALMA. I. Science Goals, Project Design, and Data ProductsRichard Teague0https://orcid.org/0000-0003-1534-5186Myriam Benisty1https://orcid.org/0000-0002-7695-7605Stefano Facchini2https://orcid.org/0000-0003-4689-2684Misato Fukagawa3https://orcid.org/0000-0003-1117-9213Christophe Pinte4https://orcid.org/0000-0001-5907-5179Sean M. Andrews5https://orcid.org/0000-0003-2253-2270Jaehan Bae6https://orcid.org/0000-0001-7258-770XMarcelo Barraza-Alfaro7https://orcid.org/0000-0001-6378-7873Gianni Cataldi8https://orcid.org/0000-0002-2700-9676Nicolás Cuello9https://orcid.org/0000-0003-3713-8073Pietro Curone10https://orcid.org/0000-0003-2045-2154Ian Czekala11https://orcid.org/0000-0002-1483-8811Daniele Fasano12https://orcid.org/0000-0003-4679-4072Mario Flock13https://orcid.org/0000-0002-9298-3029Maria Galloway-Sprietsma14https://orcid.org/0000-0002-5503-5476Himanshi Garg15https://orcid.org/0000-0002-5910-4598Cassandra Hall16https://orcid.org/0000-0002-8138-0425Iain Hammond17https://orcid.org/0000-0003-1502-4315Thomas Hilder18https://orcid.org/0000-0001-7641-5235Jane Huang19https://orcid.org/0000-0001-6947-6072John D. Ilee20https://orcid.org/0000-0003-1008-1142Andrés F. Izquierdo21https://orcid.org/0000-0001-8446-3026Kazuhiro Kanagawa22https://orcid.org/0000-0001-7235-2417Geoffroy Lesur23https://orcid.org/0000-0002-8896-9435Giuseppe Lodato24https://orcid.org/0000-0002-2357-7692Cristiano Longarini25https://orcid.org/0000-0003-4663-0318Ryan A. Loomis26https://orcid.org/0000-0002-8932-1219Frédéric Masset27https://orcid.org/0000-0002-9626-2210Francois Menard28https://orcid.org/0000-0002-1637-7393Ryuta Orihara29https://orcid.org/0000-0003-4039-8933Daniel J. Price30https://orcid.org/0000-0002-4716-4235Giovanni Rosotti31https://orcid.org/0000-0003-4853-5736Jochen Stadler32https://orcid.org/0000-0002-0491-143XLeonardo Testi33https://orcid.org/0000-0003-1859-3070Hsi-Wei Yen34https://orcid.org/0000-0003-1412-893XGaylor Wafflard-Fernandez35https://orcid.org/0000-0002-3468-9577David J. Wilner36https://orcid.org/0000-0003-1526-7587Andrew J. Winter37https://orcid.org/0000-0002-7501-9801Lisa Wölfer38https://orcid.org/0000-0002-7212-2416Tomohiro C. Yoshida39https://orcid.org/0000-0001-8002-8473Brianna Zawadzki40https://orcid.org/0000-0001-9319-1296Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology , Cambridge, MA 02139, USAUniversité Côte d’Azur , Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, France; Max-Planck Institute for Astronomy (MPIA) , Königstuhl 17, 69117 Heidelberg, GermanyDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, 20133 Milano, ItalyNational Astronomical Observatory of Japan , Osawa 2-21-1, Mitaka, Tokyo 181-8588, JapanUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, France; School of Physics and Astronomy, Monash University , Clayton, VIC 3800, AustraliaCenter for Astrophysics ∣ Harvard & Smithsonian , Cambridge, MA 02138, USADepartment of Astronomy, University of Florida , Gainesville, FL 32611, USADepartment of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology , Cambridge, MA 02139, USANational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, FranceDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, 20133 Milano, Italy; Departamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileSchool of Physics & Astronomy, University of St. Andrews , North Haugh, St. Andrews, KY16 9SS, UK; Centre for Exoplanet Science, University of St. Andrews , North Haugh, St. Andrews, KY16 9SS, UKUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, France; Laboratoire Lagrange, Université Côte d’Azur , CNRS, Observatoire de la Côte d’Azur, 06304 Nice, FranceMax-Planck Institute for Astronomy (MPIA) , Königstuhl 17, 69117 Heidelberg, GermanyDepartment of Astronomy, University of Florida , Gainesville, FL 32611, USASchool of Physics and Astronomy, Monash University , Clayton, VIC 3800, AustraliaDepartment of Physics and Astronomy, The University of Georgia , Athens, GA 30602, USA; Center for Simulational Physics, The University of Georgia , Athens, GA 30602, USA; Institute for Artificial Intelligence, The University of Georgia , Athens, GA 30602, USASchool of Physics and Astronomy, Monash University , Clayton, VIC 3800, AustraliaInstitute for Artificial Intelligence, The University of Georgia , Athens, GA 30602, USASchool of Physics and Astronomy, Monash University , Clayton, VIC 3800, Australia; Department of Astronomy, Columbia University , 538 W. 120th Street, Pupin Hall, New York, NY, USASchool of Physics and Astronomy, University of Leeds , Leeds LS2 9JT, UKLeiden Observatory , Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands; European Southern Observatory , Karl-Schwarzschild-Str. 2, D-85748 Garching bei München, GermanyCollege of Science, Ibaraki University , 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, JapanUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, FranceDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, 20133 Milano, ItalyDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, 20133 Milano, Italy; Institute of Astronomy, University of Cambridge , Madingley Road, Cambridge CB3 0HA, UKNational Radio Astronomy Observatory , 520 Edgemont Rd., Charlottesville, VA 22903, USAInstituto de Ciencias Físicas, Universidad Nacional Autónoma de México , Av. Universidad s/n, 62210 Cuernavaca, Mor., MexicoUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, FranceCollege of Science, Ibaraki University , 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, JapanSchool of Physics and Astronomy, Monash University , Clayton, VIC 3800, AustraliaDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, 20133 Milano, ItalyUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, France; Université Côte d’Azur , Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange, 06304 Nice, FranceAlma Mater Studiorum Università di Bologna , Dipartimento di Fisica e Astronomia (DIFA), Via Gobetti 93/2, 40129 Bologna, Italy; INAF-Osservatorio Astrofisico di Arcetri , Largo E. Fermi 5, 50125 Firenze, ItalyAcademia Sinica Institute of Astronomy & Astrophysics , 11F of Astronomy-Mathematics Building, AS/NTU, No.1, Sec. 4, Roosevelt Rd, Taipei 10617, TaiwanUniv. Grenoble Alpes , CNRS, IPAG, 38000 Grenoble, FranceCenter for Astrophysics ∣ Harvard & Smithsonian , Cambridge, MA 02138, USAMax-Planck Institute for Astronomy (MPIA) , Königstuhl 17, 69117 Heidelberg, Germany; Laboratoire Lagrange, Université Côte d’Azur , CNRS, Observatoire de la Côte d’Azur, 06304 Nice, FranceDepartment of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology , Cambridge, MA 02139, USANational Astronomical Observatory of Japan , 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan; Department of Astronomical Science, The Graduate University for Advanced Studies , SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, JapanDepartment of Astronomy, Van Vleck Observatory, Wesleyan University , 96 Foss Hill Drive, MiddleTown, CT 06459, USA; Department of Astronomy & Astrophysics, 525 Davey Laboratory, The Pennsylvania State University , University Park, PA 16802, USAPlanet 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. ^12 CO J = 3–2, ^13 CO J = 3–2, and CS J = 7–6 molecular emission was imaged at high angular ( $\sim 0\mathop{.}\limits^{^{\prime\prime} }15$ ) 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 μ Jy 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.https://doi.org/10.3847/2041-8213/adc43bProtoplanetary disks |
| spellingShingle | Richard Teague Myriam Benisty Stefano Facchini Misato Fukagawa Christophe Pinte Sean M. Andrews Jaehan Bae Marcelo Barraza-Alfaro Gianni Cataldi Nicolás Cuello Pietro Curone Ian Czekala Daniele Fasano Mario Flock Maria Galloway-Sprietsma Himanshi Garg Cassandra Hall Iain Hammond Thomas Hilder Jane Huang John D. Ilee Andrés F. Izquierdo Kazuhiro Kanagawa Geoffroy Lesur Giuseppe Lodato Cristiano Longarini Ryan A. Loomis Frédéric Masset Francois Menard Ryuta Orihara Daniel J. Price Giovanni Rosotti Jochen Stadler Leonardo Testi Hsi-Wei Yen Gaylor Wafflard-Fernandez David J. Wilner Andrew J. Winter Lisa Wölfer Tomohiro C. Yoshida Brianna Zawadzki exoALMA. I. Science Goals, Project Design, and Data Products The Astrophysical Journal Letters Protoplanetary disks |
| title | exoALMA. I. Science Goals, Project Design, and Data Products |
| title_full | exoALMA. I. Science Goals, Project Design, and Data Products |
| title_fullStr | exoALMA. I. Science Goals, Project Design, and Data Products |
| title_full_unstemmed | exoALMA. I. Science Goals, Project Design, and Data Products |
| title_short | exoALMA. I. Science Goals, Project Design, and Data Products |
| title_sort | exoalma i science goals project design and data products |
| topic | Protoplanetary disks |
| url | https://doi.org/10.3847/2041-8213/adc43b |
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