ALMA-IMF: VII. First release of the full spectral line cubes: Core kinematics traced by DCN J = (3-2)
Por:
Cunningham N., Ginsburg A., Galván-Madrid R., Motte F., Csengeri T., Stutz A.M., Fernández-López M., Álvarez-Gutiérrez R.H., Armante M., Baug T., Bonfand M., Bontemps S., Braine J., Brouillet N., Busquet G., Díaz-González D.J., Di Francesco J., Gusdorf A., Herpin F., Liu H., López-Sepulcre A., Louvet F., Lu X., Maud L., Nony T., Olguin F.A., Pouteau Y., Rivera-Soto R., Sandoval-Garrido N.A., Sanhueza P., Tatematsu K., Towner A.P.M., Valeille-Manet M.
Publicada:
1 ene 2023
Resumen:
ALMA-IMF is an Atacama Large Millimeter/submillimeter Array (ALMA) Large Program designed to measure the core mass function (CMF) of 15 protoclusters chosen to span their early evolutionary stages. It further aims to understand their kinematics, chemistry, and the impact of gas inflow, accretion, and dynamics on the CMF. We present here the first release of the ALMA-IMF line data cubes (DR1), produced from the combination of two ALMA 12 m-array configurations. The data include 12 spectral windows, with eight at 1.3 mm and four at 3 mm. The broad spectral coverage of ALMA-IMF (~6.7 GHz bandwidth coverage per field) hosts a wealth of simple atomic, molecular, ionised, and complex organic molecular lines. We describe the line cube calibration done by ALMA and the subsequent calibration and imaging we performed. We discuss our choice of calibration parameters and optimisation of the cleaning parameters, and we demonstrate the utility and necessity of additional processing compared to the ALMA archive pipeline. As a demonstration of the scientific potential of these data, we present a first analysis of the DCN (3-2) line. We find that DCN (3-2) traces a diversity of morphologies and complex velocity structures, which tend to be more filamentary and widespread in evolved regions and are more compact in the young and intermediate-stage protoclusters. Furthermore, we used the DCN (3-2) emission as a tracer of the gas associated with 595 continuum cores across the 15 protoclusters, providing the first estimates of the core systemic velocities and linewidths within the sample. We find that DCN (3-2) is detected towards a higher percentage of cores in evolved regions than the young and intermediate-stage protoclusters and is likely a more complete tracer of the core population in more evolved protoclusters. The full ALMA 12m-array cubes for the ALMA-IMF Large Program are provided with this DR1 release. © 2023 The Authors.
Filiaciones:
Cunningham N.:
Université Grenoble Alpes, Cnrs, Institut de Planétologie et d' Astrophysique de Grenoble, Grenoble, 38000, France
Ginsburg A.:
Department of Astronomy, University of Florida, PO Box 112055, Gainesville, United States
Galván-Madrid R.:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, Mexico
Motte F.:
Université Grenoble Alpes, Cnrs, Institut de Planétologie et d' Astrophysique de Grenoble, Grenoble, 38000, France
Csengeri T.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Stutz A.M.:
Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, 4030000, Chile
Fernández-López M.:
Instituto Argentino de Radioastronomí A (CCT-La Plata CONICET
Álvarez-Gutiérrez R.H.:
Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, 4030000, Chile
Armante M.:
Laboratoire de Physique de l' Ecole Normale Supérieure, Ens, Université Psl, Cnrs, Sorbonne Université, Université Paris Cité, Paris, 75005, France
Observatoire de Paris, PSL University, Sorbonne Université, LERMA, Paris, 75014, France
Baug T.:
S. N. Bose National Centre for Basic Sciences, Sector III, Salt Lake, Kolkata, 700106, India
Bonfand M.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Department of Astronomy, University of Virginia, Charlottesville, VA 22904, United States
Bontemps S.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Braine J.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Brouillet N.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Busquet G.:
Department de Frisca Quantica i Astrofrisca, Universitat de Barcelona (UB), c. Martí i Franquès, 1 Barcelona, Catalonia, 08028, Spain
Instituto de Cièncias Del Cosmos (ICCUB), Universitat de Barcelona (UB), c. Martí i Franquès, 1, Catalonia, Barcelona, 08028, Spain
Institut d' Estudis Espacials de Catalunya (IEEC), Gran Capita, 2-4, Barcelona, Catalonia, 08340, Spain
Díaz-González D.J.:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, Mexico
Di Francesco J.:
Herzberg Astronomy and Astrophysics Research Centre, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada
Gusdorf A.:
Laboratoire de Physique de l' Ecole Normale Supérieure, Ens, Université Psl, Cnrs, Sorbonne Université, Université Paris Cité, Paris, 75005, France
Observatoire de Paris, PSL University, Sorbonne Université, LERMA, Paris, 75014, France
Herpin F.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Liu H.:
Department of Astronomy, Yunnan University, Kunming, 650091, China
López-Sepulcre A.:
Université Grenoble Alpes, Cnrs, Institut de Planétologie et d' Astrophysique de Grenoble, Grenoble, 38000, France
Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, Saint-Martin-d' Hères, 38406, France
Louvet F.:
Université Grenoble Alpes, Cnrs, Institut de Planétologie et d' Astrophysique de Grenoble, Grenoble, 38000, France
DAS, Universidad de Chile, 1515 Camino El Observatorio, Las Condes, Santiago, Chile
Lu X.:
Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai, 200030, China
Maud L.:
Eso Headquarters, Karl-Schwarzchild-Str 2, Garching, 85748, Germany
Nony T.:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, Mexico
Olguin F.A.:
Institute of Astronomy, National Tsing Hua University, Hsinchu, 30013, Taiwan
Pouteau Y.:
Université Grenoble Alpes, Cnrs, Institut de Planétologie et d' Astrophysique de Grenoble, Grenoble, 38000, France
Rivera-Soto R.:
Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Michoacán, 58089, Mexico
Sandoval-Garrido N.A.:
Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción, 4030000, Chile
Sanhueza P.:
National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Astronomical Science Program, Graduate Institute for Advanced Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Tatematsu K.:
National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Astronomical Science Program, Graduate Institute for Advanced Studies, SOKENDAI, 2-21-1 Osawa, Mitaka, Tokyo, 181-8588, Japan
Towner A.P.M.:
Department of Astronomy, University of Florida, PO Box 112055, Gainesville, United States
Valeille-Manet M.:
Laboratoire d' Astrophysique de Bordeaux, Univ. Bordeaux, Cnrs, B18N Allée Geoffroy Saint-Hilaire, Pessac, 33615, France
Green Submitted, hybrid, Hybrid Gold
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