Статья

The PLATO field selection process

V. NascimbeniINAF – Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, ItalyG. PiottoDipartimento di Fisica e Astronomia “Galileo Galilei”, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, ItalyJ. CabreraDeutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Planetenforschung, Rutherfordstraße 2, 12489 Berlin-Adlershof, GermanyM. MontaltoINAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, ItalyS. MarinoniINAF – Osservatorio Astronomico di Roma, Via Frascati, 33, 00078 Monte Porzio Catone (RM), ItalyP. M. MarreseINAF – Osservatorio Astronomico di Roma, Via Frascati, 33, 00078 Monte Porzio Catone (RM), ItalyC. AertsInstitute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, BelgiumG. AltavillaINAF – Osservatorio Astronomico di Roma, Via Frascati, 33, 00078 Monte Porzio Catone (RM), ItalyS. BenattiINAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90129 Palermo, ItalyA. BörnerDeutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Optische Sensorsysteme, Rutherfordstraße 2, 12489 Berlin-Adlershof, GermanyM. DeleuilAix-Marseille Université, CNRS, CNES, Laboratoire d’Astrophysique de Marseille, Technopôle de Marseille-Etoile, 38, rue Frédéric Joliot-Curie, 13388 Marseille cedex 13, FranceS. DesideraINAF – Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, ItalyL. GizonMax-Planck-Institut für Sonnensystemforschung, Justus-von-Liebig-Weg 3, 37077 Göttingen, GermanyM. J. GoupilLESIA, CNRS UMR 8109, Université Pierre et Marie Curie, Université Denis Diderot, Observatoire de Paris, 92195 Meudon, FranceV. GranataDipartimento di Fisica e Astronomia “Galileo Galilei”, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, ItalyA. M. HerasEuropean Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Keplerlaan 1, 2201 AZ Noordwijk, The NetherlandsDemetrio MagrinINAF – Osservatorio Astronomico di Padova, vicolo dell’Osservatorio 5, 35122 Padova, ItalyL. MalavoltaDipartimento di Fisica e Astronomia “Galileo Galilei”, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, ItalyJ. M. Más-HesseCentro de Astrobiología (CSIC–INTA), Depto. de Astrofísica, 28692 Villanueva de la Cañada, Madrid, SpainH. P. OsbornCenter for Space and Habitability, University of Bern, Bern, SwitzerlandI. PaganoINAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, ItalyCarsten PaprothDeutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Optische Sensorsysteme, Rutherfordstraße 2, 12489 Berlin-Adlershof, GermanyD. PollaccoDepartment of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UKL. PrisinzanoINAF–Osservatorio Astronomico di Palermo, Piazza del Parlamento, 1, 90129 Palermo, ItalyRoberto RagazzoniDipartimento di Fisica e Astronomia “Galileo Galilei”, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, ItalyGavin RamsayArmagh Observatory & Planetarium, College Hill, Armagh, BT61 9DG, UKH. RauerDeutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Planetenforschung, Rutherfordstraße 2, 12489 Berlin-Adlershof, GermanyA. TkachenkoInstitute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Leuven, BelgiumS. UdryObservatoire de Genève, Université de Genève, Chemin Pegasi 51, 1290 Sauverny, Switzerland

2025en

ABI

Аннотация

PLAnetary Transits and Oscillations of stars (PLATO) is an ESA M-class mission to be launched by the end of 2026 to discover and characterize transiting planets around bright and nearby stars, and in particular habitable rocky planets hosted by solar-like stars. Over the mission lifetime, an average of 8% of the science data rate will be allocated to Guest Observer programs selected by ESA through public calls. Hence, it is essential for the community to know in advance where the observing fields will be located. In a previous paper, we identified two preliminary long-pointing fields (LOPN1 and LOPS1) for PLATO, respectively in the northern and southern hemispheres. Here we present LOPS2, a slightly adjusted version of the southern field that has recently been selected by the PLATO Science Working Team as the first field to be observed by PLATO for at least two continuous years, following the scientific requirements. In this paper, we describe the astrophysical content of LOPS2 in detail, including known planetary systems, bright stars, variables, binary stars, star clusters, and synergies with other current and future facilities.

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Идентификаторы

DOI: 10.1051/0004-6361/202452325

Цитирования и источники

Цитирований: 2Использованных источников: 0

Показатели — AkademScholar