Proyecto de Investigación: FInding ExoeaRths: tackling the ChallengEs of stellar activity
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The PLATO mission
(Springer Nature Link, 2025-04-21) Rauer, Heike; Aerts, Conny; Cabrera, Juán; Deleuil, Magali; Erikson, Anders; Gizon, Laurent; Goupil, Mariejo; Heras, Ana; Walloschek, Thomas; Lorénzo Álvarez, José; Marliani, Filippo; Martín García, César; Mas Hesse, José Miguel; O´Rourke, Laurence; Osborn, Hugh P.; Pagano, Isabella; Piotto, Giampaolo; Pollacco, Don; Ragazzoni, Roberto; Ramsay, Gavin; Udry, Stéphane; Appourchaux, Thierry; Benz, Willy; Brandeker, Alexis; Güdel, Manuel; Janot Pacheco, Eduardo; Kabath, Petr; Kjeldsen, Hans; Min, Michiel; Santos, Nuno C.; Smith, Alan; Suarez, Juan Carlos; Werner, Stephanie; Aboudan, Alessio; Abreu, Manuel; Acuña, Lorena; Adams, Moritz; Adibekyan, Vardan; Affer, Laura; Agneray, François; Agnor, Craig; Aguirre Børsen Koch, Victor; Ahmed, Saad; Aigrain, Suzanne; Al Bahlawan, Ashraf; De los Angeles Alcacera Gil, Ma; Alei, Eleonora; Alencar, Silvia; Alexander, Richard; Alfonso Garzón, Julia; Alibert, Yann; Alende Prieto, Carlos; Almeida, Leonardo; Alonso Sobrino, Roi; Altavilla, Giuseppe; Althaus, Christian; Álvarez Trujillo, Luis Alonso; Amarsi, Anish; Von Eiff, Matthias Ammler; Amôres, Eduardo; Andrade, Laerte; Antoniadis Karnavas, Alexandros; Antonio, Carlos; Aparico del Moral, Beatriz; Appolloni, Mateo; Arena, Claudio; Armstrong, David; Aroca Aliaga, José; Asplund, Martín; Audenaert, Jeoen; Auricchio, Natalia; Avelino, Pedro; Baeke, Ann; Baillié, Kevin; Balado, Ana; Ballber Balagueró, Pau; Balestra, Andrea; Ball, Warrick; Ballans, Herve; Ballot, Jerome; Barban, Caroline; Barbary, Gaële; Barbieri, Mauro; Barceló Fortaleza, Sebastià; Barker, Adrian; Barklem, Paul; Barnes, Sydney; Barrado, David; Barragan, Oscar; Baruteau, Clément; Basu, Sarbani; Baudin, Frederic; Baumeister, Philipp; Bayliss, Daniel; Bazot, Michael; Beck, Paul; Belkacem, Kevin; Bellinger, Earl; Benatti, Serena; Benomar, Othman; Bérard, Diae; Bergemann, María; Bergomi, María; Bernardo, Pierre; Biazzo, Katia; Bignamini, Andrea; Bigot, Lionel; Billot, Nicolas; Binet, Martín; Biondi, David; Biondi, Federico; Birch, Aaron; Bisch, Bertram; Bluhm Ceballos, Paz Victoria; Bódi, Attila; Bognár, Zsófia; Boisse, Isabelle; Bolmont, Emeline; Bonanno, Alfio; Bonavita, Mariangela; Bonfanti, Andrea; Bonfils, Xavier; Bonito, Rosaria; Bonomo, Aldo Stefano; Börner, Anko; Boro Saikia, Sudeshna; Borreguero Martín, Elisa; Borsa, Francesco; Borsato, Luca; Bossini, Diego; Bouchy, F.; Boué, Gwenaël; Boufleur, Rodrigo; Boumier, Patrick; Bourrier, V.; Bowman, Dominic; Bozzo, Enrico; Bradley, Louisa; Bray, John; Bressan, Aessandro; Breton, Sylvain; Brienza, Daniele; Brito, Ana; Brogi, Matteo; Brown, Beverly; Brown, David; Sacha Brun, Allan; Bruno, Giovanni; Bruns, Michael; Buchhave, Lars; Bugnet, Lisa; Buldgen, Gaël; Burgess, Patrick; Busatta, Andrea; Busso, Giogia; Buzasi, Derek; Caballero, Jose A.; Cabral, Alexandre; Cabrero Gómez, Juan Francisco; Calderone, Flavia; Cameron, Robert; Cameron, Andrew; Campante, Tiago; Campos Gestal, Néstor; Canto Martins, Bruno Leonardo; Cara, Christophe; Carone, Ludmila; Carrasco, Josep Manuel; Casagrande, Luca; Casewell, Sarah; Cassisi, Santi; Castellani, Marco; Castro, Matthieu; Catala, Claude; Catalán Fernández, Irene; Catelan, Márcio; Cegla, Heather; Cerruti, Chiara; Cessa, Virginie; Chadid, Merieme; Chaplin, William; Charpinet, Stephane; Chiappini, Cristina; Chiarucci, Simone; Chiavassa, Andrea; Chinellato, Simonetta; Chirulli, Giovanni; Christensen Dalsgaard, Jørgen; Church, Ross; Claret, Antonio; Clarke, Cathie; Claudi, Riccardo; Clermont, Lionel; et., al.; European Commission (EC); European Research Council (ERC); Agencia Estatal de Investigación (AEI)
PLATO (PLAnetary Transits and Oscillations of stars) is ESA’s M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2R) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5%, 10%, 10% for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO‘s target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile towards the end of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.
Two neighbours of the ultra-short-period Earth-sized planet K2-157 b in the warm Neptunian savanna
(EDP Sciences, 2025-07-22) Castro-González, Amadeo; Bouchy, F.; Correia, A. C. M.; Sozzetti, A.; Lillo Box, J.; Figueira, P.; Lavie, B.; Lovis, C.; Hobson, Melissa J.; Sousa, S. G.; Adibekyan, Vardan; Standing, Matthew R.; Hara, Nathan C.; Barrado, David; Silva, André; Bourrier, V.; Korth, J.; Santos, Nuno C.; Damasso, M.; Zapatero Osorio, María Rosa; Rodrigues, José; Alibert, Yann; Barros, S. C. C.; Cristiani, S.; Marcantonio, Paolo Di; González Hernández, J. I.; Lo Curto, G.; Martins, C. J. A. P.; Nunes, Nelson J.; Pallé, E.; Pepe, Francesco; Suárez Mascareño, A.; Tabernero, H. M.; Fundacao para a Ciencia e a Tecnologia (FCT); European Commission (EC); Centros de Excelencia Severo Ochoa, INSTITUTO DE ASTROFÍSICA DE CANARIAS (IAC), SEV-2015-0548
[Context] The formation and evolution of ultra-short-period (USP) rocky planets is poorly understood. However, it is widely thought that these planets could not have formed at their present-day close-in orbits, but instead migrated inwards through interactions with outer neighbours.
[Aims] We aim to confirm and characterise the USP Earth-sized validated planet K2-157 b (Porb = 8.8 h) and constrain the presence of additional companions in the system through radial velocity (RV) measurements.
[Methods] We measured 49 RVs with the ESPRESSO spectrograph and tested different planetary and non-planetary configurations to infer the model that best represents our data set. We derived the orbital and physical properties of the system through a global RV and transit model.
[Results] We detected two additional super-Neptune-mass planets located within the warm Neptunian savanna, K2-157 c (Porb,c = 25.942−0.044+0.045d, Mp,c sin i = 30.8 ± 1.9 M⊕) and K2-157 d (Porb,d = 66.50−0.59+0.71d, Mp,d sin i = 23.3 ± 2.5 M⊕). The joint analysis constrains the mass of K2-157 b at the 2.7σ level, Mp,b = 1.14−0.42+0.41 M⊕ (< 2.4 M⊕ at 3σ), which, together with the inferred radius, Rp,b = 0.935 ± 0.090 R⊕, make the planet compatible with a rocky composition with a likely (68% confidence) higher iron-to-silicate mass fraction than Earth. K2 data discard non-grazing transit configurations for K2-157 c (ic < 88.4° at 3σ), and ESPRESSO data constrain the eccentricities of K2-157 c and K2-157 d to ec < 0.2 and ed < 0.5 at 3σ. Our dynamical analysis indicates that the system is stable for eccentricities up to ec, ed ~ 0.3 and mutual inclinations up to ~60°. At a population level, we find that the trend that the closest USP planets tend to orbit late-type stars does not hold when scaling the orbital separation to the Roche limit, which suggests that the orbital distribution of the closest planets across spectral types is primarily determined by tidal disruption.
[Conclusions] The orbital architecture of K2-157 is unusual in the known exoplanet plethora, with only one similar case reported to date: 55 Cnc. The USP planets of these systems, being accompanied by massive, long-period, relatively spaced, and possibly misaligned neighbours, could have migrated inwards through eccentricity-based mechanisms triggered by secular interactions.
