Proyecto de Investigación: Binaries Escorted By Orbiting Planets
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803193
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Six transiting planets and a chain of Laplace resonances in TOI-178
(EDP Sciences, 2021-05-06) Leleu, A.; Alibert, Y.; Hara, N. C.; Hooton, M. J.; Wilson, T. G.; Robutel, P.; Delisle, J. B.; Laskar, J.; Hoyer, S.; Lovis, C.; Bryant, E. M.; Angerhausen, D.; Simon, A. E.; Beck, T.; Sousa, S. G.; Futyan, D.; Di Marcantonio, P.; Ehrenreich, D.; Erikson, A.; Figueira, P.; Acton, J. S.; Haldemann, J.; Thomas, N.; Boué, G.; Tilbrook, R. H.; Isaak, K.; Fridlund, M.; Gandolfi, D.; García Muñoz, Antonio; García, L. J.; Verrecchia, F.; Bárczy, T.; Charnoz, S.; Lecavelier des Etangs, A.; Guillon, M.; Goad, M. R.; González Hernández, J. I.; Guedel, M.; Sebastian, D.; Zapatero Osorio, María Rosa; Heng, K.; Jehin, E.; Jenkins, J. S.; Jordán, A.; Kiss, L.; Anderson, D. R.; Murray, C. A.; Anglada Escudé, G.; Fortier, A.; Barrado, David; Osborn, Hugh P. ; Lam, K.; Lendl, M.; Lillo Box, J.; Lo Curto, G.; Corral Van Damme, C.; Bekkelien, A.; Gill, S.; Billot, N.; Piotto, G.; Maxted, P. F. L.; McCormac, J.; Mehner, A.; Micela, G.; Brandeker, A.; Nunes, Nelson J.; Rando, N.; Oshagh, M.; Ottensamer, R.; Pagano, I.; Pallé, E. ; Cameron, A. C.; Persson, Carina; Polenta, G.; Pollacco, D.; Poretti, E.; Demangeon, O. D. S.; Sestovic, M.; Demory, B. O.; Magrin, D.; Di Persio, G.; Sozzetti, A.; Ragazzoni, R.; Ratti, F.; Rauer, H.; Raynard, L.; Fossati, L.; Molaro, P.; Nascimbeni, V.; Triaud, A.; Ribas, I.; Santos, Nuno C.; Scandariato, G.; Schneider, J.; Gillen, E.; Smith, A. M. S.; Steller, M.; Suárez Mascareño, A.; Szabó, Gy. M.; Ségransan, D.; Günther, M. N.; Ducrot, E.; Henderson, B.; Pozuelos, F. J. ; Hogan, A. E.; Adibekyan, V.; Thompson, S.; Turner, O.; Udry, S.; Van Grootel, V.; Olofsson, G.; Kristiansen, M. H.; Rebolo, R.; Lavie, B.; Barros, S. C. C.; Vines, J. I.; Walton, N. A.; West, R. G.; Wheatley, Peter; Martins, C. J. A. P.; Delrez, L.; Bonfanti, A.; Allart, R.; Allende Prieto, C.; Alonso, R.; Alves, D.; Moyaro, M.; Asquier, J.; Baumjohann, W.; Bayliss, D.; Beck, M.; Pedersen, P. P.; Chamberlain, S.; Pepe, Francesco; Venus, H.; Peter, G.; Correia, A. C. M.; Benz, W.; Bonfils, Xavier; Bouchy, F.; Bourrier, V.; Queloz, D.; Wolter, D.; Cabrera, J.; Dumusque, X.; Broeg, C.; Buder, M.; Burdanov, A.; Burleigh, M. R.; Reimers, C.; Cooke, B. F.; Cristiani, S.; Damasso, M.; Davies, M. B.; Deleuil, M.; Alvarez, M. [0000-0002-6786-2620]; Carrasco Martínez, J. M. [0000-0002-3029-5853]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. In this context, TOI-178 has been the subject of particular attention since the first TESS observations hinted at the possible presence of a near 2:3:3 resonant chain. Here we report the results of observations from CHEOPS, ESPRESSO, NGTS, and SPECULOOS with the aim of deciphering the peculiar orbital architecture of the system. We show that TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, with radii ranging from 1.152−0.070+0.073 to 2.87−0.13+0.14 Earth radii and periods of 1.91, 3.24, 6.56, 9.96, 15.23, and 20.71 days. All planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet, jumping from 1.02−0.23+0.28 to 0.177−0.061+0.055 times the Earth’s density between planets c and d. Using Bayesian interior structure retrieval models, we show that the amount of gas in the planets does not vary in a monotonous way, contrary to what one would expect from simple formation and evolution models and unlike other known systems in a chain of Laplace resonances. The brightness of TOI-178 (H = 8.76 mag, J = 9.37 mag, V = 11.95 mag) allows for a precise characterisation of its orbital architecture as well as of the physical nature of the six presently known transiting planets it harbours. The peculiar orbital configuration and the diversity in average density among the planets in the system will enable the study of interior planetary structures and atmospheric evolution, providing important clues on the formation of super-Earths and mini-Neptunes.
A transiting rocky super-Earth and a non-transiting sub-Neptune orbiting the M dwarf TOI-771
(EDP Sciences, 2025-06-20) Lacedelli, G.; Pallé, E.; Davis, Yasmin T.; Luque, R. ; Morello, G.; Tabernero, H. M.; Zapatero Osorio, María Rosa; Pozuelos, F. J.; Jankowski, Dawid; Nowak, G.; Murgas Alcaino, F.; Orell-Miquel, Jaume; Akana Murphy, Joseph M.; Barkaoui, K.; Charbonneau, D.; Dransfield, G.; Ducrot, E.; Geraldía González, Samuel; Irwin, J.; Jehin, E.; Osborne, H. L. M.; Pedersen, P. P.; Rackham, B. V. , P. P.; Scott, Madison Grace; Timmermans, M.; Triaud, A.; Van Eylen, V.; Agencia Estatal de Investigación (AEI); National Aeronautics and Space Administration (NASA); European Research Council (ERC); European Commission (EC); Science and Technology Facilities Council (STFC); Belgian National Fund for Scientific Research (FNRS); National Science Foundation (NSF)
[Context] The origin and evolution of the sub-Neptune population is a highly debated topic in the exoplanet community. With the advent of JWST, atmospheric studies can now put unprecedented constraints on the internal composition of this population. In this context, the THIRSTEE project aims to investigate the population properties of sub-Neptunes with a comprehensive and demographic approach, providing a homogeneous sample of precisely characterised sub-Neptunes across stellar spectral types.
[Aims] We present here the precise characterisation of the planetary system orbiting one of the THIRSTEE M-dwarf targets, TOI-771 (d = 25 pc, V = 14.9 mag), known to host one planet, TOI-771 b, which has been statistically validated using TESS observations.
[Methods] We use TESS, SPECULOOS, TRAPPIST, and M-Earth photometry together with 31 high-precision ESPRESSO radial velocities to derive the orbital parameters and investigate the internal composition of TOI-771 b, as well as exploring the presence of additional companions in the system.
[Results] We derived the precise mass and radius for TOI-771 b, a super-Earth with Rb = 1.36 ± 0.10 R⊕ and Mb = 2.47−0.31+0.32M⊕ orbiting every 2.3 days around its host star. Its composition is consistent with an Earth-like planet, and it adds up to the rocky population of subNeptunes lying below the density gap identified around M dwarfs. With a ∼ 13% precision in mass, a∼ 7% radius precision, and a warm equilibrium temperature of Teq =543K, TOI-771 b is a particularly interesting target for atmospheric characterisation with JWST, and it is indeed one of the targets under consideration for the Rocky World DDT programme. Additionally, we discover the presence of a second, non-transiting planet in the system, TOI-771 c, with a period of 7.61 days and a minimum mass of Mp sin i = 2.87−0.38+0.41M⊕. Even though the inclination is not directly constrained, the planet likely belongs to the temperate sub-Neptune population, with an equilibrium temperature of ∼ 365K.
