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Osborn, H. P.; Bonfanti, A.; Gandolfi, D.; Hedges, C.; Leleu, A.; Fortier, A.; Futyan, D.; Gutermann, P.; Maxted, P. F. L.; Borsato, L.; Collins, K. A.; Gomes da Silva, J.; Gómez Maqueo Chew, Y.; Hooton, M. J.; Lendl, M.; Parviainen, H.; Salmon, S.; Schanche, N.; Serrano, L. M.; Sousa, S. G.; Tuson, A.; Ulmer-Moll, S.; Van Grootel, V.; Wells, R. D.; Wilson, T. G.; Alibert, Y.; Alonso, R.; Anglada, G.; Asquier, J.; Barrado y Navascues, D.; Baumjohann, W.; Beck, T.; Benz, W.; Biondi, F.; Bonfils, X.; Bouchy, F.; Brandeker, A.; Broeg, C.; Bárczy, T.; Barros, S. C. C.; Cabrera, J.; Charnoz, S.; Collier Cameron, A.; Csizmadia, S.; Davies, M. B.; Deleuil, M.; Delrez, L.; Demory, B.-O.; Ehrenreich, D.; Erikson, A.; Fossati, L.; Fridlund, M.; Gillon, M.; Gömez-Munoz, M. A.; Güdel, M.; Heng, K.; Hoyer, S.; Isaak, K. G.; Kiss, L.; Laskar, J.; Lecavelier des Etangs, A.; Lovis, C.; Magrin, D.; Malavolta, L.; McCormac, J.; Nascimbeni, V.; Olofsson, G.; Ottensamer, R.; Pagano, I.; Pallé, E.; Peter, G.; Piazza, D.; Piotto, G.; Pollacco, D.; Queloz, D.; Ragazzoni, R.; Rando, N.; Rauer, H.; Reimers, C.; Ribas, I.; Demangeon, O. D. S.; Smith, A. M. S.; Sabin, L.; Santos, N.; Scandariato, G.; Schroffenegger, U.; Schwarz, R. P.; Shporer, A.; Simon, A. E.; Steller, M.; Szabó, G. M.; Ségransan, D.; Thomas, N.; Udry, S.; Walter, I.; Walton, N.
Astronomy and astrophysics (Berlin), 2022, Letnik: 664Journal Article, Web Resource
Context. TOI-2076 is a transiting three-planet system of sub-Neptunes orbiting a bright ( G = 8.9 mag), young (340 ± 80 Myr) K-type star. Although a validated planetary system, the orbits of the two outer planets were unconstrained as only two non-consecutive transits were seen in TESS photometry. This left 11 and 7 possible period aliases for each. Aims. To reveal the true orbits of these two long-period planets, precise photometry targeted on the highest-probability period aliases is required. Long-term monitoring of transits in multi-planet systems can also help constrain planetary masses through TTV measurements. Methods. We used the MonoTools package to determine which aliases to follow, and then performed space-based and ground-based photometric follow-up of TOI-2076 c and d with CHEOPS, SAINT-EX, and LCO telescopes. Results. CHEOPS observations revealed a clear detection for TOI-2076 c at $P = 21.02538_{ - 0.00074}^{ + 0.00084}$ d, and allowed us to rule out three of the most likely period aliases for TOI-2076 d. Ground-based photometry further enabled us to rule out remaining aliases and confirm the P = 35.12537 ± 0.00067 d alias. These observations also improved the radius precision of all three sub-Neptunes to 2.518 ± 0.036, 3.497 ± 0.043, and 3.232 ± 0.063 R ⊕ . Our observations also revealed a clear anti-correlated TTV signal between planets b and c likely caused by their proximity to the 2:1 resonance, while planets c and d appear close to a 5:3 period commensurability, although model degeneracy meant we were unable to retrieve robust TTV masses. Their inflated radii, likely due to extended H-He atmospheres, combined with low insolation makes all three planets excellent candidates for future comparative transmission spectroscopy with JWST.
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