May
2026
•
2026MNRAS.548ag713P
Authors
•
Peláez-Torres, A.
•
Pozuelos, F. J.
•
Morello, G.
•
Dévora-Pajares, M.
•
Barkaoui, K.
•
Gkouvelis, L.
•
Pallé, E.
•
Collins, K. A.
•
Rackham, B. V.
•
Geraldía-González, S.
•
Centenera-Merino, M.
•
Varas, R.
•
Esparza-Borges, E.
•
Parlapani, Z.
•
Flores, J.
•
Aceituno, J.
•
Amado, P. J.
•
Burdanov, A.
•
Calatayud-Borras, Y.
•
Ciardi, D. R.
•
Demory, B. O.
•
Gan, T.
•
Giacalone, S.
•
Gillon, M.
•
Chew, Y. Gómez Maqueo
•
Kawauchi, K.
•
Khandelwal, A.
•
Korth, J.
•
Lendl, M.
•
de Leon, J. P.
•
Livingston, J.
•
Morales, N.
•
Murgas, F.
•
Narita, N.
•
Ortiz, J. L.
•
Parviainen, H.
•
Marcano, M. Pichardo
•
Plauchu-Frayn, I.
•
Queloz, D.
•
Rapetti, D.
•
Saito, J.
•
Sánchez-López, A.
•
Savel, A. B.
•
Schwarz, R. P.
•
Schroffenegger, U.
•
Serra-Ricart, M.
•
Stockdale, C.
•
Triaud, A. H. M. J.
•
de Wit, J.
•
Lang, F. Zong
Abstract
•
The Transiting Exoplanet Survey Satellite (TESS) has delivered a large number of transiting planet candidates around nearby stars by identifying periodic decreases in stellar brightness. Establishing the planetary nature of these signals and determining their fundamental properties is a necessary step towards detailed studies of their internal structure, atmospheres, and formation pathways. In this work, we investigate the planetary nature of the TOI─1752 system (M1 V, $103.02\pm 0.34$ pc), which hosts two TESS candidates: TOI─1752 b, a short-period object consistent with a lava-world scenario, and TOI─1752 c, a sub-Neptune-size planet candidate located in the optimistic habitable zone. We obtained ground-based multicolour photometric follow-up observations of TOI─1752, which we combined with TESS photometry to assess the nature of both signals. We performed a formal statistical validation using the TRICERATOPS framework, while independently vetting the candidates with the neural-network-based classifier WATSON-Net, which provides a machine-learning assessment of their planetary likelihood based on light-curve morphology, centroid diagnostics, and auxiliary vetting features. We validate TOI─1752 b as a bona fide planet with a radius of $1.69\pm 0.07\, R_{\oplus }$ and an orbital period of $0.935186^{+0.000001}_{-0.000002}$ d, and TOI─1752 c with a radius of $2.29^{+0.13}_{-0.14}\, R_{\oplus }$ and an orbital period of $32.7144\pm 0.0004$ d. The combined analysis confirms TOI─1752 as a new planetary system, places TOI─1752 c within the optimistic habitable zone of its host star, and identifies TOI─1752 b as a promising target for atmospheric characterization, with an estimated emission spectroscopy metric of up to $\sim 8$.
Links
