TOI-1743 b, TOI-5799 b, TOI-5799 c and TOI-6223 b: TESS Discovery And Validation Of Four Super-Earth To Neptune-sized Planets Around M dwarfs

We combined TESS and ground-based photometric data to constrain the physical properties of the planets. TOI-6223-b is slightly larger than Neptune (R_p=5.12+0.24−0.25 R_⊕) orbiting an early M dwarf in 3.86 days, and it has an equilibrium temperature of T_eq=714±14 K. TOI-1743 b orbits its M4V star every 4.27 days.

It has a radius of R_p=1.83+0.11−0.10 R_⊕ and an equilibrium temperature of T_eq=485+14−13 K. TOI-5799 b has a radius of R_p=1.733+0.096−0.090 R_⊕, and an equilibrium temperature of T_eq=505±16 K orbits an M2 dwarf in 4.17 days.

We also present the discovery of an additional transiting planet, TOI-5799 c, that we identified in the TESS data and validated using the SHERLOCK pipeline. TOI-5799 c is a super-Earth with a radius of R_p=1.76+0.11−0.10 R_⊕.

Its orbital period and its equilibrium temperature are 14.01 days and T_eq=337±11 K, which place it near the inner edge of the habitable zone of its this http URL show that these planets are suitable for both radial velocity follow-up and atmospheric characterization. They orbit bright (< 11 K_mag) early M dwarfs, making them accessible for precise mass measurements.

The combination of the planet sizes and stellar brightness of their host stars also make them suitable targets for atmospheric exploration with the JWST. Such studies may provide insights into planet formation and evolution, as TOI-1743-b, TOI-5799-b, and TOI-5799-c lie within the so-called radius valley, while TOI-6223-b is located on the Neptunian ridge in the period-radius plane.

Period-radius diagram of transiting exoplanets. The boundaries of the Neptunian desert, ridge, and savanna (CastroGonzález et al. 2024a) are indicated with black dashed lines. TOI-6223 b is shown with green hexagon. Data were extracted from NASA Exoplanet Archive. This plot was generated with nep-des (https://github.com/castro-gzlz/nep-des). — astro-ph.EP

S. Yalçınkaya, K. Barkaoui, Ö. Baştürk, M. Gillon, F. J. Pozuelos, M. Timmermans, B. V. Rackham, A. J. Burgasser, P. Mistry, A. Peláez-Torres, G. Morello, E. K. Pass, A. Bieryla, D. W. Latham, K. A. Collins, F. Akar, Z. Benkhaldoun, A. Burdanov, J. Brande, D. R. Ciardi, C. A. Clark, E. Ducrot, J. de Wit, B. O. Demory, E. M. Esmer, M. E. Everett, G. Fernández-Rodriguez, A. Fukui, M. Ghachoui, E. A. Gilbert, E. Girardin, Y. Gómez Maqueo Chew, K. Ikuta, K. Isogai, M.J. Hooton, M. Jafariyazani, E. Jehin, J.M. Jenkins, P.R. Karpoor, Y. Kawai, K. Kawauchi, A. Khandelwal, A.C. Kutluay, G. Lacedelli, M. Lendl, M.B. Lund, F. Murgas, N. Narita, E. Palle, P. P. Pedersen, I. Plauchu-Frayn, A. S. Polanski, D. Queloz, U. Schroffenegger, R. P. Schwarz, A. Shporer, E. Softich, S. Sohy, A. Soubkiou, G. Srdoc, I.A. Strakhov, A. H. M. J. Triaud, C. Ziegler, F. Zong Lang, S. Zúñiga-Fernández

Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2509.05038 [astro-ph.EP] (or arXiv:2509.05038v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2509.05038
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From: Selcuk Yalcinkaya
[v1] Fri, 5 Sep 2025 11:54:51 UTC (7,301 KB)
https://arxiv.org/abs/2509.05038
Astrobiology,