We present the discovery by the TESS mission of one transiting Neptune-sized planet, TOI-6223, b, and two transiting super-Earths, TOI-1743, b and TOI-5799, b. We validate these planets using a statistical validation method, multi-color light curves, and other ancillary observations. We combined TESS and ground-based photometric data to constrain the physical properties of the planets. TOI-6223, b is slightly larger than Neptune (Rₚ=5. 12^ R_⊕) orbiting an early M dwarf in 3. 86 days, and it has an equilibrium temperature of T_ ̊m eq =714±14 K. TOI-1743, b orbits its mid-dwarf star every 4. 27 days. It has a radius of Rₚ=1. 83^ R_⊕ and an equilibrium temperature of T_ ̊m eq K. TOI-5799, b has a radius of Rₚ=1. 733^ R_⊕ and an equilibrium temperature of T_ ̊m eq =505±16 K. It orbit around an M2 dwarf in 4. 17 days. We also present the discovery of an additional transiting planet, TOI-5799, c, which we identified in the TESS data and validated using the SHERLOCK pipeline. TOI-5799, c is a super-Earth with a radius of Rₚ=1. 76^ R_⊕. Its orbital period and its equilibrium temperature are 14. 01 days and T_ ̊m eq =337±11 K, respectively, which place it near the inner edge of the habitable zone of its star. We show that these planets are suitable for both radial velocity follow-up and atmospheric characterization. They orbit bright (< 11 Kₘag) 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 what is known as the radius valley, while TOI-6223, b is located on the Neptunian ridge in the period--radius plane.
Yalç et al. (Mon,) studied this question.