2026A&A...707A.197B

Sub-Neptunes with planetary radii of R_p ≃ 2-4 R_⊕ are the most common planets around solar-type stars in short-period (P < 100 d) orbits. It is still unclear, however, what their most likely composition is, that is whether they are predominantly gas dwarfs or water worlds. The sub-Neptunes orbiting bright host stars are very valuable because they are suitable for atmospheric characterization, which can break the well-known degeneracy in planet composition from the planet bulk density, when combined with a precise and accurate mass measurement. Here we report on the characterization of the sub-Neptune TOI-5789 c, which transits in front of the bright (V = 7.3 mag and K_s = 5.35 mag) and magnetically inactive K1 V dwarf HIP 99452 every 12.93 days, thanks to TESS photometry and 141 high-precision radial velocities obtained with the HARPS-N spectrograph. We find that its radius, mass, and bulk density are R_c = 2.86_–0.15^+0.18 R_⊕, M_c = 5.00 ± 0.50 M_⊕, and ρ_c = 1.16 ± 0.23 g cm^–3, respectively, and we show that TOI-5789 c is a promising target for atmosp^–heric characterization with both JWST and, in the future, Ariel. By analyzing the HARPS-N radial velocities with different tools, we also detected three additional non-transiting planets, namely TOI-5789 b, d, and e, with orbital periods and minimum masses of P_b = 2.76 d, M_b sin i = 2.12 ± 0.28 M_⊕, P_d = 29.6 d, M_d sin i = 4.29 ± 0.68 M_⊕, and P_e = 63.0 d, M_e sin i = 11.61 ± 0.97 M_⊕. TOI- 5789 is a mutually inclined system as the difference between the orbital inclinations of planets b and c must be higher than ∼4 deg. Nevertheless, from sensitivity studies based on both the HARPS-N and archival HIRES radial-velocity measurements, we can exclude the possibility that these relatively high mutual inclinations are due to the perturbation by an outer gaseous giant planet.