S. C. C. Barros, O. Demangeon, Y. Alibert, A. Leleu, V. Zh. Adibekyan, C. Lovis, D. Bossini, S. G. Sousa, N. Hara, F. Bouchy, B. Lavie, J. Rodrigues, J. Gomes da Silva, J. Lillo-Box, F. Pepe, H. M. Tabernero, M. R. Zapatero Osorio, A. Sozzetti, A. Suárez Mascareño, C. Allende Prieto, S. Cristiani, M. Damasso, P. Di Marcantonio, D. Ehrenreich, J. P. Faria, P. Figueira, J. I. González Hernández, J. S. Jenkins, G. Lo Curto, C. J. A. P. Martins, G. Micela, G. Micela, N. J. Nunes, E. Pallé, N. C. Santos, R. Rebolo López, S. Seager, J. D. Twicken, S. Udry, R. K. Vanderspek, J. N. Winn

Abstract
Context. Comparing the properties of planets orbiting the same host star, and thus formed from the same accretion disc, helps in constraining theories of exoplanet formation and evolution. As a result, the scientific interest in multi-planetary systems is growing with the increasing number of detections of planetary companions.
Aims. We report the characterisation of a multi-planetary system composed of five exoplanets orbiting the K-dwarf HD 23472 (TOI-174).
Methods. In addition to the two super-Earths that were previously confirmed, we confirm and characterise three Earth-size planets in the system using ESPRESSO radial velocity observations. The planets of this compact system have periods of P_d ~ 3.98, P_e ~ 7.90, P_f ~ 12.16, P_b ~ 17.67, and P_c ~ 29.80 days and radii of R_d ~ 0.75 , R_e ~ 0.82,, R_f ~ 1.13 , R_b ~ 2.01, and, R_c ~ 1.85 R_⊕ .Because of its small size, its proximity to planet d’s transit, and close resonance with planet d, planet e was only recently found.
Results. The planetary masses were estimated to be M_d = 0.54 ± 0.22, M_e = 0.76 ± 0.30, M_f = 0.64_−0.39^+0.46, M_b = 8.42_−0.84^+0.83, and Mc = 3.37_−0.87^+0.92 M_⊕. These planets are among the lightest planets, with masses measured using the radial velocity method, demonstrating the very high precision of the ESPRESSO spectrograph. We estimated the composition of the system’s five planets and found that their gas and water mass fractions increase with stellar distance, suggesting that the system was shaped by irradiation. The high density of the two inner planets (ρ_d = 7.5_−3.1^+3.9 and ρ_e = 7.5_−3.0^+3.9 g cm⁻³) indicates that they are likely to be super-Mercuries. This is supported by the modelling of the internal structures of the planets, which also suggests that the three outermost planets have significant water or gas content.
Conclusions. If the existence of two super-Mercuries in the system is confirmed, this system will be the only one known to feature two super-Mercuries, making it an excellent testing bed for theories of super-Mercuries formation. Furthermore, the system is close to a Laplace resonance, and further monitoring could shed light on how it was formed. Its uniqueness and location in the continuous viewing zone of the James Webb space telescope will make it a cornerstone of future in-depth characterisations.

Notes
^★ Radial velocity observations are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/665/A154

^★★ Based in part on Guaranteed Time Observations collected at the European Southern Observatory under ESO programme(s) 1102.C-0744, 1102.C-0958, and 1104.C-0350 by the ESPRESSO Consortium.

Astronomy & Astrophysics
Volume 665, Article Number A154, Number of pages 24
2022 September

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