The GAPS programme at TNG

LXIV. An inner eccentric sub-Neptune and an outer sub-Neptune-mass candidate around BD+00 444 (TOI-2443)

¹ INAF – Osservatorio Astrofisico di Torino, Via Osservatorio 20, 10025 Pino Torinese, Italy
² Dipartimento di Fisica, Università degli studi di Roma “Tor Vergata”, Rome, Italy
³ Max-Planck-Institut für Astronomie, Heidelberg, Germany
⁴ Institute for Particle Physics and Astrophysics, ETH Zürich, Otto-Stern-Weg 5, 8093 Zürich, Switzerland
⁵ INAF – Osservatorio Astronomico di Roma, Monte Porzio Catone, Italy
⁶ INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123 Catania, Italy
⁷ INAF – Osservatorio Astronomico di Padova, Padova, Italy
⁸ Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA
⁹ George Mason University, 4400 University Drive, Fairfax, VA, 22030 USA
¹⁰ INAF – Osservatorio Astronomico di Palermo, Piazza del Parlamento 1, 90134 Palermo, Italy
¹¹ Dipartimento di Fisica e Chimica “Emilio Segrè”, Università di Palermo, Via Archirafi 36, Palermo, Italy
¹² Observatoire de Genéve, Université de Genéve, 1290 Versoix, Switzerland
¹³ INAF – Fundación Galileo Galilei, Rambla J. A. F. Pérez 7, 38712 Breña Baja, TF, Spain
¹⁴ Instituto de Astrofísica de Canarias (IAC), c/ Vía Láctea s/n, 38205, La Laguna (Tenerife), Canary Islands, Spain
¹⁵ Dipartimento di Fisica e Astronomia “Galileo Galilei”, Vicolo dell’Osservatorio 3, 35122 Padova, Italy

^★ Corresponding author; luca.naponiello@inaf.it

Received: 11 August 2024
Accepted: 13 November 2024

Abstract

Context. Super-Earths and sub-Neptunes are the most common types of planets outside the Solar System and likely represent the link between terrestrial planets and gas giants. Characterizing their physical and orbital properties and studying their multiplicity are key steps in testing and understanding their formation, migration, and evolution.

Aims. We examined the star BD+00 444 (GJ 105.5, TOI-2443; V = 9.5 mag; d = 23.9 pc) in depth, with the aim of characterizing and confirming the planetary nature of its small companion, the planet candidate TOI-2443.01, which was discovered by the TESS space telescope and subsequently validated by a follow-up statistical study.

Methods. We monitored BD+00 444 with the HARPS-N spectrograph for 1.5 years to search for planet-induced radial-velocity (RV) variations, and then analyzed the RV measurements jointly with TESS and ground-based photometry.

Results. We determined that the host is a quiet K5 V star with a radius of R_* = 0.631_−0.014^+0.013 R_⊕ and a mass of M_* = 0.642_−0.025^+0.026 M_⊙. We revealed that the sub-Neptune BD+00 444 b has a radius of R_b = 2.36 ± 0.05 R_⊕, a mass of M_b = 4.8 ± 1.1 M_⊕, and consequently a rather low-density value of ρ_b = 2.00_−0.45^+0.49 g cm⁻³, which makes it compatible with both an Earth-like rocky interior with a thin H-He atmosphere and a half-rocky, half-water composition with a small amount of H-He. With an orbital period of about 15.67 days and an equilibrium temperature of about 519 K, BD+00 444 b has an estimated transmission spectroscopy metric (TSM) of 159₋₃₁⁺⁴⁶, which makes it ideal for atmospheric follow-up with the James Webb Space Telescope. Notably, it is the second most eccentric inner transiting planet among those with well-determined eccentricities, with e = 0.302_−0.035^+0.051, and a mass of below 20 M_⊕. We estimated that tidal forces from the host star affect both the rotation and eccentricity of planet b, and strong tidal dissipation may signal intense volcanic activity. Furthermore, our analysis suggests the presence of a sub-Neptune-mass planet candidate, BD+00 444 c, which would have an orbital period of P_c = 96.6 ± 1.4 days and a minimum mass of M_c sin i = 9.3_−2.0^+1.8 M_⊕. With an equilibrium temperature of about 283 K, BD+00 444 c is inside the habitable zone; however, confirmation of this candidate would require further observations and stronger statistical evidence. We explored the formation and migration of both planets by means of population synthesis models, which reveal that both planets started their formation beyond the water snowline during the earliest phases of the life of their protoplanetary disk.