A multi-planetary system orbiting the early-M dwarf TOI-1238

Abstract

Context. The number of super-Earth and Earth-mass planet discoveries has increased significantly in the last two decades thanks to the Doppler radial velocity and planetary transit observing techniques. Either technique can detect planet candidates on its own, but the power of a combined photometric and spectroscopic analysis is unique for an insightful characterization of the planets, which in turn has repercussions for our understanding of the architecture of planetary systems and, therefore, their formation and evolution. Aims. Two transiting planet candidates with super-Earth radii around the nearby (d = 70.64 ± 0.06 pc) K7–M0 dwarf star TOI-1238 were announced by NASA’s Transiting Exoplanet Survey Satellite (TESS), which observed the field of TOI-1238 in four different sectors. We aim to validate their planetary nature using precise radial velocities taken with the CARMENES spectrograph. Methods. We obtained 55 CARMENES radial velocity measurements that span the 11 months between 9 May 2020 and 5 April 2021. For a better characterization of the parent star’s activity, we also collected contemporaneous optical photometric observations at the Joan Oró and Sierra Nevada observatories and retrieved archival photometry from the literature. We performed a combined TESS+CARMENES photometric and spectroscopic analysis by including Gaussian processes and Keplerian orbits to account for the stellar activity and planetary signals simultaneously. Results. We estimate that TOI-1238 has a rotation period of 40 ± 5 d based on photometric and spectroscopic data. The combined analysis confirms the discovery of two transiting planets, TOI-1238 b and c, with orbital periods of 0.764597−0.000011+0.000013 d and 3.294736−0.000036+0.000034 d, masses of 3.76−1.07+1.15 M⊕ and 8.32−1.88+1.90 M⊕, and radii of 1.21−0.10+0.11 R⊕ and 2.11−0.14+0.14 R⊕. They orbit their parent star at semimajor axes of 0.0137 ± 0.0004 au and 0.036 ± 0.001 au, respectively.The two planets are placed on opposite sides of the radius valley for M dwarfs and lie between the star and the inner border of TOI-1238’s habitable zone. The inner super-Earth TOI-1238 b is one of the densest ultra-short-period planets ever discovered (ρ = 11.7−3.4+4.2 g cm−3). The CARMENES data also reveal the presence of an outer, non-transiting, more massive companion with an orbital period and radial velocity amplitude of ≥600 d and ≥70 m s−1, which implies a likely mass of M ≥ 2 √(1− e2) MJup and a separation ≥1.1 au from its parent star.

Scattering of Giant Planets and Implications for the Origin of the Hierarchical and Eccentric Two-planet System GJ 1148

“…Introduction M dwarf stars have been a primary target in the search for exoplanets in recent years due to the large number of them in the galaxy. Their lower masses and luminosities compared to Sun-like stars make the planets in the so-called habitable zone (HZ) easier to detect with larger radial-velocity (RV) signal and shorter orbital period (Trifonov et al 2020;Sabotta et al 2021;González-Álvarez et al 2022). Current observations show that most planets orbiting around M-dwarfs have masses equivalent to a few Earth to Neptune masses (Trifonov et al 2020;González-Álvarez et al 2022), while Jupiter-mass planets are observed more frequently around Sun-like or more massive stars (Fischer & Valenti 2005;Reffert et al 2015).…”

“…Their lower masses and luminosities compared to Sun-like stars make the planets in the so-called habitable zone (HZ) easier to detect with larger radial-velocity (RV) signal and shorter orbital period (Trifonov et al 2020;Sabotta et al 2021;González-Álvarez et al 2022). Current observations show that most planets orbiting around M-dwarfs have masses equivalent to a few Earth to Neptune masses (Trifonov et al 2020;González-Álvarez et al 2022), while Jupiter-mass planets are observed more frequently around Sun-like or more massive stars (Fischer & Valenti 2005;Reffert et al 2015). GJ 1148, GJ 876 (Rivera et al 2010;Nelson et al 2016;Millholland et al 2018), and GJ 317 (Johnson et al 2007) are three unusual M-dwarf systems that have massive planets, whose formation is difficult to explain by the core-accretion theory of planet formation (Laughlin et al 2004;Morales et al 2019).…”