The TOI-2427 system: Two close-in planets orbiting a late K-dwarf star

This is the authors' abstract. We don't add key points for this paper.

Using high-precision photometry, NASA’s TESS space mission has discovered many intriguing transiting planet candidates. These discoveries require ground-based follow-up observations, including high-precision Doppler spectroscopy, to rule out false positive scenarios and measure the mass of the transiting planets. In this study, we present an intensive Doppler follow-up campaign of the TESS object of interest TOI-2427, carried out with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph to determine the mass of the previously validated transiting planet (TOI-2427 b) and search for additional orbiting companions. By analyzing TESS transit photometry alongside our HARPS radial velocity measurements, we spectroscopically confirmed the transiting planet TOI-2427 b, which orbits its host star every ∼ 1.3 d. We also discovered the presence of a second non-transiting planetary companion with an orbital period of ∼ 5.15 d, which is very close to four times the orbital period of the inner transiting planet. We found that TOI-2427 b is a short-period, high-density super-Earth with a mass of M b = 5.69 −0.50 +0.51 M ⊕ and a radius of R b = 1.64 −0.11 +0.12 R ⊕ , implying a mean density of ρ b = 7.1 −0.4 +0.8 g cm −3 . Its interior seems to be composed of a predominantly iron core and a silicate mantle and crust. Despite its high density, it is unlikely that TOI-2427 b can sustain any atmosphere composed of lighter gases; however, it could still retain heavier gases. The outer non-transiting planet TOI-2427 c has a minimum mass of M c sin i c = 6.46 −0.78 +0.79 M ⊕ . Assuming that TOI-2427 b and c are coplanar, a statistical analysis suggests that planets with a mass of ∼ 6.5 M ⊕ tend to have radii around 2.7 −0.8 +1.1 R ⊕ . This would place TOI-2457 c near the sub-Neptune regime, while also leaving open the possibility of it being a super-Earth.