The CARMENES search for exoplanets around M dwarfs

Aims. Previous estimates of planet occurrence rates in the CARMENES survey indicated increased numbers of planets on short orbits for M dwarfs with masses below 0.34M ⊙ . Here we focused on the lowest-mass stars in the survey, comprising 15 inactive targets with masses under 0.16 M ⊙ . Methods. To correct for detection biases, we determined detection sensitivity maps for individual targets and the entire sample. Using Monte Carlo simulations, we estimated planet occurrence rates for orbital periods of 1 d to 100 d and minimum masses from 0.5 M ⊕ to 10M ⊕ . We also compared the actual sample of known planets to model predictions. Results. The radial velocity (RV) data from CARMENES reveal four new planets around three stars in our sample, namely G 268– 110 b, G 261–6 b, and G 192–15 b and c. All three b planets have minimum masses of 1.03–1.52 M ⊕ and orbital periods of 1.43–5.45 d, while G 192–15 c is a 14.3 M ⊕ planet on a wide, eccentric orbit with P ≈ 1218 d and e ≈ 0.68. Our occurrence rates suggest considerable dependencies with respect to stellar masses. For planets below 3 M ⊕ we found rates consistent with one planet per star across all investigated periods, but the rates decrease almost by an order of magnitude for larger planet masses up to 10 M ⊕ . Compared to previous studies, low-mass stars tend to harbor more planets with P < 10 d. We also demonstrate that synthetic planet populations based on the standard core accretion scenario predict slightly more massive planets on wider orbits than observed. Conclusions. Our findings confirm that planet occurrence rates vary with stellar masses even among M dwarfs, as we found more planets with lower masses and on shorter orbits in our subsample of very low-mass stars compared to more massive M dwarfs. Therefore, we emphasize the need for additional differentiation in future studies.