2021A&A...653A.114S

Context. The CARMENES exoplanet survey of M dwarfs has obtained more than 18 000 spectra of 329 nearby M dwarfs over the past five years as part of its guaranteed time observations (GTO) program.
Aims. We determine planet occurrence rates with the 71 stars from the GTO program for which we have more than 50 observations.
Methods. We use injection-and-retrieval experiments on the radial-velocity time series to measure detection probabilities. We include 27 planets in 21 planetary systems in our analysis.
Results. We find 0.06_–0.03^+0.04 giant planets (100M_⊕<M_plsini<1000M_⊕) per star in periods of up to 1000d, but due to a selection bias this number could be up to a factor of five lower in the whole 329-star sample. The upper limit for hot Jupiters (orbital period of less than 10d) is 0.03 planets per star, while the occurrence rate of planets with intermediate masses (10M_⊕<M_plsini<100M_⊕) is 0.18_–0.05^+0.07 planets per star. Less massive planets with 1M_⊕<M_plsini<10M_⊕ are very abundant, with an estimated rate of 1.32_–0.31^+0.33 planets per star for periods of up to 100d. When considering only late M dwarfs with masses M_*<0.34M_☉, planets more massive than 10M_⊕ become rare. Instead, low-mass planets with periods shorter than 10d are significantly overabundant.
Conclusions. For orbital periods shorter than 100d, our results confirm the known stellar mass dependences from the Kepler survey: M dwarfs host fewer giant planets and at least two times more planets with M_plsini<10M_⊕ than G-type stars. In contrast to previous results, planets around our sample of very low-mass stars have a higher occurrence rate in short-period orbits of less than 10d. Our results demonstrate the need to take into account host star masses in planet formation models.