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Small rocky planets seem to be very abundant around low-mass M-type stars.Their actual planetary population is however not yet precisely understood.Currently several surveys aim to expand the statistics with intensive detectioncampaigns, both photometric and spectroscopic. We analyse 106 spectroscopicHARPS-N observations of the active M0-type star GJ 685 taken over the past fiveyears. We combine these data with photometric measurements from differentobservatories to accurately model the stellar rotation and disentangle itssignals from genuine Doppler planetary signals in the RV data. We run an MCMCanalysis on the RV and activity indexes time series to model the planetary andstellar signals present in the data, applying Gaussian Process regressiontechnique to deal with the stellar activity signals. We identify three periodicsignals in the RV time series, with periods of 9, 24, and 18 d. Combining theanalyses of the photometry of the star with the activity indexes derived fromthe HARPS-N spectra, we identify the 18 d and 9 d signals as activity-related,corresponding to the stellar rotation period and its first harmonicrespectively. The 24 d signals shows no relations with any activity proxy, sowe identify it as a genuine planetary signal. We find the best-fit modeldescribing the Doppler signal of the newly-found planet, GJ 685\,b,corresponding to an orbital period $P_b = 24.160^{+0.061}_{-0.047}$ d and aminimum mass $M_P \sin i = 9.0^{+1.7}_{-1.8}$ M$_\oplus$. We also study asample of 70 RV-detected M-dwarf planets, and present new statistical evidenceof a difference in mass distribution between the populations of single- andmulti-planet systems, which can shed new light on the formation mechanisms oflow-mass planets around late-type stars.

The HADES RV Programme with HARPS-N at TNG XI. GJ 685 b: a warm super-Earth around an active M dwarf