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We report on the results of an 8-year survey carried out at the La SillaObservatory with the HARPS spectrograph to detect and characterize planets inthe super-Earth and Neptune mass regime. The size of our star sample and theprecision achieved with HARPS have allowed the detection of a sufficientlylarge number of low-mass planets to study the statistical properties of theirorbital elements, the correlation of the host-star metallicity with the planetmasses, as well as the occurrence rate of planetary systems around solar-typestars. A robust estimate of the frequency of systems shows that more than 50%of solar-type stars harbor at least one planet of any mass and with period upto 100 days. Different properties are observed for the population of planetsless massive than about 30M-Earth compared to the population of gaseous giantplanets. The mass distribution of Super-Earths and Neptune-mass planets (SEN)is strongly increasing between 30 and 15M-Earth. The SEN occurence rate doesnot exhibit a preference for metal rich stars. Most of the SEN planets belongto multi-planetary systems. The orbital eccentricities of the SEN planets seemslimited to 0.45. At the opposite, the occurence rate of gaseous giant planetsis growing with the logarithm of the period, and is strongly increasing withthe host-star metallicity. About 14% of solar-type stars have a planetarycompanion more massive than 50M-Earth? on an orbit with a period shorter than10 years. Orbital eccentricities of giant planets are observed up to 0.9 andbeyond. The precision of HARPS-type spectrographs opens the possibility todetect planets in the habitable zone of solar-type stars. Identification of asignificant number of super-Earths orbiting solar-type of the Sun vicinity isachieved by Doppler spectroscopy. 37 newly discovered planets are announced inthe Appendix of this paper, among which 15 Super-Earths.

The HARPS search for southern extra-solar planets XXXIV. Occurrence,  mass distribution and orbital properties of super-Earths and Neptune-mass  planets