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M dwarfs have been found to often have super-Earth planets with short orbitalperiods. Such stars are thus preferential targets in searches for rocky orocean planets in the solar neighbourhood. In a recent paper (Bonfils et al.2011), we announced the discovery of respectively 1 and 2 low mass planetsaround the M1.5V stars Gl433 and Gl667C. We found those planets with the HARPSspectrograph on the ESO~3.6-m telescope at La Silla Observatory, fromobservations obtained during the Guaranteed Time Observing program of thatinstrument. We have obtained additional HARPS observations of those two stars,for a total of respectively 67 and 179 Radial Velocity measurements for Gl433and Gl667C, and present here an orbital analysis of those extended data setsand our main conclusion about both planetary systems. One of the three planets,Gl667Cc, has a mass of only M2.sin(i)~4.25 M_earth and orbits in the centralhabitable zone of its host star. It receives just 10% less stellar energy fromGl667C than the Earth receives from the Sun. However planet evolution inhabitable zone can be very different if the host star is a M dwarf or asolar-like star, without necessarily questioning the presence of water. The twoother planets, Gl433b and Gl667Cb, both have M2.sin(i) of ~5.5 M_earth andperiods of ~7 days. The Radial Velocity measurements of both stars containlonger time scale signals, which we fit as longer period Keplerians. For Gl433that signal probably originates in a Magnetic Cycle, while a longer time spanwill be needed to conclude for Gl667C. The metallicity of Gl433 is close tosolar, while Gl667C is metal poor with [Fe/H] ~ -0.6. This reinforces therecent conclusion that the occurence of Super-Earth planets does not stronglycorrelate with stellar metallicity.

The HARPS search for southern extra-solar planets XXXV. Super-Earths around the M-dwarf neighbors Gl433 and Gl667C