We report the detection of two new very light planets orbiting the low metallicityMdwarf Gl 581, already known to harbour a 15.7M closer-in planet (Bonfils et al. 2005b). The high radialvelocity precision reached with the HARPS spectrograph on the ESO 3.6-m telescope enabled these discoveries. The first planet, Gl 581 c, is a 5.1M super-Earth at a distance of 0.07AU from the star. Its mass is the smallest found so far for an exoplanet. At its separation from an M3 dwarf, the planet resides in the habitable zone of this low luminosity star. With a radius close to 1.5R, the planet is the closest Earth twin to date. The HARPS radial velocities also reveal a longer-period planetary companion of mass 8.2M, on a 84.4-d period orbit. Further measurements are planned to completely ascertain the 3rd planet, and a photometric followup will fully check the intrinsic stability of the star on long timescales. The two new very low-mass planets further support statistical trends already outlined in the literature: i) Small planets (Neptune mass and below) are more frequent than giant planets around M dwarfs (6 very low-mass detections against 3 Jovian planets). This result was significant at the 97% level before the detection of the two new Gl 581 planets (Bonfils et al. 2007), even without accounting for the poorer detection efficiency for lower-mass planets. ii) The fraction of detected Neptune (and lower-mass) planets around M dwarfs is much larger than the corresponding ratio for solar-type stars (Bonfils et al. 2006). The absolute numbers of detections are similar, but the number of surveyed solar-type stars is an order of magnitude larger. This may be an observational bias due to the lower mass of M-dwarf primaries, or truly reflects more frequent formation of Neptunemass planets around M dwarfs. The factual conclusion remains that Neptune-mass planets are easier to find around M dwarfs. Recent planet-formation simulations (Laughlin et al. 2004; Ida & Lin 2005) suggest that planet formation around lowmass primaries tends to produce lower mass planets, in the Uranus/Neptune domain. Formation of lower-mass planets is also favoured for solar-mass stars with metal-poor protostellar nebulae (Ida & Lin 2004; Benz et al. 2006)2. Gl 581 is a 0.3M metal-poor star, and its detected very light planets are thus just what was expected around this star. Additional detections of very-low mass planets will help understanding these 2 converging effects. From both our observational programmes and planet formation simulations, very low-mass planets seem more frequent than the previously found giant worlds. They will thus provide preferential targets for space photometric transit-search missions like COROT and Kepler, and for projects like Darwin and TPF-I/C looking for biotracers in the atmospheres of habitable planets. Acknowledgements. The authors thank the different observers from the other HARPS GTO sub-programmes who have also measured Gl 581.We would like to thank the Swiss National Science Foundation (FNRS) for its continuous support to this project. 2 Note, however, that there is no general consensus. Kornet et al. (2006) suggest that smaller-mass primaries have denser disks, which would favour giant planet formation. Gravitational instability might also form super-Earth planets around M dwarfs as well (Boss 2006). |