SPHERE is the planet finder for VLT. Direct observation of extrasolar planets allows (i) to complement the observations obtained with other techniques extending the search region to the outer part of planetary systems - we expect to discover some tens of planets with SPHERE providing a quantitative estimate of the frequency of giant planets in wide orbits over a range in stellar masses; and (ii) to characterize planets by obtaining spectroscopic and polarimetric data. Direct detection is extremely difficult due to the high contrast between the star and planet images. It requires to combine an extremely efficient adaptive optics, a coronagraph able to reduce the impact of diffraction, and a calibration technique able to suppress speckles due to the atmosphere and to the optics. SPHERE is a complex instrument made of a common path (which performs the first two functions) and three scientific channels (IRDIS, IFS and ZIMPOL) which implement the third function in different ways (angular, spectroscopic and polarimetric differential imaging), in addition to providing information useful to characterize planets. SPHERE is made by a large consortium including institutes in France, Italy, Germany, Switzerland, Netherland, and ESO. INAF is responsible of IFS, instrument control software, and have a major responsibility in the large GTO survey (260 nights). The instrument is now in the test phase at IPAG in Grenoble; PAE is foreseen next spring, and first light should be achieved during autumn 2013.