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The new planet finder for the Very Large Telescope (VLT), theSpectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE), just had itsfirst light in Paranal. A dedicated instrument for the direct detection ofplanets, SPHERE, is composed of a polametric camera in visible light, theZurich IMager POLarimeter (ZIMPOL), and two near-infrared sub-systems: theInfra-Red Dual-beam Imager and Spectrograph (IRDIS), a multi-purpose camera forimaging, polarimetry, and long-slit spectroscopy, and the integral fieldspectrograph (IFS), an integral field spectrograph. We present the resultsobtained from the analysis of data taken during the laboratory integration andvalidation phase, after the injection of synthetic planets. Since no continuousfield rotation could be performed in the laboratory, this analysis presentsresults obtained using reduction techniques that do not use the angulardifferential imaging (ADI) technique. To perform the simulations, we used theinstrumental point spread function (PSF) and model spectra of L and T-typeobjects scaled in contrast with respect to the host star. We evaluated theexpected error in astrometry and photometry as a function of the signal tonoise of companions, after spectral differential imaging (SDI) reduction forIRDIS and spectral deconvolution (SD) or principal component analysis (PCA)data reductions for IFS. We deduced from our analysis, for example, that$\beta$Picb, a 12~Myr old planet of $\sim$10~\MJ and semi-major axis of 9--10AU, would be detected with IRDIS with a photometric error of 0.16~mag and witha relative astrometric position error of 1.1~mas. With IFS, we could retrieve aspectrum with error bars of about 0.15~mag on each channel and astrometricrelative position error of 0.6~mas. For a fainter object such as HR8799d, a13~\MJ planet at a distance of 27~AU, IRDIS could obtain a relative astrometricerror of 3~mas.

Performance of the VLT Planet Finder SPHERE I. Photometry and astrometry precision with IRDIS and IFS in laboratory