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The CoRoT satellite has provided high-precision photometric light curves formore than 163,000 stars and found several hundreds of transiting systemscompatible with a planetary scenario. If ground-based velocimetric observationsare the best way to identify the actual planets among many possibleconfigurations of eclipsing binary systems, recent transit surveys have shownthat it is not always within reach of the radial-velocity detection limits. Inthis paper, we present a transiting exoplanet candidate discovered by CoRoTwhose nature cannot be established from ground-based observations, and whereextensive analyses are used to validate the planet scenario. They are based onobserving constraints from radial-velocity spectroscopy, adaptive opticsimaging and the CoRoT transit shape, as well as from priors on stellarpopulations, planet and multiple stellar systems frequency. We use the fullyBayesian approach developed in the PASTIS analysis software, and conclude thatthe planet scenario is at least 1400 times more probable than any other falsepositive scenario. The primary star is a metallic solar-like dwarf, with Ms =1.099+-0.049 Msun and Rs = 1.136 (+0.038,-0.090) Rsun . The validated planethas a radius of Rp = 4.88 (+0.17,-0.39) RE and mass less than 49 ME. Its meandensity is smaller than 2.56 g/cm^3 and orbital period is 9.7566+-0.0012 days.This object, called CoRoT-22 b, adds to a large number of validated Keplerplanets. These planets do not have a proper measurement of the mass but allowstatistical characterization of the exoplanet population.

CoRoT-22 b: a validated 4.9 RE exoplanet in 10-day orbit