  The CoRoT satellite has provided high-precision photometric light curves for
more than 163,000 stars and found several hundreds of transiting systems
compatible with a planetary scenario. If ground-based velocimetric observations
are the best way to identify the actual planets among many possible
configurations of eclipsing binary systems, recent transit surveys have shown
that it is not always within reach of the radial-velocity detection limits. In
this paper, we present a transiting exoplanet candidate discovered by CoRoT
whose nature cannot be established from ground-based observations, and where
extensive analyses are used to validate the planet scenario. They are based on
observing constraints from radial-velocity spectroscopy, adaptive optics
imaging and the CoRoT transit shape, as well as from priors on stellar
populations, planet and multiple stellar systems frequency. We use the fully
Bayesian approach developed in the PASTIS analysis software, and conclude that
the planet scenario is at least 1400 times more probable than any other false
positive 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 planet
has a radius of Rp = 4.88 (+0.17,-0.39) RE and mass less than 49 ME. Its mean
density 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 Kepler
planets. These planets do not have a proper measurement of the mass but allow
statistical characterization of the exoplanet population.
