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The formation scenario of extended counter-rotating stellar disks in galaxiesis still debated. In this paper, we study the S0 galaxy IC 719 known to hosttwo large-scale counter-rotating stellar disks in order to investigate theirformation mechanism. We exploit the large field of view and wavelength coverageof the Multi Unit Spectroscopic Explorer (MUSE) spectrograph to derivetwo-dimensional (2D) maps of the various properties of the counter-rotatingstellar disks, such as age, metallicity, kinematics, spatial distribution, thekinematical and chemical properties of the ionized gas, and the dust map. Dueto the large wavelength range, and in particular to the presence of the CalciumTriplet 8498, 8542, 8662\AA (CaT hereafter), the spectroscopic analysis allowsus to separate the two stellar components in great detail. This permits precisemeasurement of both the velocity and velocity dispersion of the two componentsas well as their spatial distribution. We derived a 2D map of the age andmetallicity of the two stellar components as well as the star formation rateand gas-phase metallicity from the ionized gas emission maps. The main stellardisk of the galaxy is kinematically hotter, older, thicker and with largerscale-length than the secondary disk. There is no doubt that the latter isstrongly linked to the ionized gas component: they have the same kinematics andsimilar vertical and radial spatial distribution. This result is in favor of agas accretion scenario over a binary merger scenario to explain the origin ofcounter-rotation in IC 719. One source of gas that may have contributed to theaccretion process is the cloud that surrounds IC 719.

Evidence for the formation of the young counter-rotating stellar disk from gas acquired by IC 719