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We disentangle two counter-rotating stellar components in NGC 4191 andcharacterize their physical properties (kinematics, morphology, age,metallicity, and abundance ratio). We performed a spectroscopic decompositionon integral field data to separate the contribution of two stellar componentsto the observed galaxy spectrum across the field of view. We also performed aphotometric decomposition, modelling the galaxy with a S\'ersic bulge and twoexponential disks of different scale length, with the aim of associating thesestructural components with the kinematic components. We measured the equivalentwidth of the absorption line indices on the best fit that represent thekinematic components and compared our measurements to the predictions ofstellar population models. We have evidence that the line-of-sight velocitydistributions (LOSVDs) are consistent with the presence of two distinctkinematic components. The combined information of the intensity of the LOSVDsand photometry allows us to associate the S\'ersic bulge and the outer diskwith the main kinematic component, and the inner disk with the secondarykinematic component. The two kinematic stellar components counter-rotate withrespect to each other. The main component is the most luminous and massive, andit rotates slower than the secondary component, which rotates along the samedirection as the ionized gas. We also found that the two kinematic componentshave the same solar metallicity and sub-solar abundance ratio, without thepresence of significant radial gradients. On the other hand, their ages showstrong negative gradients and the possible indication that the secondarycomponent is the youngest. We interpret our results in light of recentcosmological simulations and suggest gas accretion along two filaments as theformation mechanism of the stellar counter-rotating components in NGC 4191(Abridged).

The properties and the formation mechanism of the stellar counter-rotating components in NGC 4191