Rubino, M.M.RubinoPizzella, A.A.PizzellaMorelli, L.L.MorelliCoccato, L.L.CoccatoPortaluri, E.E.PortaluriDebattista, V. P.V. P.DebattistaCorsini, E. M.E. M.CorsiniDalla Bonta, E.E.Dalla Bonta2025-12-302025-12-3020211432-0746https://hdl.handle.net/20.500.12740/23942Context. In recent years integral-field spectroscopic surveys have revealed that the presence of kinematically decoupled stellar components is not a rare phenomenon in nearby galaxies. However, complete statistics are still lacking because they depend on the detection limit of these objects. Aims. We investigate the kinematic signatures of two large-scale counter-rotating stellar disks in mock integral-field spectroscopic data to address their detection limits as a function of the galaxy properties and instrumental setup. Methods. We built a set of mock data of two large-scale counter-rotating stellar disks as if they were observed with the Multi Unit Spectroscopic Explorer (MUSE). We accounted for different photometric, kinematic, and stellar population properties of the two counter-rotating components as a function of galaxy inclination. We extracted the stellar kinematics in the wavelength region of the calcium triplet absorption lines by adopting a Gauss-Hermite (GH) parameterization of the line-of-sight velocity distribution (LOSVD). Results. We confirm that the strongest signature of the presence of two counter-rotating stellar disks is the symmetric double peak in the velocity dispersion map, already known as the 2 sigma feature. The size, shape, and slope of the 2 sigma peak strongly depend on the velocity separation and relative light contribution of the two counter-rotating stellar disks. When the 2 sigma peak is difficult to detect due to the low signal-to-noise ratio of the data, the large-scale structure in the h(3) map can be used as a diagnostic for strong and weak counter-rotation. The counter-rotating kinematic signatures become fainter at lower viewing angles as an effect of the smaller projected velocity separation between the two counter-rotating components. We confirm that the observed frequency of 2 sigma galaxies represents only a lower limit of the stellar counter-rotation phenomenon. Conclusions. The parameterization with a single GH function does not provide a good description of the LOSVD in the presence of strong counter-rotation. However, using GH parametric solutions is a practical way to reveal the large-scale counter-rotating stellar disks and could be used to detect faint counter-rotating components to improve the statistics of stellar counter-rotation.Acceso Abiertogalaxieskinematics and dynamicsgalaxiesstructuregalaxiesstellar contentgalaxiesindividualIC 719galaxiesspiralgalaxiesevolutionhttp://dx.doi.org/10.1051/0004-6361/202140702