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Studying the stellar kinematics of galaxies is a key tool in thereconstruction of their evolution. However, the current measurements of thestellar kinematics are complicated by several factors, including dustextinction and the presence of multiple stellar populations. We use integralfield spectroscopic data of four galaxies from the TIMER survey to explore andcompare the kinematics measured in different spectral regions that aresensitive to distinct stellar populations. We derive the line-of-sight velocityand velocity dispersion of both a young (<2 Gyr) and an old stellar populationfrom the spectral regions around the H$\beta$ line and the Ca II Triplet. Inaddition we obtain colour excess, mean age, and metallicity. We report acorrelation of the colour excess with the difference in the kinematicparameters of the H$\beta$ line and the Ca II Triplet range, which aredominated by young and old stellar populations, respectively. Young stellarpopulations, located primarily in nuclear rings, have higher velocitydispersions than old ones. These differences in the rings are typically 10 km/sin velocity dispersion, but up to a mean value of 24 km/s in the most extremecase. Trends with age exist in the nuclear rings but are less significant thanthose with dust extinction. We report different degrees of correlation of thesetrends among the galaxies in the sample, which are related to the size of theVoronoi bins in their rings. No clear trends for the difference ofline-of-sight velocity are observed. The absence of these trends can beexplained as a consequence of the masking process of the H$\beta$ line duringthe kinematic extraction, as confirmed by dedicated simulations. Our studydemonstrates that kinematic differences caused by different stellar populationscan be identified in the central regions of nearby galaxies even fromintermediate resolution spectroscopy.

The kinematics of young and old stellar populations in nuclear rings of MUSE TIMER galaxies