Description: Electronic versions of Table A.1 and A.2 from the Appendix of Garcia et al. (2022b), as well as all analysed g-mode period-spacing patterns from this work. Abstract: Context. Gamma Doradus (hereafter gamma Dor) stars are gravity-mode pulsators whose periods carry information about the internal structure of the star. These periods are especially sensitive to the internal rotation and chemical mixing, two processes that are currently not well constrained in the theory of stellar evolution. Aims. We aim to identify the pulsation modes and deduce the internal rotation and buoyancy travel time for 106 gamma Dor stars observed by the TESS mission in its southern continuous viewing zone (hereafter S-CVZ). We rely on 140 previously detected period-spacing patterns, that is, series of (near-)consecutive pulsation mode periods. Methods. We used the asymptotic expression to compute gravity-mode frequencies for ranges of the rotation rate and buoyancy travel time that cover the physical range in γ Dor stars. Those frequencies were fitted to the observed period-spacing patterns by minimizing a custom cost function. The effects of rotation were evaluated using the traditional approximation of rotation, using the stellar pulsation code GYRE. Results. We obtained the pulsation mode identification, internal rotation and buoyancy travel time for 60 TESS gamma Dor stars. For the remaining 46 targets, the detected patterns are either too short or contained too many missing modes for unambiguous mode identification, and longer light curves are required. For the successfully analysed stars, we found that period-spacing patterns from 1-yr long TESS light curves can constrain the internal rotation and buoyancy travel time to a precision of 0.03 d^{−1} and 400s, respectively, which is about half as precise as literature results based on 4-yr Kepler light curves of gamma Dor stars.

The research leading to these results has received funding from the the KU\,Leuven Research Council (grant C16/18/005: PARADISE) and from the BELgian federal Science Policy Office (BELSPO) through PRODEX grants for the Gaia and PLATO space missions. TVR gratefully acknowledges support from the Research Foundation Flanders (FWO) under grant agreement N$^\circ$12ZB620N.