Internal rotation and buoyancy travel time of 60 gamma Doradus stars from uninterrupted TESS light curves spanning 352 days

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.