Reduced observations of HD112429

We validate the pulsation frequencies from the TESS data up to S/N>=5.6, confirming recent reports in the literature that the classical criterion S/N>=4 does not suffice for space-based observations. We identify the pulsations as prograde dipole g modes and r-mode pulsations, and measure a near-core rotation rate of 1.536(3)d^-1^ and a buoyancy travel time {Pi}0 of 4190(50) s. These results are in agreement with the observed spectral line profile variations, which were qualitatively evaluated using a newly developed toy model.

We establish a set of conditions that have to be fulfilled for an asymptotic asteroseismic analysis of g-mode pulsators. In the case of HD112429, two TESS sectors of space photometry suffice. Although a detailed asteroseismic modelling analysis is not viable for g-mode pulsators with only short or sparse light curves of space photometry, it is possible to determine global asteroseismic quantities for a subset of these stars.

Thanks to the ongoing TESS mission, this will allow us to characterise many more stars than only those with years of data.