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The TESS space mission provides us with high-precision photometricobservations of bright stars over more than 70% of the entire sky, allowing usto revisit and characterise well-known stars. We aim to conduct anasteroseismic analysis of the gamma Doradus star HD112429 using both theavailable ground-based spectroscopy and TESS photometry, and assess theconditions required to measure the near-core rotation rate and buoyancy traveltime. We collect and reduce the available five sectors of short-cadence TESSphotometry of this star, as well as 672 legacy observations from six medium- tohigh-resolution ground-based spectrographs. We determine the stellar pulsationfrequencies from both data sets using iterative prewhitening, do asymptotic gmode modelling of the star and investigate the corresponding spectral lineprofile variations using the pixel-by-pixel method. We validate the pulsationfrequencies from the TESS data up to $S/N \geq 5.6$, confirming recent reportsin the literature that the classical criterion $S/N \geq 4$ does not sufficefor space-based observations. We identify the pulsations as prograde dipole gmodes 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 inagreement with the observed spectral line profile variations, which werequalitatively evaluated using a newly developed toy model. We establish a setof conditions that have to be fulfilled for an asymptotic asteroseismicanalysis of g-mode pulsators. In the case of HD112429, two TESS sectors ofspace photometry suffice. Although a detailed asteroseismic modelling analysisis not viable for g-mode pulsators with only short or sparse light curves ofspace photometry, we find that it is possible to determine global asteroseismicquantities for a subset of these stars. (abbreviated.)

The near-core rotation of HD 112429: a gamma Doradus star with TESS photometry and legacy spectroscopy