5508 20230120150000.0 10.1051/0004-6361/202142921 DOI SCART-2021-0160 Van Reeth, T. The near-core rotation of HD112429: a γ Doradus star with TESS photometry and legacy spectroscopy 2022 Context. The TESS space mission provides us with high-precision photometric observations of large numbers of bright stars over more than 70% of the entire sky, allowing us to revisit and characterise well-known stars. Aims. We aim to conduct an asteroseismic analysis of the γ Doradus (γ Dor) star HD 112429 using both the available ground-based spectroscopy and TESS photometry, and assess the conditions required to measure the near-core rotation rate and buoyancy travel time. Methods. We collect and reduce the available five sectors of short-cadence TESS photometry of this star, as well as 672 legacy observations from six medium- to high-resolution ground-based spectrographs. We determine the stellar pulsation frequencies from both data sets using iterative prewhitening, do asymptotic g-mode modelling of the star and investigate the corresponding spectral line profile variations using the pixel-by-pixel method. Results. 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 Π 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 HD 112429, two TESS sectors of space photometry suffice. Conclusions. 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. NO asteroseismology methods: observational stars: variables: general stars: oscillations (including pulsations) stars: individual: HD11242 De Cat, P. Van Beeck, J. Prat, V. Wright, D.J. Lehmann, H. Chené, A.-N. Kambe, E. Yang, S.L.S. Gentile, G. Joos, M. Astronomy & Astrophysics 662 2022 1--15 (id. A58) peter.decat@observatoire.be 2134055 http://publi2-as.oma.be/record/5508/files/VanReeth2022_AA662_A58.pdf 3386 http://publi2-as.oma.be/record/5508/files/VanReeth2022_AA662_A58.gif?subformat=icon icon 6829 http://publi2-as.oma.be/record/5508/files/VanReeth2022_AA662_A58.jpg?subformat=icon-180 icon-180 https://ui.adsabs.harvard.edu/abs/2022A%26A...662A..58V/abstract published in REFERD