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Spectroscopic data are necessary to break degeneracies in asteroseismicmodelling of the interior structure in high- and intermediate-mass stars. Wederive precise photospheric stellar parameters for a sample of 166 B-type starswith TESS light curves, suitable for detailed asteroseismic studies, through ahomogeneous spectroscopic analysis. The variability types of these stars areclassified based on all currently available TESS sectors. We obtainedhigh-resolution spectra for all 166 targets with the FEROS spectrograph in thecontext of a large program. The Least-Squares Deconvolution method is employedto investigate spectral line profile variability and to detect binary systems.We identify 26 spectroscopic double-lined binaries; the remainder of the sampleare 42 supergiants in the LMC galaxy and 98 Galactic stars. The spectra of theGalactic stars are analysed with the zeta-Payne, a machine learning-basedspectrum analysis algorithm. We determine the five main surface parameters withaverage formal precisions of 70 K (Teff), 0.03 dex (logg), 0.07 dex ([M/H]), 8km/s (vsini), and 0.7 km/s (vmicro). The average internal uncertainties we findfor FEROS spectra with our spectrum analysis method are 430 K (Teff), 0.12 dex(logg), 0.13 dex ([M/H]), 12 km/s (vsini), and 2 km/s (vmicro). We findspectroscopic evidence that eight of the 98 Galactic targets are fast rotatingg-mode pulsators occurring in between the slowly pulsating B (SPB) stars anddelta Scuti instability strips. The g-mode frequencies of these pulsators areshifted to relatively high frequency values due to their rotation. Theirapparently too low Teff relative to the SPB instability region can in mostcases be explained by the gravity darkening effect. We also discover 13 newHgMn stars of which only one is found in a spectroscopic binary, resulting in abiased and therefore unreliable low binary rate of only 8%.

Analysis of high-resolution FEROS spectroscopy for a sample of variable B-type stars assembled from TESS photometry