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Lack of high-precision long-term continuous photometric data for largesamples of stars has prevented the large-scale exploration of pulsationalvariability in the OB star regime. As a result, the candidates for in-depthasteroseismic modelling remained limited to a few tens of dwarfs. The TESSnominal space mission has surveyed the southern sky, yielding continuous dataof at least 27 d for hundreds of OB stars. We aim to couple TESS data in thesouthern sky with spectroscopy to study the variability over mass andevolution. We focus mainly on the presence of coherent pulsation modes that mayor may not be present in the theoretical instability domains and unravel allfrequency behaviour in the amplitude spectra of the TESS data. We compose asample of 98 OB-type stars observed by TESS in Sectors 1-13 and with availablehigh-resolution spectroscopy gathered by the IACOB and OWN surveys. We presentthe short-cadence 2-min light curves of dozens of OB-type stars, that have oneor more spectra in the IACOB or OWN database. Based on these light curves andtheir Lomb-Scargle periodograms we perform variability classification andfrequency analysis, and place the stars in the spectroscopicHertzsprung-Russell diagram to interpret the variability in an evolutionarycontext. We deduce diverse origins of the variability found in all of the 98 OBstars in the TESS data. Among these we find several new variable stars,including three hybrid pulsators, three eclipsing binaries, high frequencymodes in a Be star, and potential heat-driven pulsations in two Oe stars. Weidentify stars for which future asteroseismic modelling is possible, providedmode identification is achieved. By comparing the position of the variables totheoretical instability strips we discuss the current shortcomings innon-adiabatic pulsation theory, and the distribution of pulsators in the upperHertzsprung-Russell diagram.

Variability of OB stars from TESS southern Sectors 1-13 and high-resolution IACOB and OWN spectroscopy