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Asteroseismic modelling of the internal structure of main-sequence stars bornwith a convective core has so far been based on homogeneous analyses of spacephotometric Kepler light curves of 4 years duration, to which most oftenincomplete inhomogeneously deduced spectroscopic information was added to breakdegeneracies. We composed a sample of 111 dwarf gravity-mode pulsators observedby the Kepler space telescope whose light curves allowed for determination oftheir near-core rotation rates. For this sample we assembled HERMEShigh-resolution optical spectroscopy at the 1.2-m Mercator telescope. Ourspectroscopic information offers additional observational input to also modelthe envelope layers of these non-radially pulsating dwarfs. We determinedstellar parameters and surface abundances in a homogeneous way from atmosphericanalysis with spectrum normalisation based on a new machine learning tool. Ourresults suggest a systematic overestimation of [M/H] in the literature for thestudied F-type dwarfs, presumably due to normalisation limitations caused bythe dense line spectrum of these rotating stars. CNO-surface abundances werefound to be uncorrelated with the rotation properties of the F-type stars. Forthe B-type stars, we find a hint of deep mixing from C and O abundance ratios;N abundances have too large uncertainties to reveal a correlation with therotation of the stars. Our spectroscopic stellar parameters and abundancedeterminations allow for future joint spectroscopic, astrometric (Gaia), andasteroseismic modelling of this legacy sample of gravity-mode pulsators, withthe aim to improve our understanding of transport processes in thecore-hydrogen burning phase of stellar evolution.

A homogeneous spectroscopic analysis of a Kepler legacy sample of dwarfs for gravity-mode asteroseismology