The improvement of stellar structure and evolution models using asteroseismology relies on determining the best match between the theoretical and observed stellar pulsations. Gravity mode pulsators with convective cores, such as the slowly pulsating B-type stars, are ideal laboratories for studying and constraining convective core sizes and boundary mixing – both of which provide one of the largest uncertainties in the stellar structure and evolution models of high mass stars. Here we introduce a new methodology for comparing models and observations based on Mahalanobis distances, and take the reader on a journey showing how including information from spectroscopy and Gaia astrometry in addition to the seismic information impacts the forward modelling.