  Upcoming large-scale spectroscopic surveys such as WEAVE and 4MOST will
provide thousands of spectra of massive stars, which need to be analysed in an
efficient and homogeneous way. Studies on massive stars are usually based on
samples of a few hundred objects which pushes current spectroscopic analysis
tools to their limits because visual inspection is necessary to verify the
spectroscopic fit. The novel spectroscopic analysis pipeline takes advantage of
the statistics that large samples provide, and determines the model error to
account for imperfections in stellar atmosphere codes due to simplified, wrong
or missing physics. Considering observational plus model uncertainties improve
spectroscopic fits. The pipeline utilises the entire spectrum rather than
selected diagnostic lines allowing a wider range of temperature from B to early
O stars to be analysed. A small fraction of stars like peculiar, contaminated
or spectroscopic binaries require visual inspection, which are identified
through their larger uncertainties.
