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The predicted width of the upper main sequence in stellar evolution modelsdepends on the empirical calibration of the convective overshooting parameter.Despite decades of discussions, its precise value is still unknown and furtherobservational constraints are required to gauge it. Based on a photometric andpreliminary asteroseismic analysis, we show that the mid B-type giant 18 Peg isone of the most evolved members of the rare class of slowly pulsating B-starsand, thus, bears tremendous potential to derive a tight lower limit for thewidth of the upper main sequence. In addition, 18 Peg turns out to be part of asingle-lined spectroscopic binary system with an eccentric orbit that isgreater than 6 years. Further spectroscopic and photometric monitoring and asophisticated asteroseismic investigation are required to exploit the fullpotential of this star as a benchmark object for stellar evolution theory.

The slowly pulsating B-star 18 Peg: A testbed for upper main sequence stellar evolution