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Fig. D.1.


Evolutionary tracks (solid) and isochrones (dashed) from Ekström et al. (2012). Three potential locations of B3 III stars are marked by filled shapes: 18 Peg as modeled by Nieva & Przybilla (2014, blue filled circle) as well as by Irrgang et al. (2016, gray triangle), and the generic calibration by Hohle et al. (2010, dark gray square), all discussed in Appendix C. The horizontal dash-dotted lines give the respective implied ranges of the intrinsic brightness of the Be star in HR 6819. The blue and dark gray lines assume that the apparent magnitude of the Be star is the same as that of a B3 III star as determined by Nieva & Przybilla (2014) and Hohle et al. (2010), respectively. Each pair of lines with the same color indicates a disk excess ΔV of −0.3 and −0.7 mag, respectively.

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