Fig. 6
Empirical mass-loss rate versus luminosity for the M 31 late-type WN star sample. The thick lines show the least square fits for the stars with XH ≈ 0.2 and XH ≈ 0.5, respectively. For comparison, the relations from Nugis & Lamers (2000) are also shown as dashed lines. The gray symbols are the late-type WN stars near the Galactic center from Martins et al. (2008); Liermann et al. (2010) and Oskinova et al. (2013).
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