[https://doi.org/10.1051/0004-6361:20030622]
[https://doi.org/10.1051/0004-6361:20020127]
[https://doi.org/10.1051/0004-6361/201322953]
[https://doi.org/10.1051/0004-6361:20031606]
[https://doi.org/10.1051/0004-6361:20078184]
[https://doi.org/10.1051/0004-6361/201015020]
[https://doi.org/10.1051/0004-6361:20065427]
Fig. 12
Figure to replace Fig. 10 in Moehler et al. (1995, M 15). The resulting masses for the stars in M 15 (Table 2c and d [original paper, Table 10 here]), NGC 6752 (Moehler et al. 1994), M 5, M 92, NGC 288 (Crocker et al. 1988), and NGC 6397 (de Boer et al. 1994b) plotted against Teff. The solid line represents a ZAHB model taken from Dorman et al. (1991) for [Fe/H] = −2.26 (YMS = 0.246, and [O/Fe] = 0.75). The short dashed line represents an extension of the ZAHB towards higher temperatures taken from Sweigart (1987) for YMS = 0.20 and ZMS = 10-4.
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