Figure 4
![The high-mass IMF index, α3, as a function of the global cluster metallicity, [Fe/H]. Symbols and lines as in Figs 2 and 3. NGC 3603, Arches and Wd1 have about solar metallicity. For R136 [Fe/H] ≈−0.48 is adopted, a typical value for the LMC. The data suggest the IMF to become less top heavy with increasing cluster metallicity, having the canonical value (α3= 2.3) above [Fe/H] =−0.5.](https://oup.silverchair-cdn.com/oup/backfile/Content_public/Journal/mnras/422/3/10.1111_j.1365-2966.2012.20767.x/1/mnras0422-2246-f4.jpeg?Expires=1750279873&Signature=WTfHW3ENX7b6wLW90wp92U3l0Gxv3bxyqRP99OT-tgmWCUbrJeAsSGnDAlZO7nWTFX3cAbLLU7OkZyv-Uyi-CB9khgXPdT6OoAADor9a65Y5QXxb1R4ybOe5tpRfxRGb93Rjo8HYv0aZpvnD-IdTs98BUB1tbtv1A4wdIp7HoXQe8bHqnuqfQDOTOgdP4-bXYgQHp7wEBOpPY7lcWGWY6UHCV70Pz63HaiHuEYLH8X2XeGbZ4--PGX0kjjEJGr26mhvBVimA7AdZd7kDIGVImEs8CCSRsmlEYZIyTwfM7t2iNcFdxqt1w~7yoeeIAy7cM9WUCwu-9Ih1HNZm3H9wXg__&Key-Pair-Id=APKAIE5G5CRDK6RD3PGA)
The high-mass IMF index, α3, as a function of the global cluster metallicity, [Fe/H]. Symbols and lines as in Figs 2 and 3. NGC 3603, Arches and Wd1 have about solar metallicity. For R136 [Fe/H] ≈−0.48 is adopted, a typical value for the LMC. The data suggest the IMF to become less top heavy with increasing cluster metallicity, having the canonical value (α3= 2.3) above [Fe/H] =−0.5.
