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Caption: Fig. 13.
Same as Fig. 10, but showing the effect of tilting the Scalo IMF, i.e., making it steeper by adding a constant β = 1.69 to the power‐law index in each segment. Results are also shown for a Miller‐Scalo IMF, which shows the opposite bias in that it contains more high‐mass stars than the Scalo IMF.
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