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We use deep  Hubble Space Telescope  photometry of the rich, young (∼20‐ to 45‐Myr old) star cluster NGC 1818 in the Large Magellanic Cloud to derive its stellar mass function (MF) down to  ∼0.15 M ⊙  . This represents the deepest robust MF thus far obtained for a stellar system in an extragalactic, low‐metallicity  ([Fe/H]≃−0.4 dex)  environment. Combining our results with the published MF for masses above  1.0 M ⊙  , we obtain a complete present‐day MF. This is a good representation of the cluster's initial MF (IMF), particularly at low masses, because our observations are centred on the cluster's uncrowded half‐mass radius. Therefore, stellar and dynamical evolution of the cluster will not have affected the low‐mass stars significantly. The NGC 1818 IMF is well described by both a lognormal and a broken power‐law distribution with slopes of  Γ= 0.46 ± 0.10  and  Γ≃−1.35  (Salpeter‐like) for masses in the range from 0.15 to  0.8 M ⊙   and greater than  0.8 M ⊙  , respectively. Within the uncertainties, the NGC 1818 IMF is fully consistent with both the Kroupa solar neighbourhood and the Chabrier lognormal mass distributions.

The initial mass function of the rich young cluster NGC 1818 in the Large Magellanic Cloud