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As part of the ongoing effort to characterize the low-mass (sub)stellarpopulation in a sample of massive young clusters, we have targeted the ~2 Myrold cluster NGC 2244. The distance to NGC 2244 from Gaia DR2 parallaxes is 1.59kpc, with errors of 1% (statistical) and 11% (systematic). We used theFlamingos-2 near-infrared camera at the Gemini-South telescope for deepmulti-band imaging of the central portion of the cluster (~2.4pc^2). Wedetermined membership in a statistical manner, through a comparison of thecluster's color-magnitude diagram to that of a control field. Masses andextinctions of the candidate members are then calculated with the help ofevolutionary models, leading to the first initial mass function (IMF) of thecluster extending into the substellar regime, with the 90\% completeness limitaround 0.02 Msun. The IMF is well represented by a broken power law (dN/dM\propto M^{-alpha}), with a break at ~0.4 Msun. The slope on the high mass side(0.4 - 7 Msun) is alpha=2.12+-0.08, close to the standard Salpeter slope. Inthe low-mass range (0.02 - 0.4 Msun), we find a slope alpha=1.03+-0.02, whichis at the high end of the typical values obtained in nearby star-formingregions (alpha=0.5-1.0), but still in agreement within the uncertainties. Ourresults reveal no clear evidence for variations in the formation efficiency ofbrown dwarfs and very low-mass stars due to the presence of OB stars, or for achange in stellar densities. Our finding rules out photoevaporation andfragmentation of infalling filaments as substantial pathways for brown dwarfformation.

Looking deep into the Rosette Nebula's heart: the (sub)stellar content of the massive young cluster NGC 2244