The dominant formation channel of brown dwarfs (BDs) is not well constrained yet and a promising way to discriminate between scenarios consists of testing environment-dependent efficiency in forming BDs. So far, the outcome of star formation, studied through the initial mass function, has been found to be very similar in all clusters that have been studied. We aim to characterize the low-mass (sub)stellar population of the central portion (2.4pc^2^) of the ~2Myr old cluster NGC 2244 using near-infrared spectroscopy. By studying this cluster, characterized by a low stellar density and numerous OB stars, we aim to explore the effect that OB stars may have on the production of BDs. We obtained near-infrared HK spectroscopy of 85 faint candidate members of NGC 2244. We derived the spectral type and extinction by comparison with spectral templates. We evaluated cluster membership using three gravity-sensitive spectral indices based on the shape of the H-band. Furthermore, we evaluated the infrared excess from Spitzer of all the candidate members of the cluster. Finally, we estimated the mass of all the candidate members of the cluster and derived the initial mass function, star-to-BD number ratio and disk fraction. The initial mass function is well represented by a power law (dN/dM {prop.to} M^-alpha^) below 0.4M_{sun}_, with a slope alpha=0.7-1.1 depending on the fitted mass range. We calculated a star-to-BD number ratio of 2.2-2.8. We find the low-mass population of NGC 2244 to be consistent with nearby star- forming regions, although it is at the high end of BD production. We find BDs in NGC 2244 to be, on average, closer to OB stars than to low-mass stars, which could potentially be the first piece evidence that OB stars affect the formation of BDs. We find a disk fraction of all the members with a spectral type later than K0 of 39+/-9% which is lower than typical values found in nearby star-forming regions of similar ages.

KMOS/VLT spectra and parameters of 34 candidate members of NGC 2244. The data provided are the reduced, wavelength-calibrated, telluric corrected HK bands 1-d spectra. The spectra are given in fits format and are not corrected for extinction. We also provide the full list of candidate members used in this work.

Financial support from the Severo Ochoa grant CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033

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