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Images obtained with the Gemini Multi-Object Spectrograph on Gemini South areused to examine the photometric properties and spatial distributions of mainsequence (MS) and pre-main sequence (PMS) objects in the star cluster NGC 2401.The data sample several magnitudes fainter than previous studies, and a largepopulation of candidate PMS (cPMS) stars are identified. The cPMS stars aretraced out to 2.4 arcmin from the cluster center, and have a flatter spatialdistribution than the brightest MS stars near the cluster center. Theluminosity function of all MS and candidate PMS stars can be matched by a modelthat assumes a solar neighborhood mass function, suggesting that NGC 2401 hasnot yet shed significant numbers of members with masses in excess of 0.5 solar.The frequency of wide binaries among the MS stars is ~3 times higher than amongthe cPMS stars. It is argued that the difference in the spatial distributionsof MS and PMS objects is not the consequence of secular dynamical evolution orstructural evolution driven by near-catastrophic mass loss. Rather, it issuggested that the different spatial distributions of these objects is thefossil imprint of primordial sub-clustering that arises naturally if massivestars form preferentially in the highest density central regions of aprotocluster.

The Distribution of Main Sequence and Pre-Main Sequence Stars in the Young Anticenter Cluster NGC 2401