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A consensus on the origin of the different stellar populations in NGC2808 has not been reached yet. Previous findings are based on data for a few small fields centered on the cluster (HST) or for a field of view covering about half the tidal radius (ground). There is now the need for deep photometry covering the entire cluster (tidal radius rt rt ~ 16 arcmin)
with the accuracy necessary to enable the identification of the different main sequences. This photometric catalog would allow the homogenous study of the multiple populations in NGC2808 and possibly a clear understanding of the origin and evolution of this peculiar globular cluster.
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Fig. 2: DECam g-i vs u-r vs r color-color-magnitude diagram of Omega Cen member (multiple color dots) and field stars (gray dots) seen from the front (left top panel) and the back (rightbottom). This approach can be applied to separate field and cluster stars thanks to the opportunity to use the u filter, since this band allows a better sensitivity to both effective temperature and metallicity. We will apply this method to separate cluster and field stars in NGC2808. This figure is taken from Calamida et al. (2017, AJ, 153, 175).
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