Fig. 3.
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mF606W versus mF606W − mF814W CMD of the stars shown in Fig. 2, with the same colour-coding. Photometry is from Bellini et al. (2014). Note how the two separate groups identified in Fig. 2 appear here as a tangled mixture. Crowding and incompleteness hinder the photometric precision required to resolve the two sequences in this optical CMD.
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