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tokens: with 10% and 30% of binaries. In the latter ones, the peak density is around the (0,0) point. The binaries contribute to producing an elongated structure with a lower density (which increases with the binary fraction). In NGC 5272 3 , the P1 sequence is relatively homogeneously populated with barely a very small overdensity near the origin. The same trend is observed for NGC 6254 (not shown), from which we conclude that either the binary fractions in GCs are underestimated, or binaries contribute only part of the extension of P1, and another process is at play. Fig. 7. Hess diagrams based on chromosome maps of the synthetic clusters with 10% ( top left panel ) and 30% ( top right panel ) of binaries, together with that of of NGC 5272 ( bottom panel ). A further test of the effects of binaries on the chromosome map is shown in Fig. 8 . We selected the cluster NGC 6254 since; (1) it shows an extended P1 ( Milone et al. 2017 ), (2) its metallicity corresponds to that of our models, and (3) the binary fraction decreases from the core to the outer parts of the cluster ( Dalessandro et al. 2011 ; Milone et al. 2012 ). To investigate whether or not this variation of the binary fraction is reflected in the shape of P1, we selected two regions of the cluster: the core and an annulus around it, as displayed in the left panel of Fig. 8 . We subsequently selected the stars brighter than the bottom of the RGB in each region and constructed their chromosome map. The results, shown in the right panel of Fig. 8 , do not show any significant variation of the extent of the chromosome map. This result does not depend on the choice of the core and annulus regions. If binaries governed the elongation of P1, one would expect a smaller extension in the outer regions of the cluster, which is not observed. Fig. 8. Left panel : position of stars brighter than m 814 W = 18.5 in the cluster NGC 6254. The red and blue circles indicate the two regions used to produce the chromosome maps of the right panel . Right panel : chromosome map of the stars inside the blue circle in the left panel (blue squares) and of the stars in between the red and blue circles (open red circles). Only stars brighter than m 814 W = 16.5 (i.e., above the bottom of the RGB) are considered in the chromosome maps. If binarity were the main reason for the extension of P1, one would also find a correlation between binary fraction and P1 extension. A simple comparison of two GCs with similar properties, NGC 5272 (M 3) and NGC 6205 (M 13), shows some qualitative trends. Both clusters are of about the same age, metallicity and mass ( Harris 1996 ; Marín-Franch et al. 2009 ), but M 3 shows an extended P1, while M 13 does not – see Fig. 5 of Milone et al. (2017) . According to Milone et al. (2012) , the total binary fraction in M 3 (M 13) is between 3 and 6% (2 and 10%). Thus, M 3 does not have a higher binary fraction that would explain its more extended P1. 3.3. Effect of the binary mass ratio