Fig. 2: Comparing the distributions of BSS rotational velocities in loose and high-density clusters. | Nature Communications

Fig. 2: Comparing the distributions of BSS rotational velocities in loose and high-density clusters.

From: Fast rotating blue stragglers prefer loose clusters

Fig. 2

a BSS rotational velocity distribution for loose clusters (namely, ω Centauri, M55, NGC 3201 and M4), compared to that of high-density clusters (namely, 47 Tucanae, M30, NGC 6752 and NGC 6397), in the top panel (red histogram) and in the bottom panel (blue histogram), respectively. In both cases, the fraction is referred to the total number of BSSs observed in each sample. b Comparison between the normalised cumulative distributions of BSS rotational velocities in low-density (red line) and high-density (blue line) clusters. A Kolmogorov–Smirnov test applied to the two distributions confirms that they are different at more than a 5 σ significance level.

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