Signal-to-noise ratio distributions for the remaining clusters in the sample, complementing those shown in Fig. 2. Among them, a prominent overdensity appears below NGC 362, which is caused by contamination from the Small Magellanic Cloud. In addition, NGC 5024 and NGC 5053 have very similar CMDs and are commonly regarded as an interacting pair of clusters (Chun et al. 2010), and thus they appear in each other’s field.

Continued.