We report on the astrophysical properties of a sample of star clusters in the Small Magellanic Cloud (SMC). They have been selected with the aim of looking for the connection between their ages, heliocentric distances and metallicities with the existence of tidally perturbed/induced outermost SMC regions. We derived the star cluster fundamental parameters from relatively deep Survey of the Magellanic Stellar History (SMASH) DR2 color magnitude diagrams, cleaned from field star contamination, and compared to thousand synthetic CMDs covering a wide range of heliocentric distances, ages and metal content. Heliocentric distances for 15 star clusters are derived for the first time, which represents an increase of 50 per cent of SMC clusters with estimated heliocentric distances. The analysis of the age-metallicity relationships (AMRs) of cluster located in outermost regions distributed around the SMC and in the SMC Main Body reveals that they have followed the overall galaxy chemical enrichment history. However, since half of the studied clusters are placed in front of or behind the SMC Main Body, we concluded that they formed in the SMC and have traveled outward because of the tidal effects from the interaction with the Large Magellanic Cloud (LMC). Furthermore, metal rich clusters formed recently in some of these outermost regions from gas that was also dragged by tidal effects from the inner SMC. This outcome leads to consider the SMC as a galaxy scarred by the LMC tidal interaction with distance-perturbed and newly induced outermost stellar substructures.
Illesca et al. (2025) studied this question.
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