Astrophysical properties of newly discovered Magellanic Cloud star
  clusters
  New star cluster candidates projected toward the Large and Small Magellanic
Clouds (L/SMC) have been recently discovered from relatively deep imaging
surveys. We here conduct a sound analysis of 24 star cluster candidates located
in the outer regions of the L/SMC using PSF photometry produced by the Survey
of the Magellanic Stellar History. With only one exception, the studied objects
resulted to be genuine stellar aggregates. We conclude on their physical
reality once their observed color-magnitude diagrams (CMDs) were statistically
decontaminated by the presence of field stars, and the resulting cleaned CMDs
for stars with assigned membership probabilities higher than 50\% were compared
with synthetic CMDs generated for thousand combinations of ages, distances,
metallicities, star cluster mass and binary fractions. The parameter of the
best-matched synthetic CMDs obtained from a likelihood approach were adopted as
the star cluster astrophysical properties. The present star cluster sample
spans a wide range of distances, from those star clusters located in front of
the LMC, to those along the onset of the Magellanic Bridge, up to those behind
the SMC. Their ages reveal different formation episodes that took place along
the galaxy formation and others as a consequence of the galaxy interactions.
From their estimated metallicities and ages, we speculate with the possibility
that relatively metal-deficient gaseous flows have existed between these
galaxies during nearly the last one Gyr (log(age /yr) $\approx$ 9.0), that made
possible the formation of young star clusters in the galaxy peripheries.
Despide the L/SMC interactions, the studied star clusters are similar or more
massive than their counterparts in the Milky Way, which suggests that tidal
effects are relatively more important in our Galaxy.
