We present results based on YJK _ { s } photometry of star clusters located in the outermost , eastern region of the Small Magellanic Cloud ( SMC ) .
We analysed a total of 51 catalogued clusters whose colour–magnitude diagrams ( CMDs ) , having been cleaned from field-star contamination , were used to assess the clusters ’ reality and estimate ages of the genuine systems .
Based on CMD analysis , 15 catalogued clusters were found to be possible non-genuine aggregates .
We investigated the properties of 80 % of the catalogued clusters in this part of the SMC by enlarging our sample with previously obtained cluster ages , adopting a homogeneous scale for all .
Their spatial distribution suggests that the oldest clusters , log ( t yr ^ { -1 } ) \geq 9.6 , are in general located at greater distances to the galaxy ’ s centre than their younger counterparts – 9.0 \leq log ( t yr ^ { -1 } ) \leq 9.4 – while two excesses of clusters are seen at log ( t yr ^ { -1 } ) \sim 9.2 and log ( t yr ^ { -1 } ) \sim 9.7 .
We found a trail of younger clusters which follow the Wing/Bridge components .
This long spatial sequence does not only harbour very young clusters , log ( t yr ^ { -1 } ) \sim 7.3 , but it also hosts some of intermediate ages , log ( t yr ^ { -1 } ) \sim 9.1 .
The derived cluster and field-star formation frequencies as a function of age are different .
The most surprising feature is an observed excess of clusters with ages of log ( t yr ^ { -1 } ) < 9.0 , which could have been induced by interactions with the LMC .