The color-magnitude diagram ( CMD ) of the intermediate-age Large Magellanic Cloud ( LMC ) star cluster NGCÂ 2154 and its adjacent field , has been analyzed using Padova stellar models to determine the cluster ’ s fundamental parameters and its Star Formation History ( SFH ) .
Deep BR CCD photometry , together with synthetic CMDs and Integrated Luminosity Functions ( ILFs ) , has allowed us to infer that the cluster experienced an extended star formation period of about 1.2Â Gyrs , which began approximately 2.3Â Gyr and ended 1.1Â Gyr ago .
The physical reality of such a prolonged period of star formation is however questionable , and could be the result of inadequacies in the stellar evolutionary tracks themselves .
A substantial fraction of binaries ( 70 \% ) seems to exist in NGCÂ 2154 .