J, H, K-band spectral energy distributions of our sample of six LMC globular clusters. The black solid lines indicate the most closely matching (in age and metallicity) stellar population model of Maraston (2005); i.e. age = 13 Gyr,  [Z/H]  =  −1.35 for NGC 1754, NGC 2005, and NGC 2019, age = 2 Gyr,  [Z/H]  =  −0.33 for NGC 2173, and age = 1.5 Gyr,  [Z/H]  =  −0.33 for NGC 1806 and NGC 2162. The spectra are normalised to the flux at 1.25 μm. Note the prominent spectral shape differences in the J- and H-bands between old and intermediate age clusters. The shaded areas indicate the regions with contamination by strong OH and O₂ sky line residuals.