Evolution of cluster luminosity in the optical (upper row) and NIR (lower row). The curves in the left and middle panels present SSP models with continuous IMF, whereas in the right panel we compare continuous and discrete options. Left panels: impact of dynamical mass loss on integrated luminosity of clusters of different masses and stellar low-mass limit m_l = 0.1   m_⊙. The four curves from top to bottom are models for clusters with masses M_c = 10⁴   m_⊙, M_c = 5  ×  10³   m_⊙, M_c = 10³   m_⊙, and M_c = 5  ×  10²   m_⊙, respectively. The dotted curves indicate models without mass loss. Middle panels: influence of different lower mass limits m_l of cluster stars on integrated luminosity of clusters with mass M_c = 10³   m_⊙. The upper, middle, and bottom curves correspond to m_l = 1, 0.1, 0.01   m_⊙, respectively. Right panels: integrated magnitudes of clusters modelled with continuous (curves) and discrete (connected symbols) IMFs for stellar low-mass limit m_l = 0.1   m_⊙. The upper curve and crosses are for cluster mass M_c = 10⁴   m_⊙, and the bottom curve and diamonds are for M_c = 10³   m_⊙. The mass loss owing to dynamical evolution is incorporated in both models. For comparison, the continuous model without mass loss is shown by the dotted curves.