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Using high-resolution Hubble Space Telescope data, we reexamine thefundamental properties (ages, masses and extinction values) of the rich starcluster population in the dwarf starburst galaxy NGC 5253. The gain inresolution compared to previous studies is of order a factor of two in bothspatial dimensions, while our accessible wavelength range transcends previousstudies by incorporation of both near-ultraviolet and near-infrared (IR)passbands. We apply spectral synthesis treatments based on two different simplestellar population model suites to our set of medium-, broad-band and H-alphaimages to gain an improved physical understanding of the IR-excess flux foundfor a subset of young clusters (30 of 149). With the caveat that our models arebased on fully sampled stellar mass functions, the NGC 5253 cluster populationis dominated by a significant number of relatively low-mass (M_cl <= a few 10^4Msun) objects with ages ranging from a few x 10^6 to a few x 10^7 yr, which isin excellent agreement with the starburst age of the host galaxy. The IR-excessclusters are almost all found in this young age range and have masses of up toa few x 10^4 Msun. The IR excess in the relatively low-mass NGC 5253 clustersis most likely caused by a combination of stochastic sampling effects andcolour variations due to the presence of either luminous red orpre-main-sequence stars. We also find a small number of intermediate-age (~ 1Gyr-old), ~10^5 Msun clusters, as well as up to a dozen massive, ~10 Gyr-oldglobular clusters. Their presence supports the notion that NGC 5253 is a veryactive galaxy that has undergone multiple episodes of star cluster formation.

The NGC 5253 star cluster system. I. Standard modelling and infrared-excess sources