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Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color)

WFC3/NUV,U,B,V,I,H,H a ,P b : 33 galaxies; ~100 low mass clusters. Spectral Population Synthesis + IMF-Stochastic Models: range of IMF, metallicity. Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color). Ionized gas photometry (H a , P b : luminosity, extinction).

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Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color)

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  1. WFC3/NUV,U,B,V,I,H,Ha,Pb: 33 galaxies; ~100 low mass clusters Spectral Population Synthesis + IMF-Stochastic Models: range of IMF, metallicity Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color) Ionized gas photometry (Ha, Pb: luminosity, extinction) Clusters with age<8 Myr Cluster age, mass, extinction (NUV,U,B,V,I: SED fitting + Bayesian error analysis) <S L(Ha) / S Mcluster> and s(L(Ha)/Mcluster): expectations versus observations for IMF (non)variation/sorting Mcluster > 500 Mo Ncluster(0-10 Myr)/Ncluster(10-100 Myr) • Model discrimination: • IMF variations/sorting; • Stochastic star formation history (from star cluster age distribution); • Ionizing photon leakage (if the two above are insufficient).

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