Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color)
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Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color) luster age, mass, extinction (NUV,U,B,V,I: ED fitting + Bayesian error analysis) Ionized gas photometry (H, P: luminosity, extinction) Cluste rs wi th age<8 M yr M cluster > 500 M o WFC3/NUV,U,B,V,I,H,H,P: 33 galaxies; ~100 low mass clusters Spectral Population Synthesis + IMF- Stochastic Models: range of IMF, metallicity < L(H / M cluster > and (L(H/M cluster ): expectations versus observations for IMF (non)variation/sorting Model discrimination: 1.IMF variations/sorting; 2.Stochastic star formation history (from star cluster age distri 3.Ionizing photon leakage (if the two above are insufficient). luster (0-10 Myr)/N cluster (10-100 Myr)
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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). - PowerPoint PPT Presentation
Transcript of Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color)
Cluster ID+photometry (NUV,U,B,V,I:White-light + multi-color)
Cluster age, mass, extinction (NUV,U,B,V,I:SED fitting + Bayesian error analysis)
Ionized gas photometry (H, P:luminosity, extinction)
Clusters with age<8 Myr
Mcluster > 500 M
o
WFC3/NUV,U,B,V,I,H,H,P: 33 galaxies; ~100 low mass clusters
Spectral Population Synthesis + IMF-Stochastic Models: range of IMF, metallicity
< L(H / Mcluster> and (L(H/Mcluster):expectations versus observations for IMF (non)variation/sorting
Model discrimination:1.IMF variations/sorting;2.Stochastic star formation history (from star cluster age distribution);3.Ionizing photon leakage (if the two above are insufficient).
Ncluster(0-10 Myr)/Ncluster(10-100 Myr)
