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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) - PowerPoint PPT Presentation


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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).

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PowerPoint Slideshow about 'Cluster ID+photometry (NUV,U,B,V,I: White-light + multi-color)' - logan-franklin


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slide1

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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