Journal
ASTROPHYSICAL JOURNAL
Volume 725, Issue 2, Pages 1620-1628Publisher
IOP Publishing Ltd
DOI: 10.1088/0004-637X/725/2/1620
Keywords
galaxies: dwarf; galaxies: individual (SBS 0335-052E); galaxies: starburst; galaxies: star clusters: general
Categories
Funding
- Swedish Research Council
- Swedish Royal Academy of Sciences
- Knut and Alice Wallenberg foundation
- Swedish National Space Board
- Swiss National Science Foundation
- National Aeronautics and Space Administration
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The spectral energy distribution analysis of very young unresolved star clusters challenges our understanding of the cluster formation process. Studies of resolved massive clusters in the Milky Way and in the nearby Magellanic Clouds show us that the contribution from photoionized gas is very important during the first Myr of cluster evolution. We present our models which include both a self-consistent treatment of the photoionized gas and the stellar continuum and quantify the impact of such a nebular component on the total flux of young unresolved star clusters. A comparison with other available models is considered. The very young star clusters in the SBS 0335-052E dwarf starburst galaxy are used as a test for our models. Due to the low metallicity of the galactic medium our models predict a longer lasted nebular phase which contributes between 10% and 40% of the total near-infrared (NIR) fluxes at around 10 Myr. We thus propose a possible solution for the observed flux excess in the six bright super star clusters (SSCs) of SBS 0335-052E. Reines et al. showed that the observed cluster fluxes, in the red-optical and NIR range, sit irreconcilably above the stellar continuum models provided. We find that in the age range estimated from the H alpha emission we can explain the red excess in all six SSCs as due to nebular emission, which at cluster ages around 10 Myr still affects the NIR wavebands substantially.
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