关于非常年轻的超星团中红色过剩的起源：SBS 0335- 052 E的情况
On the origin of the red excess in very young super star clusters: the case of SBS 0335-052E
摘要：
对非常年轻的未分辨星团的光谱能量分布分析挑战了我们对团簇形成过程的理解。对银河系和附近麦哲伦云中的大质量星系团的研究表明，在星系团演化的第一个百万年期间，光电离气体的贡献是非常重要的。我们提出了我们的模型，其中包括一个自洽的治疗的光电离气体和恒星的连续性和量化的影响，这样的星云组件上的总通量的年轻的未解决的星团。被认为是与其他可用的模型的比较。SBS 0335- 052 E矮星爆星系中的非常年轻的星团被用来作为我们的模型的测试。由于银河系介质的金属丰度较低，我们的模型预测了一个持续时间较长的星云阶段，在大约1000万年的时间里，它贡献了总近红外（NIR）通量的10-40%。因此，我们针对SBS 0335- 052 E的6个明亮超级星团中观察到的通量过剩提出了一种可能的解决方案。Reines等人的研究表明，在红光和近红外波段观测到的星团通量，都不可避免地高于恒星连续统模型。我们发现，在由H_α辐射估算的年龄范围内，我们可以解释所有6个超级星团中的红色过剩是由于星云辐射造成的，在1000万年左右的星团年龄，星云辐射仍然对近红外波段有很大的影响。
英文摘要：
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 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 10-40% of the total near infrared (NIR) fluxes at around 10 Myr. We propose thus a possible solution for the observed flux excess in the 6 bright super star clusters of SBS 0335-052E. Reines et al. showed that the observed cluster fluxes, in the red-optical and NIR range, sit irreconcilably above the provided stellar continuum models. We find that in the age range estimated from the H_alpha emission we can explain the red excess in all the 6 super star clusters as due to nebular emission, which at cluster ages around 10 Myr still affects the NIR wavebands substantially.
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