用IGIMF理论预测恒星形成星系的发散UV和H α通量
Diverging UV and Halpha fluxes of star forming galaxies predicted by the IGIMF theory
摘要：
虽然恒星初始质量函数（IMF）仅在星团中直接确定，但它已被广泛应用于银河系尺度。但考虑到恒星形成的集群性质，银河系范围内的IMF是通过添加所有年轻星团的IMF导致一个完整的银河系初始质量函数（IGIMF）。IGIMF是顶轻相比，典型的IMF在星团和陡峭的降低总恒星形成率（SFR）。这种差异对于大的盘星系来说是微不足道的，但对于SMC型星系和质量较小的星系来说变得很重要。在这里，我们构建IGIMF为基础的总FUV和NUV光度的星系和基础的SFR之间的关系。我们预测，恒星形成矮星系的H α光度的下降速度比紫外光度的下降更快的SFR。当总SFR低于10^-2 M_sun/yr时，这种Halpha-UV通量比的降低应该是明显的。
英文摘要：
Although the stellar initial mass function (IMF) has only been directly determined in star clusters it has been manifoldly applied on galaxy-wide scales. But taking the clustered nature of star formation into account the galaxy-wide IMF is constructed by adding all IMFs of all young star clusters leading to an integrated galactic initial mass function (IGIMF). The IGIMF is top-light compared to the canonical IMF in star clusters and steepens with decreasing total star formation rate (SFR). This discrepancy is marginal for large disk galaxies but becomes significant for SMC-type galaxies and less massive ones. We here construct IGIMF-based relations between the total FUV and NUV luminosities of galaxies and the underlying SFR. We make the prediction that the Halpha luminosity of star forming dwarf galaxies decreases faster with decreasing SFR than the UV luminosity. This turn-down of the Halpha-UV flux ratio should be evident below total SFRs of 10^-2 M_sun/yr.
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