恒星形成星系中的G-矮星分布：流入和流出之间的拔河
The G-dwarf distribution in star-forming galaxies: a tug-of-war between infall and outflow
摘要：
在过去，累积金属丰度分布函数（CMDF）被证明是一个有用的工具，以约束吸积历史的各种组成部分的银河系。在这封信中，通过分析，漏盒化学演化模型（即包括两个落入和星系流出），我们研究了本地恒星形成星系的CMDF遵循两个基本的经验标度关系，即质量金属丰度和主序星关系。我们的分析表明，主要在低质量系统中占主导地位的银河风在塑造这个函数，特别是在确定其陡峭度和曲率方面发挥着重要作用。结果表明，低质量（M $_{\star}$/M $_{\odot} \le 10^{9.5}$）和高质量（M $_{\star}$/M $_{\odot}$> 10 $^{10.5}$）星系的CMDF与"闭盒"模型的结果有很大的偏差，因为前（后）系统的演化主要由外流（入流）主导.在银河系缩小的背景下，我们表明，向下凹的CMDFs（与系统具有极小的下降时间尺度和非常强劲的风）是更频繁的低质量星系，其中包括较大比例的年轻系统和气体吸积和再处理（无论是通过恒星形成或风）之间的平衡更大的偏差。
英文摘要：
In the past, the cumulative metallicity distribution function (CMDF) turned out as a useful tool to constrain the accretion history of various components of the Milky Way. In this Letter, by means of analytical, leaky-box chemical evolution models (i.e. including both infall and galactic outflows) we study the CMDF of local star-forming galaxies that follow two fundamental empirical scaling relations, namely the mass-metallicity and main sequence relations. Our analysis shows that galactic winds, which are dominant mostly in low-mass systems, play a fundamental role in shaping this function and, in particular, in determining its steepness and curvature. We show that the CMDF of low-mass (M$_{\star}$/M$_{\odot} \le 10^{9.5}$) and high-mass (M$_{\star}$/M$_{\odot}$>10$^{10.5}$) galaxies deviate substantially from the results of a 'closed-box' model, as the evolution of the former (latter) systems is mostly dominated by outflows (infall). In the context of galactic downsizing, we show that downward-concave CMDFs (associated with systems with extremely small infall timescales and with very strong winds) are more frequent in low-mass galaxies, which include larger fractions of young systems and present more substantial deviations from equilibrium between gas accretion and reprocessing (either via star formation or winds).
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