反馈和反循环风吸积：组装z=0星系质量函数
Feedback and Recycled Wind Accretion: Assembling the z=0 Galaxy Mass Function
摘要：
我们分析宇宙学流体动力学模拟，包括观测约束的处方银河系外流。如果这些模拟的风准确地代表了真实宇宙中的风，那么以前在风中喷出的物质为红移z<1的新恒星形成提供了主要的气体流入源。这种循环风吸积，或风模式，提供了第三个物理上不同的吸积通道，除了“热”和“冷”模式强调在最近的理论研究。由于外流和气体之间的相互作用和周围的晕，风材料的再循环时间尺度（t_rec）是更短的质量较高的系统，其中居住在稠密的气体环境。在这些模拟中，这种差异回收在塑造当今的星系恒星质量函数（GSMF）中起着核心作用。如果我们去除所有曾经在风中喷出的粒子，那么预测的GSMF比观察到的要陡得多;星系质量受到气体直接去除和周围环境的流体动力学加热的抑制，这减少了随后的下降。考虑到风的再循环，结合了我们喜欢的动量驱动风定标的模拟再现了恒星质量为10^9 < M < 5x10^10 Msolar时观测到的GSMF。在更高的质量，风循环导致过度的星系质量和过度的恒星形成率相对于观测。在这些大质量系统中，某些猝灭机制必须抑制从恒星形成星系喷出的气体的再吸积。简而言之，正如人们长期以来所预期的那样，GSMF的形式是由外流控制的;这里对我们模拟的风的意想不到的扭曲是，它主要不是物质的喷射，而是喷射物质如何重新吸积来控制GSMF。
英文摘要：
We analyse cosmological hydrodynamic simulations that include observationally-constrained prescriptions for galactic outflows. If these simulated winds accurately represent winds in the real Universe, then material previously ejected in winds provides the dominant source of gas infall for new star formation at redshifts z<1. This recycled wind accretion, or wind mode, provides a third physically distinct accretion channel in addition to the "hot" and "cold" modes emphasised in recent theoretical studies. Because of the interaction between outflows and gas in and around halos, the recycling timescale of wind material (t_rec) is shorter in higher-mass systems, which reside in denser gaseous environments. In these simulations, this differential recycling plays a central role in shaping the present-day galaxy stellar mass function (GSMF). If we remove all particles that were ever ejected in a wind, then the predicted GSMFs are much steeper than observed; galaxy masses are suppressed both by the direct removal of gas and by the hydrodynamic heating of their surroundings, which reduces subsequent infall. With wind recycling included, the simulation that incorporates our favoured momentum-driven wind scalings reproduces the observed GSMF for stellar masses 10^9 < M < 5x10^10 Msolar. At higher masses, wind recycling leads to excessive galaxy masses and excessive star formation rates relative to observations. In these massive systems, some quenching mechanism must suppress the re-accretion of gas ejected from star-forming galaxies. In short, as has long been anticipated, the form of the GSMF is governed by outflows; the unexpected twist here for our simulated winds is that it is not primarily the ejection of material but how the ejected material is re-accreted that governs the GSMF.
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