mufasa: the assembly of the red sequence
mufasa: the assembly of the red sequence
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mufasa：红色序列的组装
DOI：
10.1093/mnras/stx1693
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发表时间：
2017
影响因子：
4.8
通讯作者：
Robert J. Thompson
中科院分区：
文献类型：
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作者：
R. Dav'e;M. Rafieferantsoa;Robert J. Thompson
我们在木法沙宇宙流体力学模拟中研究了猝灭星系的生长和演化，其中包括基于晕质量的演化猝灭处方，计算的星系颜色考虑了单个恒星粒子的视线消光。木法沙相当好地再现了观测到的今天的红色序列，包括它的斜率、幅度和散布。在木法沙，红色序列斜率完全由陡峭的恒星质量-恒星金属丰度关系驱动，这与观测结果独立地一致。高质量恒星形成星系平稳地混合到红色序列中，表明在M*>；10^10.5 Mo缺乏清晰的绿色山谷。最大质量的星系最早熄灭，然后通过干合并获得很小的质量增长；它们在较早的时期达到高质量，那时冷流入更有效地穿透热晕。对于红移更高的星系，红色序列变得越来越多地被巨大的尘埃恒星形成星系所污染；UVJ的选择微妙但有效地分离了这些星系群。然后，我们研究了中央星系和卫星星系通过UVJ分裂为被动星系和恒星形成星系的质量函数的演化。大质量猝灭系统显示出与观测到z~2的良好一致性，尽管不包括与合并相关的快速早期猝灭模式。然而，在木法沙的z<；1处，低质量熄灭的星系太多了，这表明木法沙强烈地过度熄灭了卫星。流体力学模拟的一个挑战是设计一个猝灭模型，它能产生足够多的早期质量猝灭的星系，并使它们保持猝灭到z=0，同时又不至于太强，以至于过度猝灭卫星；木法沙目前的计划在后者失败了。
We examine the growth and evolution of quenched galaxies in the Mufasa cosmological hydrodynamic simulations that include an evolving halo mass-based quenching prescription, with galaxy colours computed accounting for line-of-sight extinction to individual star particles. Mufasa reproduces the observed present-day red sequence reasonably well, including its slope, amplitude, and scatter. In Mufasa, the red sequence slope is driven entirely by the steep stellar mass-stellar metallicity relation, which independently agrees with observations. High-mass star-forming galaxies blend smoothly onto the red sequence, indicating the lack of a well-defined green valley at M*>10^10.5 Mo. The most massive galaxies quench the earliest and then grow very little in mass via dry merging; they attain their high masses at earlier epochs when cold inflows more effectively penetrate hot halos. To higher redshifts, the red sequence becomes increasingly contaminated with massive dusty star-forming galaxies; UVJ selection subtly but effectively separates these populations. We then examine the evolution of the mass functions of central and satellite galaxies split into passive and star-forming via UVJ. Massive quenched systems show good agreement with observations out to z~2, despite not including a rapid early quenching mode associated with mergers. However, low-mass quenched galaxies are far too numerous at z<1 in Mufasa, indicating that Mufasa strongly over-quenches satellites. A challenge for hydrodynamic simulations is to devise a quenching model that produces enough early massive quenched galaxies and keeps them quenched to z=0, while not being so strong as to over-quench satellites; Mufasa's current scheme fails at the latter.
DOI：
10.1088/0004-637x/744/1/63
发表时间：
2011-06
期刊：
The Astrophysical Journal
影响因子：
--
作者：
L. Oser;T. Naab;J. Ostriker;P. Johansson
通讯作者：
L. Oser;T. Naab;J. Ostriker;P. Johansson