Size matters: abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE
Size matters: abundance matching, galaxy sizes, and the Tully-Fisher relation in EAGLE
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大小很重要：丰度匹配、星系大小以及 EAGLE 中的 Tully-Fisher 关系
DOI：
10.1093/mnras/stw2691
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发表时间：
2016
影响因子：
4.8
通讯作者：
T. Theuns
中科院分区：
文献类型：
--
作者：
I. Ferrero;J. Navarro;M. Abadi;L. Sales;R. Bower;R. Crain;C. Frenk;M. Schaller;J. Schaye;T. Theuns
Tully-Fisher关系（TFR）将盘状星系Mstr的恒星质量与其旋转速度联系起来：它很好地近似于幂律，显示出很少的散射，并且随着红移而微弱地演化。这种关系被解释为反映了暗物质晕的质量-速度缩放（M∝V3），但这种解释受到了丰度匹配（AM）模型的质疑，该模型预测星系-晕的质量关系在很大程度上偏离了单一的幂律，并随着红移而迅速演变。我们利用冷暗物质（_CDM）的EAGLE宇宙学模拟，研究了发光螺旋的TFR及其与AM的关系。要匹配这两种关系，需要圆盘的大小满足由晕的浓度及其对星系集合的响应所给出的约束。EAGLE星系大致符合这些限制条件，并显示出与观测到的TFR相比有利的紧密质量-速度缩放。TFR退化为星系形成效率和质量-尺寸关系的变化；如果星系遵循不同的质量-大小关系，那么不能匹配星系恒星质量函数的模拟可能符合观测到的TFR。在固定的光晕质量下，星系质量与自转速度的相关性较强，使得模拟TFR结果的散射较小。EAGLE星系的回溯时间演化近似遵循AM模型的公式和观测到的明亮螺旋的质量-大小关系，导致弱TFR演化与z = 1以内的观测一致。匹配星系丰度和大小作为恒星质量函数的_CDM模型不难再现观测到的TFR及其演化。
The Tully–Fisher relation (TFR) links the stellar mass of a disc galaxy, Mstr, to its rotation speed: it is well approximated by a power law, shows little scatter, and evolves weakly with redshift. The relation has been interpreted as reflecting the mass–velocity scaling (M ∝ V3) of dark matter haloes, but this interpretation has been called into question by abundance-matching (AM) models, which predict the galaxy–halo mass relation to deviate substantially from a single power law and to evolve rapidly with redshift. We study the TFR of luminous spirals and its relation to AM using the EAGLE set of _ cold dark matter (_CDM) cosmological simulations. Matching both relations requires disc sizes to satisfy constraints given by the concentration of haloes and their response to galaxy assembly. EAGLE galaxies approximately match these constraints and show a tight mass–velocity scaling that compares favourably with the observed TFR. The TFR is degenerate to changes in galaxy formation efficiency and the mass–size relation; simulations that fail to match the galaxy stellar mass function may fit the observed TFR if galaxies follow a different mass–size relation. The small scatter in the simulated TFR results because, at fixed halo mass, galaxy mass and rotation speed correlate strongly, scattering galaxies along the main relation. EAGLE galaxies evolve with lookback time following approximately the prescriptions of AM models and the observed mass–size relation of bright spirals, leading to a weak TFR evolution consistent with observation out to z = 1. _CDM models that match both the abundance and size of galaxies as a function of stellar mass have no difficulty reproducing the observed TFR and its evolution.
DOI：
10.1111/j.1365-2966.2009.15034.x
发表时间：
2008-08
影响因子：
4.8
作者：
K. Dolag;S. Borgani;S. Borgani;S. Borgani;G. Murante;V. Springel
通讯作者：
K. Dolag;S. Borgani;S. Borgani;S. Borgani;G. Murante;V. Springel