Luminous red galaxies in hierarchical cosmologies
Luminous red galaxies in hierarchical cosmologies
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分层宇宙学中的发光红色星系
DOI：
10.1111/j.1365-2966.2008.13179.x
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发表时间：
2008
影响因子：
4.8
通讯作者：
Almeida C
中科院分区：
文献类型：
--
作者：
Almeida C
发光的红色星系(LRG)比L*星系稀有得多，质量也大得多。再加上它们的极端颜色，LRG因此为大质量星系形成的物理学提供了一个苛刻的试验场。我们首次在层次结构形成模型中对LRG的丰度和性质进行了自洽预测。我们测试了两个已发表的模型，它们使用完全不同的机制来抑制大质量星系的形成：鲍尔等人。该模型调用“活动星系核(AGN)反馈”来防止气体在大质量晕中冷却，以及Baugh等人。该模型依靠“超风”在气体变成恒星之前喷出气体。在不调整任何参数的情况下，鲍尔等人。该模型与斯隆数字巡天中观测到的LRG的光度函数(红移中值为Z=0.24)和它们的星团有很好的匹配；模型在这些方面就不那么成功了。在模型中，LRG是典型的球面主控系统，恒星质量为≈2×1011h−1M⊙，速度色散为σ∼2 5 0 km S−1。LRG模型中大约一半的恒星质量已经由z∼2.2形成，并由z∼1.5组装成一个主祖星；平均而言，只有25%的主要前身质量被添加到z∼1之后。LRG被预测存在于广泛的晕质量中，这一结论依赖于适当地考虑到晕形成历史中的散射。值得注意的是，我们发现LRG的关联函数被预测为一个幂定律，直到小的配对间隔，这与观测估计非常一致。鲍尔等人也没有。Baugh等人也是如此。模型能够重现观测到的LRG半径。
Luminous red galaxies (LRGs) are much rarer and more massive thanL*galaxies. Coupled with their extreme colours, LRGs therefore provide a demanding testing ground for the physics of massive galaxy formation. We present the first self-consistent predictions for the abundance and properties of LRGs in hierarchical structure formation models. We test two published models which use quite different mechanisms to suppress the formation of massive galaxies: the Bower et al. model which invokes ‘active galactic nuclei (AGN) feedback’ to prevent gas from cooling in massive haloes and the Baugh et al. model which relies upon a ‘superwind’ to eject gas before it is turned into stars. Without adjusting any parameters, the Bower et al. model gives an excellent match to the observed luminosity function of LRGs in the Sloan Digital Sky Survey (with a median redshift ofz= 0.24) and to their clustering; the Baugh et al. model is less successful in these respects. Both models fail to match the observed abundance of LRGs atz= 0.5 to better than a factor of ≈2. In the models, LRGs are typically bulge-dominated systems with stellar masses of ≈2 × 1011h−1M⊙and velocity dispersions of σ∼ 250 km s−1. Around half of the stellar mass in the model LRGs is already formed byz∼ 2.2 and is assembled into one main progenitor byz∼ 1.5; on average, only 25 per cent of the mass of the main progenitor is added afterz∼ 1. LRGs are predicted to be found in a wide range of halo masses, a conclusion which relies on properly taking into account the scatter in the formation histories of haloes. Remarkably, we find that the correlation function of LRGs is predicted to be a power law down to small pair separations, in excellent agreement with observational estimates. Neither the Bower et al. nor the Baugh et al. model is able to reproduce the observed radii of LRGs.
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DOI：
10.1111/j.1365-2966.2006.09994.x
发表时间：
2006-02
影响因子：
4.8
作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
通讯作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
星系形成对星团 X 射线演化的影响
DOI：
--
发表时间：
2000
期刊：
影响因子：
--
作者：
R. Bower;Andrew J Benson;C. Lacey;C. Baugh;S. Cole;C. Frenk
通讯作者：
C. Frenk
DOI：
10.1086/376517
发表时间：
2002-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Berlind;D. Weinberg;A. Benson;C. Baugh;S. Cole;R. Dav'e;C. Frenk;A. Jenkins;N. Katz;C. Lacey
通讯作者：
A. Berlind;D. Weinberg;A. Benson;C. Baugh;S. Cole;R. Dav'e;C. Frenk;A. Jenkins;N. Katz;C. Lacey
DOI：
10.1111/j.1365-2966.2007.11593.x
发表时间：
2006-05
影响因子：
4.8
作者：
N. Padmanabhan;D. Schlegel;U. Seljak;U. Seljak;A. Makarov;N. Bahcall;M. Blanton;J. Brinkmann;D. Eisenstein;D. Finkbeiner;J. Gunn;D. Hogg;Ž. Ivezić;G. Knapp;J. Loveday;R. Lupton;R. Nichol;D. Schneider;M. Strauss;M. Tegmark;D. York
通讯作者：
N. Padmanabhan;D. Schlegel;U. Seljak;U. Seljak;A. Makarov;N. Bahcall;M. Blanton;J. Brinkmann;D. Eisenstein;D. Finkbeiner;J. Gunn;D. Hogg;Ž. Ivezić;G. Knapp;J. Loveday;R. Lupton;R. Nichol;D. Schneider;M. Strauss;M. Tegmark;D. York
DOI：
--
发表时间：
1998
期刊：
影响因子：
--
作者：
C. Baugh;Andrew J Benson;S. Cole;C. Frenk;C. Lacey
通讯作者：
C. Lacey