The redshift evolution of the distribution of star formation among dark matter halos as seen in the infrared
The redshift evolution of the distribution of star formation among dark matter halos as seen in the infrared
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红外光中观察到的暗物质晕中恒星形成分布的红移演化
DOI：
10.1051/0004-6361/201321688
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发表时间：
2013
影响因子：
6.5
通讯作者：
H. Aussel
中科院分区：
文献类型：
--
作者：
M. B'ethermin;Lingyu Wang;O. Dor'e;G. Lagache;M. Sargent;E. Daddi;M. Cousin;H. Aussel
最近的研究揭示了星星形成率（SFR）
和恒星质量的大多数恒星形成星系，所谓的恒星形成的主要
顺序一种经验建模方法（2-SFM框架），
主序星和更罕见的星暴星系能够复制大多数统计数据，
红外星系的性质，如计数，光度函数和红移
分布。在本文中，我们通过建立以下关系来扩展这种方法：
恒星质量和晕质量。基于一些简单的
假设和物理动机的形式主义，我们的模型成功地预测了
宇宙红外背景（CIB）的（交叉）功率谱，交叉相关
CIB和宇宙微波背景（CMB）透镜之间的关系，
由赫歇尔观测到的明亮的红外星系，
Planck、ACT和SPT。我们用这个模型来推断红移
CIB各向异性和CIB × CMB透镜信号的分布，以及
CIB各向异性在不同波长之间的相关性。我们研究了
暗物质晕和恒星形成星系之间的联系。我们
据预测，90%以上的宇宙星星形成活动发生在质量
在1011.5和1013.5 M之间。如果服用
考虑到随后的晕质量增长，这意味着大多数恒星都是
最初（在z > 3时）形成于
集群
(Mh(z= 0）> 1013.5 M Ω），
然后分组
（1012.5 < Mh（z = 0）< 1013.5 Mh）
在0.5 < z < 3，和
最后在银河般的光环中
（1011.5 < Mh（z = 0）< 1012.5 Mh）
z < 0.5。在所有的红移中，
对SFR密度的贡献来自质量晕
~1012 M轨道，其中瞬时星星
形成效率-这里定义为SFR和重子吸积率之间的比率-
最大值（~70%）。在支配银河系的星系中SFR的强红移演化
因此，CIB可能是由来自宇宙网的增加的吸积驱动的，
特征质量标度材料（有效光谱能量分布，微分
晕的发射率，Mh和SFR之间的关系）
与此模型相关的信息可在http://irfu.cea.fr/Sap/Phocea/Page/index.php?上获得id=537。
Recent studies have revealed a strong correlation between the star formation rate (SFR)
and stellar mass of the majority of star-forming galaxies, the so-called star-forming main
sequence. An empirical modeling approach (the 2-SFM framework) that distinguishes between
the main sequence and rarer starburst galaxies is capable of reproducing most statistical
properties of infrared galaxies, such as number counts, luminosity functions, and redshift
distributions. In this paper, we extend this approach by establishing a connection between
stellar mass and halo mass with the technique of abundance matching. Based on a few simple
assumptions and a physically motivated formalism, our model successfully predicts the
(cross-)power spectra of the cosmic infrared background (CIB), the cross-correlation
between CIB and cosmic microwave background (CMB) lensing, and the correlation functions
of bright, resolved infrared galaxies measured by Herschel,
Planck, ACT, and SPT. We use this model to infer the redshift
distribution of CIB-anisotropies and of the CIB × CMB lensing signal, as well as the level
of correlation between CIB-anisotropies at different wavelengths. We study the link
between dark matter halos and star-forming galaxies in the framework of our model. We
predict that more than 90% of cosmic star formation activity occurs in halos with masses
between 1011.5 and 1013.5 M⊙. If taking
subsequent mass growth of halos into account, this implies that the majority of stars were
initially (at z > 3) formed in the progenitors of
clusters
(Mh(z = 0) > 1013.5 M⊙),
then in groups
(1012.5 < Mh(z = 0) < 1013.5 M⊙)
at 0.5 < z < 3, and
finally in Milky-Way-like halos
(1011.5 < Mh(z = 0) < 1012.5 M⊙)
at z < 0.5. At all redshifts, the dominant
contribution to the SFR density stems from halos of mass
~1012 M⊙, in which the instantaneous star
formation efficiency – defined here as the ratio between SFR and baryonic accretion rate –
is maximal (~70%). The strong redshift-evolution of SFR in the galaxies that dominate the
CIB is thus plausibly driven by increased accretion from the cosmic web onto halos of this
characteristic mass scale. Material (effective spectral energy distributions, differential
emissivities of halos, relations between Mh and SFR)
associated to this model is available at http://irfu.cea.fr/Sap/Phocea/Page/index.php?id=537.
影响因子：
4.8
作者：
G. Addison;G. Addison;J. Dunkley;J. Bond
通讯作者：
G. Addison;G. Addison;J. Dunkley;J. Bond
DOI：
10.1088/0004-637x/768/1/74
发表时间：
2012-11
期刊：
The Astrophysical Journal
影响因子：
--
作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-
通讯作者：
L. Tacconi;R. Neri;R. Genzel;F. Combes;A. Bolatto;M. Cooper;S. Wuyts;F. Bournaud;A. Burkert-