A HEURISTIC PREDICTION OF THE COSMIC EVOLUTION OF THE CO-LUMINOSITY FUNCTIONS
A HEURISTIC PREDICTION OF THE COSMIC EVOLUTION OF THE CO-LUMINOSITY FUNCTIONS
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DOI：
10.1088/0004-637x/702/2/1321
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发表时间：
2009-07
期刊：
影响因子：
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通讯作者：
D. Obreschkow;I. Heywood;H. Klöckner;S. Rawlings
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文献类型：
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作者：
D. Obreschkow;I. Heywood;H. Klöckner;S. Rawlings
我们预测了12C16O在红移z = 0到z = 10的星系中前10次旋转跃迁的发射线光度函数（LFs）。这一预测依赖于最近提出的基于千禧年模拟的对~ 3 × 107演化星系中分子冷气体含量的模拟。我们将此模拟与分子质量与CO-line强度之间的转换模型相结合，该模型包含以下机制：(1)分子气体被宇宙微波背景（CMB）、星暴（SBs）和活动星系核（AGNs）加热；(2)致密或倾斜星系中的分子云可以重叠；(3)致密气体在圆盘密度最大的部分分布较均匀；(4) CO光度随星系间金属丰度变化的尺度；(5) CO的光度总是根据CMB来检测的。我们分析了这些效应的相对重要性，并预测了CO-LFs的宇宙演化。最值得注意的结论是，探测到高z≥7 CO发射的规则星系（即没有AGN，没有大质量SB）将受到与CMB微弱对比的极大阻碍，这与之前声称CMB加热将减轻高红移CO的探测相矛盾。银河系外CO谱线的完整模拟和预测的CO- lfs在任何红移都可以在线访问（http://s-cubed.physics.ox.ac）。英国/，去“S3-SAX”)，他们应该是有用的模拟co线调查与未来的望远镜，如阿塔卡马大型毫米/亚毫米阵列或平方公里阵列。
We predict the emission line luminosity functions (LFs) of the first 10 rotational transitions of 12C16O in galaxies at redshift z = 0 to z = 10. This prediction relies on a recently presented simulation of the molecular cold gas content in ∼3 × 107 evolving galaxies based on the Millennium Simulation. We combine this simulation with a model for the conversion between molecular mass and CO-line intensities, which incorporates the following mechanisms: (1) molecular gas is heated by the cosmic microwave background (CMB), starbursts (SBs), and active galactic nuclei (AGNs); (2) molecular clouds in dense or inclined galaxies can overlap; (3) compact gas can attain a smooth distribution in the densest part of disks; (4) CO luminosities scale with metallicity changes between galaxies; and (5) CO luminosities are always detected against the CMB. We analyze the relative importance of these effects and predict the cosmic evolution of the CO-LFs. The most notable conclusion is that the detection of regular galaxies (i.e., no AGN, no massive SB) at high z ≳ 7 in CO emission will be dramatically hindered by the weak contrast against the CMB, in contradiction to earlier claims that CMB heating will ease the detection of high-redshift CO. The full simulation of extragalactic CO lines and the predicted CO-LFs at any redshift can be accessed online (http://s-cubed.physics.ox.ac.uk/, go to “S3-SAX”) and they should be useful for the modeling of CO-line surveys with future telescopes, such as the Atacama Large Millimeter/submillimeter Array or the Square Kilometre Array.