从LambdaCDM对赫歇尔的预测：揭开宇宙恒星形成历史
Predictions for Herschel from LambdaCDM: unveiling the cosmic star formation history
摘要：
我们使用一个基于LambdaCDM宇宙学的远红外星系演化模型，对赫歇尔空间天文台即将进行的宇宙学调查进行详细的预测。我们使用GALFORM半解析星系形成模型和GRASIL分光光度计程序计算星系的SED，包括尘埃对辐射的再加工。该模型与Baugh et al.（2005）的模型相同，假设了两种不同的IMF：一种是正常的太阳邻域IMF，用于盘状静止恒星的形成;另一种是非常头重脚轻的IMF，用于星系合并引发的恒星爆发。我们以前已经表明，头重脚轻的IMF似乎是必要的，以解释数量计数和暗亚毫米星系的红移。在本文中，我们提出的星系光度函数，数计数和红移分布的赫歇尔成像带的预测。我们发现，源混淆将是一个严重的问题，在最深的计划调查。我们还显示了预测的物理性质，如恒星形成率和恒星，气体和晕质量，以及在其他波长（从远紫外线到无线电）相关的多波长后续观测通量。我们研究了在宇宙历史上，尘埃和大质量恒星形成的总红外辐射中有多少部分应该通过赫歇尔计划的巡天来解决，并发现了一个分数~30- 50%，这取决于混乱。最后，我们表明，星系在赫歇尔调查应显着集群。
英文摘要：
We use a model for the evolution of galaxies in the far-IR based on the LambdaCDM cosmology to make detailed predictions for upcoming cosmological surveys with the Herschel Space Observatory. We use the combined GALFORM semi-analytical galaxy formation model and GRASIL spectrophotometric code to compute galaxy SEDs including the reprocessing of radiation by dust. The model, which is the same as that in Baugh et al. (2005), assumes two different IMFs: a normal solar neighbourhood IMF for quiescent star formation in disks, and a very top-heavy IMF in starbursts triggered by galaxy mergers. We have shown previously that the top-heavy IMF appears necessary to explain the number counts and redshifts of faint sub-mm galaxies. In this paper, we present predictions for galaxy luminosity functions, number counts and redshift distributions in the Herschel imaging bands. We find that source confusion will be a serious problem in the deepest planned surveys. We also show predictions for physical properties such as star formation rates and stellar, gas and halo masses, together with fluxes at other wavelengths (from the far-UV to the radio) relevant for multi-wavelength follow-up observations. We investigate what fraction of the total IR emission from dust and of the high-mass star formation over the history of the Universe should be resolved by planned surveys with Herschel, and find a fraction ~30-50%, depending on confusion. Finally, we show that galaxies in Herschel surveys should be significantly clustered.
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