自调节重子坍缩模型中亚毫米星系的成团
Clustering of sub-millimeter galaxies in a self-regulated baryon collapse model
摘要：
我们在Granato等人（2004）的原球状星系物理演化模型框架下研究了宇宙红外背景（CIB）各向异性。在使用散粒噪声幅度的可用确定重新校准了在$λ\ge 850\,μ$ m处的累积通量函数$dS/dz$之后（原始模型已经在较短波长下正确地再现了它）通过{ \it Planck}、{ \it Herschel}、SPT和ACT实验测量的在从$250\,μ$ m到$2\,$ mm的波长处的CIB功率谱已经使用仅具有2个自由参数的晕模型来拟合，最小晕质量和卫星星系平均占有函数的幂律指数。最佳拟合{ \it最小值}晕质量为$\log(M_{\rm min}/M_\odot) = 12.24 \pm 0.06$，高于Amblard等人（2011）的估计值，但在误差范围内一致，接近普朗克合作组织（2011）的估计值。由该模型得到的星系体发射率的红移演化与由数据推断的结果一致。导出的$z\simeq 2$亚毫米星系的{ \it有效}晕质量，$M_{\rm eff} \simeq 5\times 10^{12}\,M_\odot$，接近于在相同的红移下对最有效的恒星形成者的估计。的有效偏置因子和共动集群半径在$z\simeq 2$产生的模型是大大低于发现的模型，恒星形成的燃料稳定的气体吸积，但大大高于合并驱动的星系演化与头重脚轻的初始质量函数。
英文摘要：
We have investigated the Cosmic Infrared Background (CIB) anisotropies in the framework of the physical evolutionary model for proto-spheroidal galaxies by Granato et al. (2004). After having re-calibrated the cumulative flux function $dS/dz$ at $λ\ge 850\,μ$m using the available determinations of the shot noise amplitude (the original model already correctly reproduces it at shorter wavelengths) the CIB power spectra at wavelengths from $250\,μ$m to $2\,$mm measured by {\it Planck}, {\it Herschel}, SPT and ACT experiments have been fitted using the halo model with only 2 free parameters, the minimum halo mass and the power-law index of the mean occupation function of satellite galaxies. The best-fit {\it minimum} halo mass is $\log(M_{\rm min}/M_\odot) = 12.24 \pm 0.06$, higher than, but consistent within the errors, with the estimate by Amblard et al. (2011) and close to the estimate by Planck Collaboration (2011). The redshift evolution of the volume emissivity of galaxies yielded by the model is found to be consistent with that inferred from the data. The derived {\it effective} halo mass, $M_{\rm eff} \simeq 5\times 10^{12}\,M_\odot$, of $z\simeq 2$ sub-millimeter galaxies is close to that estimated for the most efficient star-formers at the same redshift. The effective bias factor and the comoving clustering radius at $z\simeq 2$ yielded by the model are substantially lower than those found for a model whereby the star formation is fueled by steady gas accretion, but substantially higher than those found for a merging-driven galaxy evolution with a top-heavy initial mass function.
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