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arXiv 1504.04516astro-ph.CO
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尘埃恒星形成星系团的成团演化

The Clustering Evolution of Dusty Star-Forming Galaxies

William I. Cowley, Cedric G. Lacey, Carlton M. Baugh, Shaun Cole

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21 pages, 18 figures, Accepted by MNRAS
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摘要：

我们提出了对通过远红外（FIR）和亚毫米波长发射选择的星系聚集的预测。这包括对这些波长下单碟望远镜的粗糙角分辨率引起的聚类偏差的影响的第一次预测。我们结合一个新版本的GALFORM模型的星系形成的自洽模型计算星际尘埃的吸收和再辐射。在$850$ $μ$ m处选择的模型星系位于质量为$M_{\rm halo}\sim10^{11.5}-10^{12}$ $h^{-1}$ M $_{\odot}$的暗物质晕中，与红移（对于$0.2\lesssim z\lesssim4$）或通量（对于$0.25\lesssim S_{850μ\rm m}\lesssim4$ mJy）无关。在$z\sim2.5$，最亮的星系（$S_{850μ\rm m}>4$ mJy）表现出$r_{0}=5.5_{-0.5}^{+0.3}$ $h^{-1}$ Mpc的相关长度，与观测结果一致。我们发现，这些星系的后代与恒星质量$M_{\star}\sim10^{11}$ $h^{-1}$ M $_{\odot}$占据晕跨越广泛的质量范围$M_{\rm halo}\sim10^{12}-10^{14}$ $h^{-1}$ M $_{\odot}$。在较短的波长（$250$，$350$和$500$ $μ$ m）的远红外辐射率也主要由星系晕质量范围$M_{\rm halo}\sim10^{11.5}-10^{12}$ $h^{-1}$ M $_{\odot}$，再次独立的红移（对于$0.5\lesssim z\lesssim5$）。我们比较了我们的预测宇宙红外背景各向异性的角功率谱在这些波长的观测，发现协议的$\sim2$在所有尺度和波长的一个因素内，改进了早期版本的模型。在$850$ $μ$ m模拟图像，我们表明，混淆的影响，提高测量的角度相关函数的所有尺度上的$\sim4$的一个因素。这具有重要的后果，可能导致推断的晕质量被高估了一个数量级。

英文摘要：

We present predictions for the clustering of galaxies selected by their emission at far infra-red (FIR) and sub-millimetre wavelengths. This includes the first predictions for the effect of clustering biases induced by the coarse angular resolution of single-dish telescopes at these wavelengths. We combine a new version of the GALFORM model of galaxy formation with a self-consistent model for calculating the absorption and re-emission of radiation by interstellar dust. Model galaxies selected at $850$ $μ$m reside in dark matter halos of mass $M_{\rm halo}\sim10^{11.5}-10^{12}$ $h^{-1}$ M$_{\odot}$, independent of redshift (for $0.2\lesssim z\lesssim4$) or flux (for $0.25\lesssim S_{850μ\rm m}\lesssim4$ mJy). At $z\sim2.5$, the brightest galaxies ($S_{850μ\rm m}>4$ mJy) exhibit a correlation length of $r_{0}=5.5_{-0.5}^{+0.3}$ $h^{-1}$ Mpc, consistent with observations. We show that these galaxies have descendants with stellar masses $M_{\star}\sim10^{11}$ $h^{-1}$ M$_{\odot}$ occupying halos spanning a broad range in mass $M_{\rm halo}\sim10^{12}-10^{14}$ $h^{-1}$ M$_{\odot}$. The FIR emissivity at shorter wavelengths ($250$, $350$ and $500$ $μ$m) is also dominated by galaxies in the halo mass range $M_{\rm halo}\sim10^{11.5}-10^{12}$ $h^{-1}$ M$_{\odot}$, again independent of redshift (for $0.5\lesssim z\lesssim5$). We compare our predictions for the angular power spectrum of cosmic infra-red background anisotropies at these wavelengths with observations, finding agreement to within a factor of $\sim2$ over all scales and wavelengths, an improvement over earlier versions of the model. Simulating images at $850$ $μ$m, we show that confusion effects boost the measured angular correlation function on all scales by a factor of $\sim4$. This has important consequences, potentially leading to inferred halo masses being overestimated by an order of magnitude.

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