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arXiv 2204.01649astro-ph.GAastro-ph.CO
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具有层析宇宙红外背景-星系互相关的宇宙星形成历史

Cosmic star formation history with tomographic cosmic infrared background-galaxy cross-correlation

Ziang Yan, Ludovic van Waerbeke, Angus H. Wright, Maciej Bilicki, Shiming Gu, Hendrik Hildebrandt, Abhishek S. Maniyar, Tilman Tröster

备注：
22 pages, 14 figures, 3 tables, the abstract is abridged, published on A&A
发表信息：
A&A 665, A52 (2022)
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摘要：

在这项工作中，我们探测宇宙的恒星形成的历史，利用层析交叉相关的宇宙红外背景（CIB）和星系样本。星系样本来自千度巡天（KiDS），而CIB地图则来自\planck \，即天空地图。我们在谐波空间中测量互相关，其显著性为43 $σ$。我们模拟的交叉相关性与晕模型，它将CIB各向异性的恒星形成率（SFR）和星系丰度。我们假设，SFR有一个对数正态依赖于晕质量，而星系丰度遵循晕占据分布（HOD）模型。互相关给出了$η_{\mathrm{max}}= 0.41^{+0.09}_{-0.14}$在晕质量$\log_{10}(M_{\mathrm{peak}}/M_{\odot})= {12.14\pm 0.36}$下的最佳拟合最大恒星形成效率。导出的恒星形成率密度（SFRD）被很好地约束到$z\sim 1.5$。在高红移的约束功率主要是由KiDS调查深度的限制。结合先前研究的外部SFRD测量值，得到$\log_{10}(M_{\mathrm{peak}}/M_{\odot})=12.42^{+0.35}_{-0.19}$。这将SFRD约束收紧到$z=4$，在$z=1.74^{+0.06}_{-0.02}$处产生$0.09_{-0.004}^{+0.003}\,M_{\odot} \mathrm { year }^{-1} \mathrm{Mpc}^{-3}$的峰值SFRD，对应于$10.05^{+0.12}_{-0.03}$ Gyr的回看时间。这两个约束是一致的，和SFRD同意与以前的研究和模拟。此外，我们估计的星系偏差$b$的KiDS星系的约束HOD参数，并产生一个增加的偏差从$z=0$ $b=1.1_{-0.31}^{+0.17}$在$z=1.5$的$b=1.96_{-0.64}^{+0.18}$。最后，我们提供了一个预测未来的星系调查，并得出结论，由于其相当大的深度，未来的调查将产生一个更严格的限制SFRD的演变。

英文摘要：

In this work, we probe the star formation history of the Universe using tomographic cross-correlation between the cosmic infrared background (CIB) and galaxy samples. The galaxy samples are from the Kilo-Degree Survey (KiDS), while the CIB maps are made from \planck\, sky maps. We measure the cross-correlation in harmonic space with a significance of 43$σ$. We model the cross-correlation with a halo model, which links CIB anisotropies to star formation rates (SFR) and galaxy abundance. We assume that SFR has a lognormal dependence on halo mass, while galaxy abundance follows the halo occupation distribution (HOD) model. The cross-correlations give a best-fit maximum star formation efficiency of $η_{\mathrm{max}}= 0.41^{+0.09}_{-0.14}$ at a halo mass $\log_{10}(M_{\mathrm{peak}}/M_{\odot})= {12.14\pm 0.36}$. The derived star formation rate density (SFRD) is well constrained up to $z\sim 1.5$. The constraining power at high redshift is mainly limited by the KiDS survey depth. A combination with external SFRD measurements from previous studies gives $\log_{10}(M_{\mathrm{peak}}/M_{\odot})=12.42^{+0.35}_{-0.19}$. This tightens the SFRD constraint up to $z=4$, yielding a peak SFRD of $0.09_{-0.004}^{+0.003}\,M_{\odot} \mathrm { year }^{-1} \mathrm{Mpc}^{-3}$ at $z=1.74^{+0.06}_{-0.02}$, corresponding to a lookback time of $10.05^{+0.12}_{-0.03}$ Gyr. Both constraints are consistent, and the derived SFRD agrees with previous studies and simulations. Additionally, we estimate the galaxy bias $b$ of KiDS galaxies from the constrained HOD parameters and yield an increasing bias from $b=1.1_{-0.31}^{+0.17}$ at $z=0$ to $b=1.96_{-0.64}^{+0.18}$ at $z=1.5$. Finally, we provide a forecast for future galaxy surveys and conclude that, due to their considerable depth, future surveys will yield a much tighter constraint on the evolution of the SFRD.

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