论文标题
宇宙恒星形成史与层析成像宇宙红外背景 - 跨与互相关
Cosmic star formation history with tomographic cosmic infrared background-galaxy cross-correlation
论文作者
论文摘要
在这项工作中，我们使用宇宙红外背景（CIB）和星系样品之间的层析成像互相关探测了宇宙的恒星形成历史。银河样品来自Kilo-Agree调查（儿童），而CIB地图由\ planck \，Sky Maps制成。我们测量谐波空间中的互相关，其显着性为43 $σ$。我们与晕圈模型对互相关进行建模，该模型将CIB各向异性与恒星形成速率（SFR）和星系丰度联系起来。我们假设SFR对光环质量具有对数正态依赖性，而星系丰度遵循Halo占用分布（HOD）模型。互相关给出了$η_{\ Mathrm {max}} = 0.41^{+0.09} _ { - 0.14} $的最佳最大恒星形成效率为$η 0.36} $。派生的星形速率密度（SFRD）受到$ z \ sim 1.5 $的限制。高红移的约束功率主要受孩子调查深度的限制。与以前研究的外部SFRD测量的结合给出了$ \ log_ {10}（M _ {\ Mathrm {peach}}}/m _ {\ odot}）= 12.42^{+0.35} _ { - 0.19} $。这将SFRD约束加强到$ z = 4 $，产生了$ 0.09 _ { - 0.004}^{+0.003} \，m _ {\ odot} \ Mathrm {eYalrm {eYal}^{ - 1}^{ - 1} \ Mathrm {mpc}^{mpc}^{-3} $ at的峰值SFRD的峰值SFRD的峰值SFRD峰值。 $ z = 1.74^{+0.06} _ { - 0.02} $，对应于$ 10.05^{+0.12} _ { - 0.03} $ gyr的回顾时间。这两种约束都是一致的，并且派生的SFRD与以前的研究和模拟一致。此外，我们从约束的HOD参数中估算了Galaxy偏见$ b $的儿童星系，并从$ b = 1.1 _ { - 0.31}^{+0.17} $ a $ z = 0 $ to $ z = 0 $ to $ b = 1 $ b = 1.96 _ = 1.96 _ { - 0.64}^{ - 0.64}^{+0.18} $ z $ z = 1.5 $ z = 1.5。最后，我们为未来的星系调查提供了一个预测，得出的结论是，由于其深度，未来的调查将对SFRD的演变产生严格的限制。
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.
