具有亚毫米星系放大偏差的宇宙学：层析分析
Cosmology with the sub-millimetre galaxies magnification bias: Tomographic Analysis
摘要：
与Gonzalez-Nuevo等人2017和Bonavera等人2019一样，由于它们的放大偏差，高z亚毫米星系可以用作引力透镜研究的背景样本。特别是，在Bonavera et al. 2020中，可以利用放大偏差来约束晕占据分布（HOD）模型的自由参数和一些主要的宇宙学参数。在这项工作中，放大率偏差已被评估为宇宙学工具，在层析成像设置。互相关函数（CCF）数据已被用来联合约束天体物理参数$M_{min}$，$M_{1}$和$α$在每个选定的红移箱和$Ω_{M}$，$σ_{8}$和$H_0$宇宙学的（$Λ$ CDM）.此外，我们还探讨了在联合分析（$ω_0$ CDM和$ω_0ω_a$ CDM）中引入$ω_0, ω_a$参数的暗能量密度的可能的时间演化。我们测量了一个GAMA星系的前景光谱样本和一个测光红移>1.2的H-ATLAS星系样本之间的CCF，GAMA星系的前景光谱样本被分成四个红移仓（0.1-0.2，0.2-0.3，0.3-0.5和0.5-0.8）。CCF的建模使用的描述，取决于HOD和宇宙学参数，估计与MCMC在不同的情况下。对于$Λ$ CDM模型，分析得出的最大后验值为0.26，$[0.17,0.41]$ 68\%C. I。$Ω_M$为0.87，$[0.75,1]$为68\%C. I.关于PDMATHAMBMZ根据我们目前的结果，$H_0$尚未受到限制。对于$ω_0$ CDM模型，对$Ω_M$和$σ_8$的约束是相似的，但是我们发现$ω_0$的最大后验值为-1，其中$[-1.56, -0.47]$ 68\%C. I.在$ω_0ω_a$ CDM模型中，结果为-1.09，其中$[-1.72, -0.66]$ 68\%CI对$ω_0$和对$[-1.88, 1.48]$ 68\%C. I.关于$ω_a$
英文摘要：
As in Gonzalez-Nuevo et al. 2017 and Bonavera et al. 2019, the high-z sub-millimetre galaxies can be used as background sample for gravitational lensing studies thanks to their magnification bias. In particular, as in Bonavera et al. 2020 the magnification bias can be exploited in order to constrain the free parameters of a Halo Occupation Distribution (HOD) model and some of the main cosmological parameters. In this work the magnification bias has been evaluated as cosmological tool in a tomographic set up. The cross-correlation function (CCF) data have been used to jointly constrain the astrophysical parameters $M_{min}$, $M_{1}$ and $α$ in each one of the selected redshift bins and the $Ω_{M}$, $σ_{8}$, and $H_0$ cosmological ones ($Λ$CDM). Moreover, we explore the possible time evolution of the dark energy density introducing also the $ω_0, ω_a$ parameters in the joint analysis ($ω_0$CDM and $ω_0ω_a$CDM). The CCF has been measured between a foreground spectroscopic sample of GAMA galaxies that has been divided into four redshift bins (0.1-0.2, 0.2-0.3, 0.3-0.5 and 0.5-0.8) and a sample of H-ATLAS galaxies with photometric redshifts >1.2. The CCF is modelled using a description that depends on HOD and cosmological parameters that are estimated with MCMC in different cases. For the $Λ$CDM model, the analysis yields a maximum posterior value at 0.26 with $[0.17,0.41]$ 68\% C.I. for $Ω_M$ and at 0.87 with $[0.75,1]$ 68\% C.I. for $σ_8$. With our current results $H_0$ is not yet constrained. With the $ω_0$CDM model, the constraints on $Ω_M$ and $σ_8$ are similar, but we found a maximum posterior value for $ω_0$ at -1 with $[-1.56, -0.47]$ 68\% C.I. In the $ω_0ω_a$CDM model, the results are -1.09 with $[-1.72, -0.66]$ 68\% C.I. for $ω_0$ and -0.19 with $[-1.88, 1.48]$ 68\% C.I. for $ω_a$.
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