论文标题
使用$ \ MATHTT {GALWCAT19} $ optical-spectrosproscopic SDSS目录中的$ω_m$和$σ_8$的宇宙学约束
Cosmological Constraint on $Ω_m$ and $σ_8$ from Cluster Abundances using the $\mathtt{GalWCat19}$ Optical-Spectroscopic SDSS Catalog
论文作者
论文摘要
我们使用$ \ mathtt {galwcat19} $获得了对物质密度的宇宙学限制，以及波动的振幅，\ sig，我们在Sloan Digital Sky Survey-Dry13 specy-Dr13 spectroscic数据集中确定的1800个星系群集的目录，该目录是我们在Sloan Digital Sumple-Dry13 spectroscic数据集中确定的。 \ citep {abdullah18，abdullah19}。通过分析756个簇的子样本，红移范围为$ 0.045 \ leq z \ leq 0.125 $和$ m \ geq 0.8 \ geq 0.8 \ times10^{14} $ \ hm〜的病毒质量，平均红色速度为$ z = 0.085 $ \ pm 0.041 $（系统）和\ sig〜 $ = 0.810^{+0.031} _ { - 0.036} \ pm 0.035 $（系统），集群归一化关系为$σ_8= 0.43ω_m^{ - 0.55} $。我们的方法有几个独特的方面：我们使用当前可用的最大光谱数据集，并且我们使用加工技术分配了会员资格，我们证明我们非常有效地同时最大化{\ it {bona fide}}群集成员的数量，同时最大程度地减少污染的interpopers的数量。此外，我们没有使用缩放关系，而是使用病毒质量估计器分别计算簇质量。由于$ \ mathtt {galwcat19} $是一个低红色群集目录，因此我们不需要在宇宙参数或集群本身的属性中对进化做出任何假设。我们对\ om〜和\ sig〜的约束与从非群集丰度宇宙学探针（例如宇宙微波背景（CMB），Baryonic声学振荡（BAO）（BAO）和Supernovae（SNE）等获得的非群集丰度宇宙学探针相关。与Planck18+Bao+Pantheon对我们的群集数据的联合分析给出了\ om〜 $ = 0.315^{+0.013} _ { - 0.011} $和\ sig〜 $ = 0.810^{+0.810^{+0.011} _ { - 0.010} $。
We derive cosmological constraints on the matter density, \om, and the amplitude of fluctuations, \sig, using $\mathtt{GalWCat19}$, a catalog of 1800 galaxy clusters we identified in the Sloan Digital Sky Survey-DR13 spectroscopic data set using our GalWeight technique to determine cluster membership \citep{Abdullah18,Abdullah19}. By analyzing a subsample of 756 clusters in a redshift range of $0.045\leq z \leq 0.125$ and virial masses of $M\geq 0.8\times10^{14}$ \hm ~with mean redshift of $z = 0.085$, we obtain \om ~$=0.310^{+0.023}_{-0.027} \pm 0.041$ (systematic) and \sig ~$=0.810^{+0.031}_{-0.036}\pm 0.035$ (systematic), with a cluster normalization relation of $σ_8= 0.43 Ω_m^{-0.55}$. There are several unique aspects to our approach: we use the largest spectroscopic data set currently available, and we assign membership using the GalWeight technique which we have shown to be very effective at simultaneously maximizing the number of {\it{bona fide}} cluster members while minimizing the number of contaminating interlopers. Moreover, rather than employing scaling relations, we calculate cluster masses individually using the virial mass estimator. Since $\mathtt{GalWCat19}$ is a low-redshift cluster catalog we do not need to make any assumptions about evolution either in cosmological parameters or in the properties of the clusters themselves. Our constraints on \om ~and \sig ~are consistent and very competitive with those obtained from non-cluster abundance cosmological probes such as Cosmic Microwave Background (CMB), Baryonic Acoustic Oscillation (BAO), and supernovae (SNe). The joint analysis of our cluster data with Planck18+BAO+Pantheon gives \om ~$=0.315^{+0.013}_{-0.011}$ and \sig ~$=0.810^{+0.011}_{-0.010}$.
