Detection of Cosmological 21 cm Emission with the Canadian Hydrogen Intensity Mapping Experiment-猫眼课题宝

DOI：

10.3847/1538-4357/acb13f

发表时间：

2022-02

期刊：

The Astrophysical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

Chime Collaboration;M. Amiri;K. Bandura;Tianyue Chen;M. Deng;M. Dobbs;M. Fandino;S. Foreman;M. Halpern;A. Hill;G. Hinshaw;Carolin Hofer;Joseph W. Kania;T. Landecker;Joshua MacEachern;K. Masui;J. Mena-Parra;N. Milutinovic;A. Mirhosseini;L. Newburgh;A. Ordog;U. Pen;T. Pinsonneault-Marotte;Ava Polzin;A. Reda;A. Renard;J. Shaw;S. Siegel;Saurabh Singh;K. Vanderlinde;Haochen Wang;D. Wiebe;D. Wulf

我们提出了一个检测21厘米发射的红移0.78和1.43之间的大尺度结构（LSS）与加拿大氢强度测绘实验。超过102个夜晚获得的射电观测被用来构建地图，这些地图是前景过滤和堆叠在发光红色星系（LRG），发射线星系（ELG）和类星体（QSO）的角度和光谱位置上的。我们发现决定性的证据时，堆叠在所有三个示踪剂的LSS，贝叶斯因子的对数等于18.9（LRG），10.8（ELG），和56.3（类星体）的检测。另一种基于似然比检验的频率论解释，产生了7.1σ（LRG），5.7σ（ELG）和11.1σ（QSO）的检测显著性。这些是用干涉仪进行的第一个21 cm强度映射测量。我们将中性氢的有效成团幅度定义为Ω HI，其中Ω HI是中性氢的宇宙丰度，B HI是中性氢的线性偏置，= 0.552表示红移空间畸变的线性效应.我们发现LRG（z = 0.84）的HI=1.51 - 0.97+3.60，ELG（z = 0.96）的HI=6.76 - 3.79+9.04，类星体（z = 1.20）的HI=1.68 - 0.67+1.10，其约束受到非线性尺度建模不确定性的限制。我们对每个示踪物的光谱红移的偏差也很敏感，我们发现类星体的非零偏差Δ v = − 66 ± 20 km s−1。我们将类星体目录分成三个红移仓，并在每个仓中进行了决定性的探测，z = 1.30的上仓产生了迄今为止最高的红移21 cm强度映射测量。

We present a detection of 21 cm emission from large-scale structure (LSS) between redshift 0.78 and 1.43 made with the Canadian Hydrogen Intensity Mapping Experiment. Radio observations acquired over 102 nights are used to construct maps that are foreground filtered and stacked on the angular and spectral locations of luminous red galaxies (LRGs), emission-line galaxies (ELGs), and quasars (QSOs) from the eBOSS clustering catalogs. We find decisive evidence for a detection when stacking on all three tracers of LSS, with the logarithm of the Bayes factor equal to 18.9 (LRG), 10.8 (ELG), and 56.3 (QSO). An alternative frequentist interpretation, based on the likelihood ratio test, yields a detection significance of 7.1σ (LRG), 5.7σ (ELG), and 11.1σ (QSO). These are the first 21 cm intensity mapping measurements made with an interferometer. We constrain the effective clustering amplitude of neutral hydrogen (H i), defined as HI≡103ΩHIbHI+〈fμ2〉 , where ΩH i is the cosmic abundance of H i, b H i is the linear bias of H i, and 〈f μ 2〉 = 0.552 encodes the effect of redshift-space distortions at linear order. We find HI=1.51−0.97+3.60 for LRGs (z = 0.84), HI=6.76−3.79+9.04 for ELGs (z = 0.96), and HI=1.68−0.67+1.10 for QSOs (z = 1.20), with constraints limited by modeling uncertainties at nonlinear scales. We are also sensitive to bias in the spectroscopic redshifts of each tracer, and we find a nonzero bias Δ v = − 66 ± 20 km s−1 for the QSOs. We split the QSO catalog into three redshift bins and have a decisive detection in each, with the upper bin at z = 1.30 producing the highest-redshift 21 cm intensity mapping measurement thus far.

Detection of Cosmological 21 cm Emission with the Canadian Hydrogen Intensity Mapping Experiment

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