We present a sound horizon independent measurement of the Hubble parameter using a multiprobe large-scale structure analysis. Removing the dependency on the sound horizon with a rescaling procedure at the matter power spectrum level, we analyse the BOSS full-shape power spectrum and bispectrum (for the first time) using the effective field theory of large-scale structure up to one loop. We combine this analysis with the auto- and cross-angular power spectra from the DESI Legacy Imaging Survey DR9, the $3 \times 2$pt analysis from DES Y3, and the CMB gravitational lensing power spectrum from Planck PR3. Our baseline analysis, that does not rely on supernovae data, yields $h = 0.702^{+0.022}_{-0.024}$, $Ω_m = 0.310 \pm 0.013$, and $σ_8 = 0.799 \pm 0.020$, corresponding to $3-4 \%$ precision measurements. When adding supernovae data from Pantheon+, we obtain a $2.6 \%$ measurement of $h$, with $h = 0.686 \pm 0.018$. We further note that our EFTBOSS analysis indicates a slight deviation of the BAO scale parameter (at $1.8 σ$) from its $Λ$CDM value, caused by the small scales of the bispectrum. We finally use the sound horizon-free EFTBOSS analysis as a diagnosis for the presence of new physics, finding that our results are consistent with the recent hints of evolving dark energy.
Geometrical compression: a new method to enhance the BOSS galaxy bispectrum monopole constraints
我们提出了一种新的方法来压缩星系聚类三点统计，并将其应用到红移空间星系双谱测量从BOSS DR 12 CMASS数据考虑$k$ -空间范围的$0.03-0.12\,h/\mathrm{Mpc}$。该方法包括在binning在一起的双谱评价在组的波数形成封闭的三角形具有类似的几何性质：面积，余弦的最大角度和馀下两个角度的余弦之间的比率。这使得我们能够增加双谱测量的数量，例如通过标准分箱（从使用的116到2734个三角形）的因子$23$，否则标准分箱受限于可用于估计导出参数约束所需的协方差矩阵的模拟目录的数量。因此，推断参数$\left(b_1,b_2,f,σ_8\right)$的$68\%$可信区间分别减少了$\left(-39\%,-49\%,-29\%,-22\%\right)$。我们发现非常好的协议与最近获得的替代最大压缩方法的后验。这种新的方法不需要先验计算的数据向量协方差矩阵，并有可能直接适用于其他三点统计（如glaxy聚类，弱引力透镜，21厘米发射线）从未来的调查，如DESI，欧几里德，PFS和SKA测量。
We use analytic covariance matrices to carry out a full-shape analysis of the galaxy power spectrum multipoles from the Baryon Oscillation Spectroscopic Survey (BOSS). We obtain parameter estimates that agree well with those based on the sample covariance from two thousand galaxy mock catalogs, thus validating the analytic approach and providing substantial reduction in computational cost. We also highlight a number of additional advantages of analytic covariances. First, the analysis does not suffer from sampling noise, which biases the constraints and typically requires inflating parameter e…
The DES-CMASS sample (DMASS) is designed to optimally combine the weak lensing measurements from the Dark Energy Survey (DES) and redshift-space distortions (RSD) probed by the CMASS galaxy sample from the Baryonic Oscillation Spectroscopic Survey (BOSS). In this paper, we demonstrate the feasibility of adopting DMASS as the equivalent of BOSS CMASS for a joint analysis of DES and BOSS in the framework of modified gravity. We utilize the angular clustering of the DMASS galaxies, cosmic shear of the DES METACALIBRATION sources, and cross-correlation of the two as data vectors. By jointly fittin…
Measurement of the Weyl Potential Evolution and $E_G$ Statistic from KiDS-1000, BOSS and 2dFLenS
State Key Laboratory of Radio Astronomy and Technology, Xinjiang Astronomical Observatory, Chinese Academy of Sciences（中国科学院新疆天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Xinjiang University（新疆大学）；Henan University（河南大学）
Primordial power spectrum reconstructions from BOSS + eBOSS
Instituto de Física de Cantabria, CSIC-Universidad de Cantabria（坎塔布里亚物理研究所，西班牙国家研究委员会-坎塔布里亚大学）；Departamento de Física Moderna, Universidad de Cantabria（坎塔布里亚大学现代物理系）；Universitat de Barcelona（巴塞罗那大学）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚空间研究院）；Institut de Ciències del Cosmos (ICCUB), Universitat de Barcelona (UB)（巴塞罗那大学宇宙科学研究所）
We present the analysis of the full shape of anisotropic clustering measurement from the extended Baryon Oscillation Spectroscopic Survey (eBOSS) quasar sample together with the combined galaxy sample from the Baryon Oscillation Spectroscopic Survey (BOSS), re-analysed using an updated recipe for the non-linear matter power spectrum and the non-local bias parameters. We obtain constraints for flat $Λ$CDM cosmologies, focusing on the cosmological parameters that are independent of the Hubble parameter $h$. Our recovered value for the RMS linear perturbation theory variance as measured on the sc…
We present an effective model for the one-dimensional Lyman-$α$ flux power spectrum far above the baryonic Jeans scale. The main new ingredient is constituted by a set of two parameters that encode the impact of small, highly non-linear scales on the one-dimensional power spectrum on large scales, where it is measured by BOSS. We show that, by marginalizing over the model parameters that capture the impact of the intergalactic medium, the flux power spectrum from both simulations and observations can be described with high precision. The model displays a degeneracy between the neutrino masses …
The Effect of Interstellar Absorption on Measurements of the Baryon Acoustic Peak in the Lyman-α Forest
近年来，人们利用氢Lyman-α森林的自相关性，利用BOSS巡天的数万条类星体谱，观测到了红移2 < z < 3.5的重子声峰。然而，银河系的星际介质会将吸收线引入任何河外源的光谱中。这些谱线虽然很弱，在单一BOSS光谱中无法检测到，但可能会使宇宙学信号产生偏差。为了检验这一点，我们通过叠加超过一百万个星系和类星体的光谱来生成吸收线图。我们发现，系统介绍太小，影响目前的重子声学峰值的准确性，但可能是相关的未来调查，如暗能量光谱仪（DESI）。我们概述了一种方法来解释这与未来的数据集。
We present the calibration of the Dark Energy Survey Year 3 (DES Y3) weak lensing source galaxy redshift distributions $n(z)$ from clustering measurements. In particular, we cross-correlate the weak lensing (WL) source galaxies sample with redMaGiC galaxies (luminous red galaxies with secure photometric redshifts) and a spectroscopic sample from BOSS/eBOSS to estimate the redshift distribution of the DES sources sample. Two distinct methods for using the clustering statistics are described. The first uses the clustering information independently to estimate the mean redshift of the source gala…
Constraining and Comparing the Dynamical Dark Energy and f(R) Modified Gravity Models with Cosmological Distance Measurements
National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Department of Physics, College of Sciences, Northeastern University（东北大学理学院物理系）
We present clustering redshift measurements for Dark Energy Survey (DES) lens sample galaxies to be used in weak gravitational lensing and galaxy clustering studies. To perform this measurement, we cross-correlate with spectroscopic galaxies from the Baryon Acoustic Oscillation Survey (BOSS) and its extension, eBOSS. We validate our methodology in simulations, including a new technique to calibrate systematic errors due to the galaxy clustering bias, finding our method to be generally unbiased in calibrating the mean redshift. We apply our method to the data, and estimate the redshift distribu…
Estimating the power spectrum covariance matrix with fewer mock samples
星系巡天测量功率谱（P（k））的协方差矩阵在理论上很难计算。目前的最佳实践是通过计算大量模拟目录的样本协方差来估计协方差矩阵。下一代星系巡天将需要数千个大体积模型来确定协方差矩阵，以达到所需的精度。逆协方差矩阵中的误差更大，并且随着P（k）箱的数量而缩放，使得问题更加尖锐。我们开发了一种估计协方差矩阵的方法，使用理论上合理的，少参数模型，校准与模拟目录。使用一组600个BOSS DR 11模拟星表，我们证明了一个七参数模型足以拟合BOSS DR 11 P（k）测量的协方差矩阵。使用此方法计算的协方差优于任何模拟数量的样本协方差，并且仅需要~100个模拟就可以完全收敛，并且逆协方差矩阵以相同的速率收敛。这种方法应该同样适用于下一代星系调查，尽管对更高精度的需求可能需要在拟合函数中添加额外的参数。
We evaluate the consistency between lensing and clustering probes of large-scale structure based on measurements of projected galaxy clustering from BOSS combined with overlapping galaxy-galaxy lensing from three surveys: DES Y3, HSC Y1, and KiDS-1000. An intra-lensing-survey study finds good agreement between these lensing data. We model the observations using the Dark Emulator and fit the data at two fixed cosmologies: Planck, with $S_8=0.83$, and a Lensing cosmology with $S_8=0.76$. For a joint analysis limited to scales with $R>5.25h^{-1}$Mpc, we find that both cosmologies provide an accep…
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: combining correlated Gaussian posterior distributions
包含在各向异性星系团测量的宇宙学信息往往可以压缩成少量的参数，其后验分布是很好地描述了高斯。我们提出了一个一般的方法来结合这些估计到一个单一的一组共识约束，编码的总信息的个人测量，考虑到不同的方法之间的完整的协方差。我们说明了这种技术，应用它来结合从不同的聚类分析，包括测量的签名的重子声学振荡（BAO）和红移空间扭曲（RSD），最终SDSS-III重子振荡光谱巡天（BOSS）的一组模拟目录的基础上得到的结果。我们的研究结果表明，由共识约束所允许的参数空间的区域小于单个方法的区域，这突出了即使在测量高度相关的情况下，对星系调查进行多重分析的重要性。本文是分析BOSS最终星系聚类数据集的一部分。这里提出的方法在Alam et al.（2016）中用于从BOSS产生最终的宇宙学约束。
Spectral Classification and Redshift Measurement for the SDSS-III Baryon Oscillation Spectroscopic Survey
我们描述了斯隆数字巡天III（SDSS-III）的重子振荡光谱巡天（BOSS）使用的自动光谱分类，红移测定和参数测量管道，截至数据发布9，包含831，000个中等分辨率光谱。我们给出了一个审查的算法，并描述的变化，已实施BOSS相对于以前的SDSS-I/II版本，包括新的恒星，星系和类星体红移模板的管道。对于BOSS为大尺度宇宙学测量而瞄准的红移0.4 <~ z <~ 0.8的大质量星系的颜色选择的CMASS样本，管道实现了98.7%的自动分类成功率，并确认了95.4%的独特CMASS目标是星系（其余大部分是M星）。基于对BOSS星系的一个子集的目视检查，我们发现~0.2%的CMASS样本分类和红移是不正确的，并且~0.4%的CMASS光谱是当前算法未分类的对象，这些对象可能是可恢复的。BOSS管道证实，约51.5%的类星体目标具有类星体光谱，其余主要由恒星组成。对于星系和类星体来说，由光子噪声传播的统计（而不是系统）红移误差通常为几十km/s，对于类星体来说，有一个明显的尾巴，达到几百km/s。我们使用重复观测来测试这些统计红移误差估计的准确性，发现它们被低估了1.19到1.34倍的星系，和2倍的类星体。我们评估了天空减法质量，S/N和其他因素对星系红移成功的影响。最后，我们记录已知的问题，并描述正在进行的发展方向。
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: Cosmological implications of the Fourier space wedges of the final sample
The scattering of cosmic microwave background (CMB) photons off the free-electron gas in galaxies and clusters leaves detectable imprints on high resolution CMB maps: the thermal and kinematic Sunyaev-Zel'dovich effects (tSZ and kSZ respectively). We use combined microwave maps from the Atacama Cosmology Telescope (ACT) DR5 and Planck in combination with the CMASS and LOWZ galaxy catalogs from the Baryon Oscillation Spectroscopic Survey (BOSS DR10 and DR12), to study the gas associated with these galaxy groups. Using individual reconstructed velocities, we perform a stacking analysis and rejec…
We prove from the modified gravity (MG) galaxy/halo mock catalogs that the shape of the pairwise kinematic Sunyaev-Zeldovich (kSZ) power spectrum $P_{\rm kSZ}$ has constraining power on discriminating different gravity theories on cosmological scales. By varying the effective optical depth $τ_{\rm T}$ as a free parameter, we verify that the $τ_{\rm T}$-$f$ (the linear growth rate) degeneracy in the linear theory of $P_{\rm kSZ}$ is broken down by the non-linear structure growth and the scale-dependence of $f$ in some MG theories. Equivalently speaking, the shape of $P_{\rm kSZ}$ alone could be…
Preference for evolving dark energy in light of the galaxy bispectrum
University of Science and Technology of China（中国科学技术大学）；CAS Key Laboratory for Research in Galaxies and Cosmology, School of Astronomy and Space Science, University of Science and Technology of China（中国科学院星系与宇宙学重点实验室，中国科学技术大学天文与空间科学学院）；Deep Space Exploration Laboratory（深空探测实验室）；Laboratoire Univers & Particules de Montpellier, CNRS & Université de Montpellier（蒙彼利埃宇宙与粒子实验室，法国国家科学研究中心与蒙彼利埃大学）；ETH Zürich（苏黎世联邦理工学院）；Università degli Studi di Milano（米兰大学）
