We present cosmological constraints from a joint analysis of the pre- and post-reconstruction galaxy power spectrum multipoles from the final data release of the Baryon Oscillation Spectroscopic Survey (BOSS). Geometric constraints are obtained from the positions of BAO peaks in reconstructed spectra, analyzed in combination with the unreconstructed spectra in a full-shape (FS) likelihood using a joint covariance matrix, giving stronger parameter constraints than FS-only or BAO-only analyses. We introduce a new method for obtaining constraints from reconstructed spectra based on a correlated theoretical error, which is shown to be simple, robust, and applicable to any flavor of density-field reconstruction. Assuming $\Lambda$CDM with massive neutrinos, we analyze data from two redshift bins $z_\mathrm{eff}=0.38,0.61$ and obtain $1.6\%$ constraints on the Hubble constant $H_0$, using only a single prior on the current baryon density $\omega_b$ from Big Bang Nucleosynthesis (BBN) and no knowledge of the power spectrum slope $n_s$. This gives $H_0 = 68.6\pm1.1\,\mathrm{km\,s}^{-1}\mathrm{Mpc}^{-1}$, with the inclusion of BAO data sharpening the measurement by $40\%$, representing one of the strongest current constraints on $H_0$ independent of cosmic microwave background data. Restricting to the best-fit slope $n_s$ from Planck (but without additional priors on the spectral shape), we obtain a $1\%$ $H_0$ measurement of $67.8\pm 0.7\,\mathrm{km\,s}^{-1}\mathrm{Mpc}^{-1}$. We find strong constraints on the cosmological parameters from a joint analysis of the FS, BAO, and Planck data. This sets new bounds on the sum of neutrino masses $\sum m_\nu < 0.14\,\mathrm{eV}$ (at $95\%$ confidence) and the effective number of relativistic degrees of freedom $N_\mathrm{eff} = 2.90^{+0.15}_{-0.16}$, though contours are not appreciably narrowed by the inclusion of BAO data.

中文翻译：

---

结合星系功率谱的全形状和 BAO 分析：对 H0 的 1.6% CMB 独立约束

我们通过对重子振荡光谱调查 (BOSS) 最终数据发布的重建前和重建后星系功率谱多极子的联合分析，提出了宇宙学约束。从重构光谱中 BAO 峰的位置获得几何约束，并使用联合协方差矩阵在全形状 (FS) 似然中结合未重构光谱进行分析，提供比仅 FS 或仅 BAO 分析更强的参数约束。我们引入了一种基于相关理论误差从重构光谱中获取约束的新方法，该方法被证明简单、稳健，并且适用于任何类型的密度场重构。假设 $\Lambda$CDM 具有大量中微子，我们分析来自两个红移箱 $z_\mathrm{eff}=0.38,0.61$ 的数据并获得 $1。6\%$ 对哈勃常数 $H_0$ 的约束，仅使用来自大爆炸核合成 (BBN) 的当前重子密度 $\omega_b$ 的单个先验，并且不知道功率谱斜率 $n_s$。这给出了 $H_0 = 68.6\pm1.1\,\mathrm{km\,s}^{-1}\mathrm{Mpc}^{-1}$，包含 BAO 数据使测量值锐化了 $40\% $，代表独立于宇宙微波背景数据的 $H_0$ 目前最强的约束之一。限制到普朗克的最佳拟合斜率 $n_s$（但在光谱形状上没有额外的先验），我们获得了 $1\%$ $H_0$ 测量值 $67.8\pm 0.7\,\mathrm{km\,s}^ {-1}\mathrm{Mpc}^{-1}$。通过对 FS、BAO 和普朗克数据的联合分析，我们发现了对宇宙学参数的强烈限制。这为中微子质量 $\sum m_\nu < 0.14\ 的总和设置了新的界限，