标题： 重新分析DESI DR1：1。 $Λ$CDM 限制来自功率谱和三阶谱 显示英文标题

标题： Reanalyzing DESI DR1: 1. $Λ$CDM Constraints from the Power Spectrum and Bispectrum

摘要： 我们对DESI数据发布1中的星系聚类数据进行了首次独立再分析，采用基于有效场理论（EFT）的全形状模型。 我们使用基于窗口去卷积准最优估计器的自定义流程分析公共目录的功率谱和三阶谱，仔细考虑所有相关的系统效应。 与官方合作分析相比，我们增加了星系功率谱的十六极矩和三阶谱的单极矩，并引入了一种新的纤维碰撞随机估计器，这有助于进行稳健的三阶谱分析。 作为首次应用，我们在标准宇宙学模型，$\Lambda$CDM的背景下，对DESI的功率谱和三阶谱进行了基于EFT的全形状分析。 利用物理重子密度和原初功率谱倾斜度的外部先验，我们将物质密度比例限制为$\Omega_m=0.284\pm 0.011$，哈勃常数限制为$h=0.707\pm 0.011$，并将质量波动幅度限制为$\sigma_8=0.811\pm 0.030$。 双谱对参数估计有明显影响：它使$\sigma_8$和$\Omega_m$的约束变紧，提高了$\approx 10$%，并将$\Omega_m$向 Planck$\Lambda$CDM 值移动了$\approx 1\sigma$。 将我们的全形状似然与官方 DESI DR2 BAO 测量结果相结合，宇宙学参数进一步向\textit{普朗克}值移动，其中$\Omega_m=0.296\pm 0.007$，$h=0.688\pm 0.006$，$\sigma_8=0.818\pm 0.029$（在联合分析中获得更紧的约束）。 最后，星系三阶矩数据显著提高了二次偏差参数的测量，这些参数与晕占有率分布模型的预测一致。 我们的工作突显了高阶统计的重要性，并为未来非最小宇宙学模型的全形状分析奠定了基础。 显示英文摘要

摘要： We present the first independent re-analysis of the galaxy clustering data from DESI Data Release 1, utilizing an effective field theory (EFT)-based full-shape model. We analyze the power spectra and bispectra of the public catalogs using a custom-built pipeline based on window-deconvolved quasi-optimal estimators, carefully accounting for all relevant systematic effects. Compared to the official collaboration analysis, we add the galaxy power spectrum hexadecapole and the bispectrum monopole, and also introduce a novel stochastic estimator for fiber collisions, which facilitates robust bispectrum analyses. As a first application, we perform an EFT-based full-shape analysis of the DESI power spectra and bispectra in the context of the standard cosmological model, $\Lambda$CDM. Using external priors on the physical baryon density and the primordial power spectrum tilt, we constrain the matter density fraction to $\Omega_m=0.284\pm 0.011$, the Hubble constant to $h=0.707\pm 0.011$, and the mass fluctuation amplitude to $\sigma_8=0.811\pm 0.030$. The bispectrum has a noticeable effect on parameter estimation: it sharpens the constraints on $\sigma_8$ and $\Omega_m$ by $\approx 10$\% and shifts $\Omega_m$ by $\approx 1\sigma$ towards the Planck $\Lambda$CDM value. Combining our full-shape likelihood with the official DESI DR2 BAO measurements, cosmological parameters shift further towards the \textit{Planck} values, with $\Omega_m=0.296\pm 0.007$, $h=0.688\pm 0.006$, $\sigma_8=0.818\pm 0.029$ (with tighter constraints obtained in joint analyses). Finally, the galaxy bispectrum data dramatically improves measurements of quadratic bias parameters, which are consistent with predictions from halo occupation distribution models. Our work highlights the importance of higher-order statistics and sets the stage for upcoming full-shape analyses of non-minimal cosmological models.