标题： 重子声波振荡在断层角密度和红移涨落中 显示英文标题

标题： Baryon Acoustic Oscillations in tomographic Angular Density and Redshift Fluctuations

摘要： 在本研究中，我们研究了二维角度和红移空间 $\{\theta, \Delta z\}$ 中的重子声学振荡 (BAO)，其中 $\Delta z$ 表示两个给定角度壳层之间的红移差。 因此，我们在大尺度结构 (LSS) 的层析成像分析背景下开展工作，其中数据被切片到不同的红移壳层中，并从两个不同探测器的自角和交叉角光谱中提取宇宙学约束，这两个探测器分别是标准星系角密度涨落 (ADF，或二维聚类) 和星系角红移涨落 (ARF)。 对于这两个可观测量，我们首次研究了 BAO 峰值如何在 $\{\theta, \Delta z\}$ 平面中出现。 尽管这是一个较弱的特征（尤其对于 $\Delta z \neq 0$），但 Fisher 预测分析表明，先验地，关于宇宙学和星系偏差参数的大部分信息都由壳层自角和交叉角功率谱中的 BAO 特征所​​承载。 同一项研究表明，联合探测分析 (ADF+ARF) 可以将与宇宙学参数（例如 $H_0$ 或暗能量 Chevallier-Polarski-Linder (CPL) 参数 $\{w_0,w_a\}$）相关的 Fisher 行列式至少提高一个数量级。 我们还研究了在不同的红移壳层配置下，关于宇宙学和星系偏置相关参数的费舍尔信息量如何变化：包括与相邻壳层的交叉关联，对于ADF（ARF）来说，需要扩展到$(\Delta z)^{\rm tot}\sim 0.6$（$(\Delta z)^{\rm tot}\sim 0.4$）以使费舍尔信息收敛。 同时，使用窄壳宽（$\sigma_z \leq 0.02$）的配置保留了与特殊速度相关的宇宙信息，并且通常产生的费舍尔行列式比宽壳（$\sigma_z>0.02$）配置的大两个数量级。 显示英文摘要

摘要： In this work we examine the baryon acoustic oscillations (BAO) in 2D angular and redshift space $\{\theta, \Delta z\}$, with $\Delta z$ denoting the redshift difference between two given angular shells. We thus work in the context of tomographic analyses of the large scale structure (LSS) where data are sliced in different redshift shells and constraints on Cosmology are extracted from the auto and cross-angular spectra of two different probes, namely the standard galaxy angular density fluctuations (ADF, or 2D clustering), and the galaxy angular redshift fluctuations (ARF). For these two observables we study by first time how the BAO peak arises in the $\{\theta, \Delta z\}$ plane. Despite being a weak feature (particularly for $\Delta z \neq 0$), a Fisher forecast analysis shows that, a priori, most of the information on cosmological and galaxy bias parameters is carried by the BAO features in shell auto- and cross-angular power spectra. The same study shows that a joint probe analysis (ADF+ARF) increases the Fisher determinant associated to cosmological parameters such as $H_0$ or the Dark Energy Chevallier-Polarski-Linder (CPL) parameters $\{w_0,w_a\}$ by at least an order of magnitude. We also study how the Fisher information on cosmological and galaxy bias-related parameters behaves under different redshift shell configurations: including cross-correlations to neighbour shells extending up to $(\Delta z)^{\rm tot}\sim 0.6$ ($(\Delta z)^{\rm tot}\sim 0.4$) for ADF (ARF) is required for Fisher information to converge. At the same time, configurations using narrow shell widths ($\sigma_z \leq 0.02$) preserve the cosmological information associated to peculiar velocities and typically yield Fisher determinants that are about two orders of magnitudes larger than for wider shell ($\sigma_z>0.02$) configurations.