未来宽视场巡天的三维星系团：球形傅里叶-贝塞尔分析的优点
3D galaxy clustering with future wide-field surveys: Advantages of a spherical Fourier-Bessel analysis
摘要：
即将进行的光谱星系巡天非常有希望帮助解决宇宙学的主要挑战，特别是在理解暗宇宙的性质方面。这些调查的力量来自其前所未有的深度和广度。最佳地提取它们的三维信息对于最好地约束暗宇宙的属性至关重要。虽然有理论的动机和新的工具来探索这些调查使用的三维球面傅里叶-贝塞尔（SFB）的星系数计数$C_\ell(k,k^\prime)$的功率谱，大多数调查的优化和预测是基于层析球面谐波功率谱$C^{(ij)}_\ell$。我们进行了一个新的调查的信息，可以从断层扫描和3D SFB技术通过比较预测宇宙学参数的约束条件，从Fisher分析的背景下，计划第四阶段的宽视场星系调查。在两个分析中，通过对非线性尺度进行仔细和连贯的处理，可以进行比较。与尺度和红移相关的星系偏置相关的营养参数也首次包括在3D SFB和层析功率谱的计算中。层析成像和3D SFB方法可以恢复类似的限制，在系统的情况下。然而，从3D SFB分析的约束是不太敏感的红移和尺度依赖的星系偏差所产生的不可避免的系统。即使是针对断层扫描优化的勘测，3D SFB分析也更强大。此外，对于调查优化，3D SFB方法的品质因数随着红移的增加而增加得更快，特别是在更高的红移下，这表明3D SFB方法应该优先用于设计和分析未来的宽场光谱调查。
英文摘要：
Upcoming spectroscopic galaxy surveys are extremely promising to help in addressing the major challenges of cosmology, in particular in understanding the nature of the dark universe. The strength of these surveys comes from their unprecedented depth and width. Optimal extraction of their three-dimensional information is of utmost importance to best constrain the properties of the dark universe. Although there is theoretical motivation and novel tools to explore these surveys using the 3D spherical Fourier-Bessel (SFB) power spectrum of galaxy number counts $C_\ell(k,k^\prime)$, most survey optimisations and forecasts are based on the tomographic spherical harmonics power spectrum $C^{(ij)}_\ell$. We performed a new investigation of the information that can be extracted from the tomographic and 3D SFB techniques by comparing the forecast cosmological parameter constraints obtained from a Fisher analysis in the context of planned stage IV wide-field galaxy surveys. The comparison was made possible by careful and coherent treatment of non-linear scales in the two analyses. Nuisance parameters related to a scale- and redshift-dependent galaxy bias were also included for the first time in the computation of both the 3D SFB and tomographic power spectra. Tomographic and 3D SFB methods can recover similar constraints in the absence of systematics. However, constraints from the 3D SFB analysis are less sensitive to unavoidable systematics stemming from a redshift- and scale-dependent galaxy bias. Even for surveys that are optimised with tomography in mind, a 3D SFB analysis is more powerful. In addition, for survey optimisation, the figure of merit for the 3D SFB method increases more rapidly with redshift, especially at higher redshifts, suggesting that the 3D SFB method should be preferred for designing and analysing future wide-field spectroscopic surveys.
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