模拟相对论对晕功率谱偶极子的贡献
Modeling relativistic contributions to the halo power spectrum dipole
摘要：
我们通过射线追踪研究了包含相对论效应的N体模拟的功率谱偶极，并覆盖了低红移宇宙直到$z_{\rm max} = 0.465$（RayGalGroup模拟）。我们模型相对论修正以及广角，演化，窗口和光锥效应。我们的模型包括所有的相对论修正，包括三阶偏置膨胀。我们考虑线性依赖于$\mathcal{H}/k$（弱场近似）的所有项。我们还研究了引力红移和横向多普勒效应对物质功率谱的影响。我们发现广角和窗函数效应对偶极子信号有显著的贡献。当考虑到所有贡献时，我们的偶极模型可以准确地捕获引力红移和多普勒项，直到我们的比较（$k=0.48\,h{\rm Mpc}^{-1}$）中包含的最小尺度，而我们的横向多普勒项模型则不太准确。我们发现多普勒项是这个低红移样本的主导信号。我们使用Fisher矩阵预测来研究未来暗能量光谱仪（DESI）检测相对论对功率谱偶极的贡献的潜力。保守估计表明，BGS样本应至少能够检测到$4.4σ$，而更乐观的估计发现检测到高达$10σ$。在星系分布中检测到这些影响可以在最大尺度上进行新的引力测试，为星系调查实验提供了一个有趣的额外科学案例。
英文摘要：
We study the power spectrum dipole of an N-body simulation which includes relativistic effects through ray-tracing and covers the low redshift Universe up to $z_{\rm max} = 0.465$ (RayGalGroup simulation). We model relativistic corrections as well as wide-angle, evolution, window and lightcone effects. Our model includes all relativistic corrections up to third-order including third-order bias expansion. We consider all terms which depend linearly on $\mathcal{H}/k$ (weak field approximation). We also study the impact of 1-loop corrections to the matter power spectrum for the gravitational redshift and transverse Doppler effect. We found wide-angle and window function effects to significantly contribute to the dipole signal. When accounting for all contributions, our dipole model can accurately capture the gravitational redshift and Doppler terms up to the smallest scales included in our comparison ($k=0.48\,h{\rm Mpc}^{-1}$), while our model for the transverse Doppler term is less accurate. We find the Doppler term to be the dominant signal for this low redshift sample. We use Fisher matrix forecasts to study the potential for the future Dark Energy Spectroscopic Instrument (DESI) to detect relativistic contributions to the power spectrum dipole. A conservative estimate suggests that the DESI-BGS sample should be able to have a detection of at least $4.4σ$, while more optimistic estimates find detections of up to $10σ$. Detecting these effects in the galaxy distribution allows new tests of gravity on the largest scales, providing an interesting additional science case for galaxy survey experiments.
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