Relativistic and wide-angle corrections to galaxy power spectra

Abstract

Galaxy surveys contain information on the largest scales via wide-angle and relativistic contributions. By combining two different galaxy populations, we can suppress the strong cosmic variance on ultra-large scales and thus enhance the detectability of the signals. The relativistic Doppler and Sachs-Wolfe effects are of a similar magnitude to the leading wide-angle corrections, so that it is important to treat them together, especially since they can partially cancel. The power spectra depend on the choice of line of sight for each galaxy pair and we present results for a general line of sight. Then we estimate the detection significance of the auto- and cross-power spectra for a variety of cases. We use two futuristic galaxy samples based on a `beyond-DESI' survey and a SKA Phase 2 survey, covering 15,000\,deg${}^2$ up to $z=1$. We find a detection significance for the total relativistic wide-angle effects that ranges from $\sim 5\sigma$ to $>15\sigma$, depending on the line-of-sight configuration.

arXiv comment23 pages, 9 figures, 'version accepted by JCAP'

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Cited by in corpus (6)

• Primordial non-Gaussianity -- the effects of relativistic and wide-angle corrections to the power spectrum
• Using relativistic effects in large-scale structure to constrain astrophysical properties of galaxy populations
• Constraining primordial non-Gaussianity by combining photometric galaxy and 21cm intensity mapping surveys
• Detecting Relativistic Doppler in Galaxy Clustering with Tailored Galaxy Samples
• Detecting Relativistic Doppler by Multi-Tracing a Single Galaxy Population
• Multipoles of the galaxy bispectrum on a light cone: wide-separation and relativistic corrections