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Large-scale clustering of galaxies in general relativity
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Large-scale clustering of galaxies in general relativity
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Several recent studies have shown how to properly calculate the observed clustering of galaxies in a relativistic context, and uncovered corrections to the Newtonian calculation that become significant on scales near the horizon. Here, we retrace these calculations and show that, on scales approaching the horizon, the observed galaxy power spectrum depends strongly on which gauge is assumed to relate the intrinsic fluctuations in galaxy density to matter perturbations through a linear bias relation. Starting from simple physical assumptions, we derive a gauge-invariant expression relating galaxy density perturbations to matter density perturbations on large scales, and show that it reduces to a linear bias relation in synchronous-comoving gauge, corroborating an assumption made in several recent papers. We evaluate the resulting observed galaxy power spectrum, and show that it leads to corrections similar to an effective non-Gaussian bias corresponding to a local (effective) fNL < 0.5. This number can serve as a guideline as to which surveys need to take into account relativistic effects. We also discuss the scale-dependent bias induced by primordial non-Gaussianity in the relativistic context, which again is simplest in synchronous-comoving gauge.
Forward citations
Cited by 10 Pith papers
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Nonlinear Relativistic Effects on Cosmological Redshift Drift
Second-order relativistic effects on redshift drift are computed, showing distortions appear only at this order with enhanced nonlinear bispectrum contributions at low redshift and large momenta.
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Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges
Newtonian motion gauges extend the validity of Newtonian EFTofLSS to scale-dependent growth and GR effects by transforming linear equations to Newtonian form, computing nonlinear clustering there, and transforming res...
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Effective Field Theory of Large Scale Structure and Newtonian Motion Gauges
A Newtonian Motion Gauge found via Einstein-Boltzmann solver maps linear dynamics with scale-dependent growth and GR corrections to Newtonian equations, enabling consistent nonlinear EFT calculations that are transfor...
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Nonlinear Relativistic Effects on Cosmological Redshift Drift
Second-order relativistic corrections to the redshift drift are derived; the dominant sub-Hubble term is the squared radial velocity gradient, producing a bispectrum that can exceed the squared power spectrum at low z.
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Impact and measurability of linear relativistic effects in galaxy surveys
Neglecting linear GR effects biases f_NL at 1–3σ for Euclid/SPHEREx in SFB forecasts; multi-tracer improves Doppler detection and weakly breaks b_ϕ f_NL degeneracy.
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The observer power spectrum for lightcone statistics, integrated relativistic observables and wide angle effects
Introduces the observer power spectrum as a diagonal Fourier-space statistic for lightcone observables by transforming over observer positions rather than sources.
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The observer power spectrum for lightcone statistics, integrated relativistic observables and wide angle effects
Fourier transforming over observer positions yields a diagonal power spectrum for any lightcone observable, from which standard two-point and higher-order statistics follow as projections.
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Unbiased analysis of primordial non-Gaussianity: the multipoles of the full relativistic power spectrum
Integrated relativistic (lensing, ISW, time-delay) corrections to power-spectrum multipoles bias predicted f_NL constraints by ~3σ (Euclid) and ~20σ (MegaMapper); a bright-faint split partly offsets the luminosity-fun...
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Impact of lensing magnification on the power spectrum turnover
Lensing magnification biases the recovered turnover scale k0 by up to 3.6 sigma in high-z mocks, vanishing above z~3.7 for MegaMapper-like surveys and requiring modeling above z~2.9.
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Relativistic effects in k-essence
Relativistic effects dominate large-scale galaxy power spectra and grow with redshift, but are largely insensitive to k-essence microphysics in Fourier space while the angular spectrum shows clearer model distinctions...
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