Using relativistic effects in large-scale structure to constrain astrophysical properties of galaxy populations

TL;DR

This paper proposes using relativistic effects in galaxy clustering, specifically dipole and octupole signals, to better constrain astrophysical properties like evolution and magnification biases of galaxy populations in large-scale surveys.

Contribution

It introduces a novel method of splitting galaxy samples to utilize relativistic multipoles for improved bias measurements, applicable to future large-scale structure surveys.

Findings

Splitting galaxy samples enhances bias constraints.

Relativistic multipoles break parameter degeneracies.

Method applicable to various tracers and surveys.

Abstract

Upcoming large-scale structure surveys will be able to measure new features in the galaxy two point correlation function. Relativistic effects appear on large scales as subtle corrections to redshift-space distortions, showing up as a dipole and octupole when cross-correlating two different tracers of dark matter. The dipole and octupole are very sensitive to the evolution and magnification biases of the observed tracers which are hard to model accurately as they depend upon the derivative of the luminosity function at the flux limit of the survey. We show that splitting a galaxy population into bright and faint samples allows us to cross-correlate these and constrain both the evolution bias and magnification bias of the two samples -- using the relativistic odd multipoles of the correlation function, together with the even Newtonian multipoles. Although the octupole has much lower signal-to-noise than the dipole, it significantly improves the constraints by breaking parameter degeneracies. We illustrate this in the case of a futuristic survey with the Square Kilometre Array, and demonstrate how splitting the samples in different ways can help improve constraints. This method is quite general and can be used on different types of tracers to improve knowledge of their luminosity functions. Furthermore, the signal-to-noise of the dipole and octupole peaks on intermediate scales, which means that that they can deliver a clean measurement of the magnification bias and evolution bias without contamination from local primordial non-Gaussianities or from systematics on very large scales.