Kinematic cosmic dipole from a large sample of strong lenses

TL;DR

This paper proposes a new method using strong gravitational lenses to measure the kinematic cosmic dipole, aiming to resolve existing tensions between CMB and high-redshift source count measurements, with potential for high-precision results.

Contribution

It introduces a novel approach leveraging Einstein radius measurements and spectroscopic data to accurately determine the cosmic dipole, improving upon previous methods.

Findings

Einstein radius measurements alone are insufficient for high-precision dipole estimation.

Including spectroscopic velocity dispersions significantly enhances measurement accuracy.

The method can discriminate between CMB and source count dipole values at about 5σ significance.

Abstract

Measurements of the kinematic cosmic dipole continue to show an intriguing tension between the value inferred from the CMB and that obtained from high-redshift source number counts. While the measured dipole direction appears consistent, the amplitude, set by the observer's peculiar velocity $v_{o}$, remains in significant disagreement. In this paper, we propose using strong gravitational lenses with well-measured Einstein radii to estimate the kinematic cosmic dipole, through the relativistic aberration of the Einstein angle induced by the observer's motion. We show that this effect could be detected solely from measurements of the Einstein radius in wide, high-resolution imaging surveys such as Euclid. However, the precision achievable using Einstein-radius measurements alone, without redshift or lens-galaxy mass information, appears insufficient to discriminate between the CMB value of $v_{o}$ and that derived from source number counts at high statistical significance. Nevertheless, we demonstrate that including a large sample of lenses with available kinematic information, either via the Fundamental Plane relation or, ideally, through spectroscopic velocity-dispersion measurements, drastically reduces the noise and substantially improves the constraining power of this method. We show that, for a realistic sample of strong lenses detected by Euclid and complemented with spectroscopic velocity dispersion measurements from 4MOST or DESI, it is possible to discriminate between the CMB- and source-number-counts-inferred values at the $\sim 5\sigma$ level using a new, fully independent method. We further demonstrate that this technique is only weakly sensitive to strong-lensing selection effects, with selection biases and threshold effects estimated to be well below the 1% level.