Evidence for galaxy dynamics tracing background cosmology below the de Sitter scale of acceleration

TL;DR

This paper presents evidence that galaxy dynamics at accelerations below the de Sitter scale can be used to probe background cosmology, revealing a holographic origin of inertia and a transition in galaxy behavior consistent with weak gravity modifications.

Contribution

It introduces a novel link between galaxy dynamics and background cosmology, proposing a holographic origin of inertia and analyzing galaxy rotation curves across redshifts to support this connection.

Findings

Galaxy dynamics probe weak gravity below the de Sitter scale.

Transition radius in galaxies correlates with mass and Hubble parameter.

Anomalous galaxy behavior consistent with holographic inertia origin.

Abstract

Galaxy dynamics probes weak gravity at accelerations below the de Sitter scale of acceleration $a_{dS}=cH$, where $c$ is the velocity of light and $H$ is the Hubble parameter. Low and high redshift galaxies hereby offer a novel probe of weak gravity in an evolving cosmology, satisfying $H(z)=H_0\sqrt{1+\omega_m(6z+12z^2+12z^3+6z^4+(6/5)z^5)}/(1+z)$ with baryonic matter content $\omega_m$ sans tension to $H_0$ in surveys of the Local Universe. Galaxy rotation curves show anomalous galaxy dynamics in weak gravity $a_N<a_{dS}$ across a transition radius $r_t = 4.7\,\mbox{kpc}\,M_{11}^{1/2}(H_0/H)^\frac{1}{2}$ in galaxies of mass $M=10^{11}M_\odot M_{11}$, where $a_N$ is the Newtonian acceleration based on baryonic matter content. We identify this behavior with a holographic origin of inertia from entanglement entropy, that introduces a $C^0$ onset across $a_N=a_{dS}$ with asymptotic behavior described by a Milgrom parameter satisfying $a_0=\omega_0/2\pi$, where $\omega_0=\sqrt{1-q}H$ is a fundamental eigenfrequency of the cosmological horizon. Extending an earlier confrontation with data covering $0.003\lesssim a_N/a_{dS}\lesssim1$ at redshift $z\sim0$ in Lellie et al. (2016), the modest anomalous behavior in the Genzel et al. sample at redshifts $0.854\le z\le 2.282$ is found to be mostly due to clustering $0.36\lesssim a_N/a_{dS}\lesssim1$ close to the $C^0$ onset to weak gravity and an increase of up to 65\% in $a_0$.