Void Replenishment: How Voids Accrete Matter Over Cosmic History

Abstract

Cosmic voids are underdense regions filling up most of the volume in the universe. They are expected to emerge in regions comprising negative initial density fluctuations, and subsequently expand as the matter around them collapses and forms walls, filaments, and clusters. We report results from the analysis of a cosmological simulation specially designed to accurately describe low-density regions, such as cosmic voids. Contrary to the common expectation, we find that voids also experience significant mass inflows over cosmic history. On average, 10% of the mass of voids in the sample at z ∼ 0 is accreted from overdense regions, reaching values beyond 35% for a significant fraction of voids. More than half of the mass entering the voids lingers on periods of time ∼10 Gyr well inside them, reaching inner radii. This would imply that part of the gas lying inside voids at a given time proceeds from overdense regions (e.g., clusters or filaments), where it could have been preprocessed, thus challenging the scenario of galaxy formation in voids, and dissenting from the idea of them being pristine environments.

Properties of Voids and Void Galaxies in the TNG300 Simulation

“…Voids are not completely devoid of internal structure, and even the most mature voids in the local Universe show substructure in the form of galaxies and diffuse filaments (Szomoru et al 1996;El-Ad & Piran 1997;Sheth & van de Weygaert 2004;Kreckel et al 2012;Alpaslan et al 2014). The dynamical structure within voids can have significant impact on cosmic flow patterns in the local Universe, with matter around the ridges of voids affecting the peculiar motions of galaxies around nearby walls and filaments (see, e.g., Bothun et al 1992;van de Weygaert 2016;Vallés-Pérez et al 2021;Bermejo et al 2022).…”