Relic galaxy analogues in Illustris TNG50: the formation pathways of surviving red nuggets in a cosmological simulation

TL;DR

This study identifies and analyzes relic galaxy analogues in the TNG50 simulation, revealing their formation pathways and comparing their properties with observed relics to understand their evolution and rarity.

Contribution

First identification of relic galaxy analogues in TNG50 simulation, elucidating their formation pathways and comparing simulated properties with observations.

Findings

One TNG50 analogue closely matches observed relics in properties.

Relic analogues form via environmental stripping or early gas consumption.

Progenitors of relics inhabit more massive halos at high redshift.

Abstract

Relic galaxies are massive compact quiescent galaxies that formed at high-redshift and remained almost unchanged since then. In this work, we search for analogues to relic galaxies in the TNG50 cosmological simulations to understand relic formation and test the ability of TNG50 to reproduce such rare objects. Using stellar mass, age, radius, quiescence and stellar assembly criteria, we find 5 subhalos in TNG50 that could be potential relic analogues. We compare their properties with other constraints imposed by a sample of 13 observed relic galaxies. We find one analogue in TNG50 that simultaneously satisfies most of the available observational constraints, such as metallicity and morphology. It also shows similarities to the confirmed relic NGC 1277, regarding environment and dark matter fraction. By taking into account a degree of relicness, a second relic analogue may also be considered. However, the central parts of the brightness and density profiles of the analogues are less steep than that of real relic galaxies, possibly due to limited numerical resolution. We identify two formation pathways of relic analogues in TNG50 depending on their environment: they either have their remaining gas stripped during the infall into a cluster at $z \lesssim 1.2$ or consume it before $z > 1.5$. They are then deprived of significant star formation, leaving their stellar populations almost unaltered during the last 9 Gyr. We also find that the analogue progenitors at $z \sim 4$ inhabit more massive halos than progenitors of quiescent galaxies with similar stellar mass at $z \sim 0$.