The heartbeat of stellar halos: Insights from the stellar halo mass-metallicity relation

TL;DR

This study explores the evolution of the stellar halo mass-metallicity relation from redshift 3.5 to 0 using simulations, introducing a novel method to date halo assembly and merger history.

Contribution

It introduces halo cardiograms and the concept of stability time to analyze stellar halo assembly and its relation to the mass-metallicity relation evolution.

Findings

Stellar halos at z=3.5 already define an MZhR similar to z=0.

Metallicity increases by ~0.21 dex from z=3.5 to 0 for fixed halo mass.

A correlation exists between stability time and merger time, aiding in halo assembly dating.

Abstract

This work investigates the presence and evolution of the MZhR from redshift z=3.5 to z=0, and identifies when galaxies settle on the present-day MZhR. We used central galaxies with log10(Mgal/Msun)=[9,11] from CIELO simulations. We identified stellar halos, from z=3.5 to z=0, using the AM-E method, focusing on the region between the 1.5 optical radius and the virial radius. We presented halo cardiograms, a novel approach to studying the assembly history of stellar halos. Using them, we defined a stability time (tst) as the first time that the median halo metallicity does not change more than \pm 0.1 dex with respect to its value at z=0. CIELO stellar halos reproduce the present-day observed MZhR. At z=3.5, stellar halos already define an MZhR whose slope is similar to the slope at z=0. For a fixed stellar halo mass, the metallicity increases ~0.21 dex from z=3.5 to z=0, reflecting the progressive chemical enrichment provided by the accretion of satellites with diverse masses and different levels of enrichment. When the first stellar halo main contributor (SHMC1) provides a mass fraction at least 20% higher than the remaining contributors, the stellar halo metallicity is set once SHMC1 is fully disrupted (tmerger). This yields a clear correlation between tst and tmerger, with a scatter of 2.2 Gyr driven by the relative importance of the second and third main contributing satellites. We provide two observational tracers for tst: t90 and a stability time from the age-metallicity relation. Our results suggest that estimating tst could serve as a proxy for dating the moment at which the stellar halo reaches the present-day MZhR, as well as for dating the last major merger that builds them. Combined with an estimation of the merger time of the main contributing satellite, it can provide insights into the relative importance of the second and third contributing satellites. (abridged)