The HYENAS project: a prediction for the X-ray undetected galaxy groups

TL;DR

This study uses zoom-in simulations from the HYENAS project to explore why many galaxy groups are X-ray undetected, revealing that halo formation time influences hot gas fractions and X-ray brightness.

Contribution

It demonstrates the role of halo formation time in hot gas content variability, providing insights into X-ray undetected galaxy groups using novel simulations.

Findings

Early-formed halos have significantly brighter X-ray luminosities.

X-ray undetected groups are likely late-formed halos.

Gas fraction variability is linked to halo formation history.

Abstract

Galaxy groups contain the majority of bound mass with a significant portion of baryons due to the combination of halo mass and abundance (Cui 2024). Hence they serve as a crucial missing piece in the puzzle of galaxy formation and the evolution of large-scale structures in the Universe. In observations, mass-complete group catalogues are normally derived from galaxy redshift surveys detected through various three-dimensional group-finding algorithms. Confirming the reality of such groups, particularly in the X-rays, is critical for ensuring robust studies of galaxy evolution in these environments. Recent works have reported numerous optical groups that are X-ray undetected (see, e.g., Popesso et al. 2024), sparking debates regarding the reasons for the unexpectedly low hot gas fraction in galaxy groups. To address this issue, we utilise zoomed-in simulations of galaxy groups from the novel HYENAS project to explore the range of hot gas fractions within galaxy groups and investigate the intrinsic factors behind the observed variability in X-ray emission. We find that the halo formation time can play a critical role -- we see that groups in halos that formed earlier exhibit up to an order of magnitude brighter X-ray luminosities compared to those formed later. This suggests that undetected X-ray groups are preferentially late-formed halos and highlights the connection between gas fraction and halo formation time in galaxy groups. Accounting for these biases in galaxy group identification is essential for advancing our understanding of galaxy formation and achieving precision in cosmological studies.