  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.
