  Recent observations have revealed remarkable insights into the gas reservoir
in the circumgalactic medium (CGM) of galaxy haloes. In this paper, we
characterise the gas in the vicinity of Milky Way and Andromeda analogues in
the HESTIA (High resolution Environmental Simulations of The Immediate Area)
suite of constrained Local Group (LG) simulations. The HESTIA suite comprise of
a set of three high-resolution {\sc arepo}-based simulations of the LG, run
using the Auriga galaxy formation model. For this paper, we focus only on the
$z = 0$ simulation datasets and generate mock skymaps along with a power
spectrum analysis to show that the distributions of ions tracing
low-temperature gas (HI and SiIII) are more clumpy in comparison to warmer gas
tracers (OVI, OVII and OVIII). We compare to the spectroscopic CGM observations
of M31 and low-redshift galaxies. HESTIA under-produces the column densities of
the M31 observations, but the simulations are consistent with the observations
of low-redshift galaxies. A possible explanation for these findings is that the
spectroscopic observations of M31 are contaminated by gas residing in the CGM
of the Milky Way.
