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We investigate how the X-ray circumgalactic medium (CGM) of present-daygalaxies depends on galaxy morphology and azimuthal angle using mockobservations generated from the EAGLE cosmological hydrodynamic simulation. Bycreating mock stacks of {\it eROSITA}-observed galaxies oriented to be edge-on,we make several observationally-testable predictions for galaxies in thestellar mass range $M_\star=10^{10.7-11.2}\;$M$_{\odot}$. The soft X-ray CGM ofdisc galaxies is between 60 and 100\% brighter along the semi-major axiscompared to the semi-minor axis, between 10-30 kpc. This azimuthal dependenceis a consequence of the hot ($T>10^6$ K) CGM being non-spherical: specificallyit is flattened along the minor axis such that denser and more luminous gasresides in the disc plane and co-rotates with the galaxy. Outflows enrich andheat the CGM preferentially perpendicular to the disc, but we do not find anobservationally-detectable signature along the semi-minor axis. Spheroidalgalaxies have hotter CGMs than disc galaxies related to spheroids residing athigher halos masses, which may be measurable through hardness ratios spanningthe $0.2-1.5$ keV band. While spheroids appear to have brighter CGMs than discsfor the selected fixed $M_\star$ bin, this owes to spheroids having higherstellar and halo masses within that $M_\star$ bin, and obscures the fact thatboth simulated populations have similar total CGM luminosities at the exactsame $M_\star$. Discs have brighter emission inside 20 kpc and more steeplydeclining profiles with radius than spheroids. We predict that the {\iteROSITA} 4-year all-sky survey should detect many of the signatures we predicthere, although targeted follow-up observations of highly inclined nearby discsafter the survey may be necessary to observe some of our azimuthally-dependentpredictions.

Predictions for the X-ray circumgalactic medium of edge-on discs and spheroids