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X-ray observations of circumgalactic coronae provide a valuable means bywhich to test galaxy formation theories. Two primary mechanisms are thought tobe responsible for the establishment of such coronae: accretion ofintergalactic gas (IGM) and/or galactic feedback. In this paper, we firstcompare our Chandra sample of galactic coronae of 53 nearby highly-inclineddisc galaxies to an analytical model considering only the accretion of IGM. Weconfirm the existing conclusion that this pure accretion model substantiallyover-predicts the coronal emission. We then select 30 field galaxies from ouroriginal sample, and correct their coronal luminosities to uniformly comparethem to deep X-ray measurements of several massive disc galaxies from theliterature, as well as to a comparable sample of simulated galaxies drawn fromthe Galaxies-Intergalactic Medium Interaction Calculation (GIMIC). Thesesimulations explicitly model both accretion and SNe feedback and yield galaxiesexhibit X-ray properties in broad agreement with our observational sample.However, notable and potentially instructive discrepancies exist between theslope and scatter of the Lx-M200 and Lx-SFR relations, highlighting some knownshortcomings of GIMIC, e.g., the absence of AGN feedback, and possibly theadoption of constant stellar feedback parameters. The simulated galaxiesexhibit a tight Lx-M200 correlation with little scatter. Having inferred M200for our observational sample via the Tully-Fisher relation, we find a weakerand more scattered correlation. In the simulated and observed samples alike,massive non-starburst galaxies above a typical transition mass of M*~2e11Msunor M200~1e13Msun tend to have higher Lx/M* and Lx/M200 than low-masscounterparts, indicating that the accretion of IGM plays an increasinglyimportant role in establishing the observable hot circumgalactic medium withincreasing galaxy mass.

Chandra Survey of Nearby Highly Inclined Disc Galaxies - III: Comparison with Hydrodynamical Simulations of Circumgalactic Coronae