2018MNRAS.480.2963O

Hydrostatic equilibrium (HSE), where the thermal pressure gradient balances the force of gravity, is tested across a range of simulated EAGLE haloes from Milky Way L* haloes (M₂₀₀~10¹²M_☉) to cluster scales. Clusters (M₂₀₀~10¹⁴M_☉) reproduce previous results with thermal pressure responsible for ∼90 per cent of the support against gravity, but this fraction drops for group-sized haloes (M₂₀₀~10¹³M_☉) and is even lower (40-70 per cent) for L* haloes between 0.1 and 0.3R₂₀₀. Energy from feedback grows relative to the binding energy of a halo towards lower mass resulting in greater deviations from HSE. Tangential motions comprise the largest deviation from HSE in L* haloes indicating that the hot circumgalactic medium (CGM) has significant subcentrifugal rotation and angular momentum spin parameters 2-3 x higher than the dark matter spin parameters. Thermal feedback can buoyantly rise to the outer CGM of M₂₀₀ <= 10¹²M_☉ haloes, both moving baryons beyond R₂₀₀ and feeding uncorrelated tangential motions. The resulting hot halo density and rotation profiles show promising agreement with X-ray observations of the inner Milky Way halo, and we discuss future observational prospects to detect spinning hot haloes around other galaxies. Acceleration and radial streaming motions also comprise significant deviations from HSE, especially net outward accelerations seen in L* and group haloes indicating active feedback. Black hole feedback acts in a preventative manner during the later growth of group haloes, applying significant accelerations via shocks that do not feed tangential motions. We argue that HSE is a poor assumption for the CGM, especially in the inner regions, and rotating baryonic hot haloes are a critical consideration for analytic models of the CGM.