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We explore the circumgalactic metal content traced by commonly observed lowion absorbers, including C II, Si II, Si III, Si IV, and Mg II. We use a set ofcosmological hydrodynamical zoom simulations run with the EAGLE model andincluding a non-equilibrium ionization and cooling module that follows 136ions. The simulations of z~0.2 L* (M_200=10^11.7-10^12.3 Msol) haloes hostingstar-forming galaxies and group-sized (M_200=10^12.7-10^13.3 Msol) haloeshosting mainly passive galaxies reproduce key trends observed by the COS-Halossurvey-- low ion column densities show 1) little dependence on galaxy specificstar formation rate, 2) a patchy covering fraction indicative of 10^4 K cloudswith a small volume filling factor, and 3) a declining covering fraction asimpact parameter increases from 20-160 kpc. Simulated Si II, Si III, Si IV, CII, and C III column densities show good agreement with observations, while MgII is under-predicted. Low ions trace a significant metal reservoir, ~10^8Msol, residing primarily at 10-100 kpc from star-forming and passive centralgalaxies. These clouds tend to flow inwards and most will accrete onto thecentral galaxy within the next several Gyr, while a small fraction areentrained in strong outflows. A two-phase structure describes the inner CGM(<0.5 R_200) with low-ion metal clouds surrounded by a hot, ambient medium.This cool phase is separate from the O VI observed by COS-Halos, which arisesfrom the outer CGM (>0.5 R_200) tracing virial temperature gas around L*galaxies. Physical parameters derived from standard photo-ionization modellingof observed column densities (e.g. aligned Si II/Si III absorbers) arevalidated against our simulations. Our simulations therefore support previousionization models indicating that cloud covering factors decline whiledensities and pressures show little variation with increasing impact parameter.

The multiphase circumgalactic medium traced by low metal ions in EAGLE zoom simulations