Single-phase photoionization equilibrium ( PIE ) models are often used to infer the underlying physical properties of galaxy halos probed in absorption with ions at different ionization potentials .
To incorporate the effects of turbulence , we use the MAIHEM code to model an isotropic turbulent medium exposed to a redshift zero metagalactic UV background , while tracking the ionizations , recombinations , and species-by-species radiative cooling for a wide range of ions .
By comparing observations and simulations over a wide range of turbulent velocities , densities , and metallicity with a Markov chain Monte Carlo technique , we find that MAIHEM models provide an equally good fit to the observed low-ionization species compared to PIE models , while reproducing at the same time high-ionization species such as \ion Si4 and \ion O6 .
By including multiple phases , MAIHEM models favor a higher metallicity ( Z / Z _ { \odot } \approx 40 \% ) for the circumgalactic medium compared to PIE models .
Furthermore , all of the solutions require some amount of turbulence ( \sigma _ { 3 D } \geqslant 26 { km } { s } ^ { -1 } ) .
Correlations between turbulence , metallicity , column density , and impact parameter are discussed alongside mechanisms that drive turbulence within the halo .