The physical nature of circumgalactic medium absorbers in <scp>Simba</scp>

We study the nature of low-redshift CGM in Simba cosmological simulations as traced by ultraviolet absorption lines around galaxies bins stellar mass ($M_\star>10^{10}M_\odot$) for star-forming, green valley and quenched at impact parameters $r_\perp\leq 1.25r_{200}$. generate synthetic spectra HI, MgII, CII, SiIII, CIV, OVI, fit Voigt profiles to obtain line properties, estimate density, temperature, metallicity absorbing gas. find that absorbers are most abundant star forming with $M_\star < 10^{11}M_\odot$, while abundance show similar behaviour those galaxies, suggesting "quenches" before formation ceases. HI gas exists across a broad range cosmic phases (condensed gas, diffuse hot halo Warm-Hot Intergalactic Medium), essentially all low-ionisation metal arises from condensed OVI split between WHIM. The fraction collisionally ionised is $\sim 25-55\%$ CIV 80-95\%$ depending on parameter. In general, highest column density features each ion arise dense Satellite defined within $10r_{1/2,\star},$ contributes 3\%$ overall but 30\%$ MgII absorption, satellites decreasing increasing excitation energy.