  We examine the properties of the low-redshift circumgalactic medium (CGM)
around star-forming and quenched galaxies in the Simba cosmological
hydrodynamic simulations, focusing on comparing HI and metal line absorption to
observations from the COS-Halos and COS-Dwarfs surveys. Halo baryon fractions
are always well below the cosmic fraction due to stellar feedback at low
masses, and jet-mode AGN feedback at high masses. Baryons and metals in the CGM
of quenched galaxies are mostly in hot gas, while the CGM of star-forming
galaxies is more multiphase. Hot CGM gas has low metallicity, while warm and
cool CGM gas have metallicity close to that of galactic gas. Equivalent widths,
covering fractions and total path absorption of HI and selected metal lines
(MgII, SiIII, CIV and OVI) around a matched sample of Simba galaxies are
broadly consistent with COS-Halos and COS-Dwarfs observations. Absorption is
higher around star forming galaxies, and drops with radius. HI absorption
around Simba star-forming galaxies is in good agreement with observations,
however around quenched galaxies HI absorption is under-predicted. Metal-line
absorption is sensitive to choice of photo-ionising background; assuming recent
backgrounds, Simba matches OVI but under-predicts low ions, while an older
background matches low ions but under-predicts OVI. Simba reproduces the
observed dichotomy of OVI absorption around star forming and quenched galaxies.
CGM metals primarily come from stellar feedback, while jet-mode AGN feedback
reduces absorption particularly for lower ions.
