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We combine cosmological, hydrodynamical simulations with accurate radiativetransfer corrections to investigate the relation between strong HI absorbers(N_HI >~ 10^17 /cm^2) and galaxies at redshift z = 3. We find a stronganti-correlation between the column density and the impact parameter thatconnects the absorber to the nearest galaxy. The median impact parameters forLyman Limit (LL) and Damped Lyman-{\alpha} (DLA) systems are ~10 and ~1 properkpc, respectively. If normalized to the size of the halo of the nearest centralgalaxy, the median impact parameters for LL and DLA systems become ~1 and~10^-1 virial radii, respectively. At a given HI column density, the impactparameter increases with the mass of the closest galaxy, in agreement withobservations. We predict most strong HI absorbers to be most closely associatedwith extremely low-mass galaxies, M_star < 10^8 M_sun and star formation rate<10^-1 M_sun/yr. We also find a correlation between the column density ofabsorbers and the mass of the nearest galaxy. This correlation is mostpronounced for DLAs with N_HI > 10^21 /cm^2 which are typically close togalaxies with M_star >~ 10^9 M_sun. Similar correlations exist between columndensity and other properties of the associated galaxies such as their starformation rates, halo masses and HI content. The galaxies nearest to HIabsorbers are typically far too faint to be detectable with currentinstrumentation, which is consistent with the high rate of (often unpublished)non-detections in observational searches for the galaxy counterparts of strongHI absorbers. Moreover, we predict that the detected nearby galaxies aretypically not the galaxies that are most closely associated with the absorbers,thus causing the impact parameters, star formation rates and stellar masses ofthe observed counterparts to be biased high.

Predictions for the relation between strong HI absorbers and galaxies at redshift 3