A Comprehensive Investigation of Metals in the Circumgalactic Medium of Nearby Dwarf Galaxies

Dwarf galaxies are found to have lost most of their metals via feedback processes; however, there still lacks consistent assessment on the retention rate of metals in their circumgalactic medium (CGM). Here we investigate the metal content in the CGM of 45 isolated dwarf galaxies with M * = 106.5-9.5 M circle dot (M 200m = 1010.0-11.5 M circle dot) using the Hubble Space Telescope/Cosmic Origins Spectrograph. While H i (Ly alpha) is ubiquitously detected (89%) within the CGM, we find low detection rates (approximate to 5%-22%) in C ii, C iv, Si ii, Si iii, and Si iv, largely consistent with literature values. Assuming these ions form in the cool (T approximate to 104 K) CGM with photoionization equilibrium, the observed H i and metal column density profiles can be best explained by an empirical model with low gas density and high volume filling factor. For a typical galaxy with M 200m = 1010.9 M circle dot (median of the sample), our model predicts a cool gas mass of M CGM,cool similar to 108.4 M circle dot, corresponding to similar to 2% of the galaxy's baryonic budget. Assuming a metallicity of 0.3 Z circle dot, we estimate that the dwarf galaxy's cool CGM likely harbors similar to 10% of the metals ever produced, with the rest either in more ionized states in the CGM or transported to the intergalactic medium. We further examine the EAGLE simulation and show that H i and low ions may arise from a dense cool medium, while C iv arises from a diffuse warmer medium. Our work provides the community with a uniform data set on dwarf galaxies' CGM that combines our recent observations, additional archival data and literature compilation, which can be used to test various theoretical models of dwarf galaxies.