METAL-Z: Measuring Dust Depletion in Low-metallicity Dwarf Galaxies

Abstract The cycling of metals between interstellar gas and dust is a critical aspect of the baryon cycle of galaxies, yet our understanding of this process is limited. This study focuses on understanding dust depletion effects in the low-metallicity regime (<20% Z ⊙ ) typical of cosmic noon. Using medium-resolution UV spectroscopy from the Cosmic Origins Spectrograph on board the Hubble Space Telescope, gas-phase abundances and depletions of iron and sulfur were derived toward 18 sight lines in local dwarf galaxies IC 1613 and Sextans A. The results show that the depletion of Fe and S is consistent with that found in the Milky Way (MW), LMC, and SMC. The depletion level of Fe increases with gas column density, indicating dust growth in the interstellar medium. The level of Fe depletion decreases with decreasing metallicity, resulting in the fraction of iron in gas ranging from 3% in the MW to 9% in IC 1613 and ∼19% in Sextans A. The dust-to-gas and dust-to-metal ratios ( D / G , D / M ) for these dwarf galaxies were estimated based on the MW relations between the depletion of Fe and other elements. The study finds that D / G decreases only slightly sublinearly with metallicity, with D / M decreasing from 0.41 ± 0.05 in the MW to 0.11 ± 0.11 at 0.10 Z ⊙ (at log N (H) = 21 cm −2 ). The trend of D / G versus metallicity using depletion in local systems is similar to that inferred in Damped Ly α systems from abundance ratios but lies higher than the trend inferred from far-IR measurements in nearby galaxies.