A Dusty Dawn: Galactic Dust Buildup at z5

Over the last decade, the Atacama Large Millimeter Array has revealed massive, dusty star-forming galaxies at z5, and the James Webb Space Telescope is primed to uncover even more information about them. These observations need dust evolution theory to provide context and are excellent benchmarks to test this theory. Here, we investigate the evolution of galactic dust budget at cosmic dawn using a suite of cosmological zoom-in simulations of moderately massive, high-redshift (M ₒₓ₀ₑ10⁹ M_; z5) galaxies from the FIRE project, the highest resolution (m ₁ 7100\, M_) of such simulations to date. Our simulations incorporate a dust evolution model that accounts for the dominant sources of dust production, growth, and destruction and follows the evolution of specific dust species, allowing it to replicate a wide range of present-day observations. We find, similar to other theoretical works, that dust growth via gas-dust accretion is the dominant producer of dust mass for these massive, z 5 galaxies. However, our fiducial model produces M ₃ₔₒₓ that fall 1 dex below observations at any given M ₒₓ₀ₑ (typical uncertainties are 1 dex), which we attribute to reduced accretion efficiencies caused by a combination of low galactic metallicities and extremely bursty star formation. Modest enhancements (i. e. , within observational/theoretical uncertainties) to accretion and SNe II dust creation raise M ₃ₔₒₓ by 1 dex, but this still falls below observations which assume T ₃ₔₒₓ25 K. One possibility is that inferred dust masses for z4 galaxies are overestimated, and recent observational/analytical works that find T ₃ₔₒₓ50 K along with metallicity constraints tentatively support this.