Interstellar dust acts as a shield, protecting cosmic objects from harsh radiation. Dust shielding allows molecular clouds to cool, which leads to the formation of new stars and planets. Its role in star formation makes interstellar dust an essential driver of galaxy evolution.
To form, dust requires metals (carbon, silicon, iron, magnesium, aluminum, etc.), and these metals were scarce in the early Universe. It's not clear whether early, metal-poor stars are able to produce much dust. Nonetheless, there is evidence for dust in high redshift quasars when the Universe was less than 1 billion years old (e.g., see here, here, and here). How did this dust get there?
Most stars from about 1-10x the mass of our Sun go through the AGB phase after they use up all their core hydrogen. The AGB phase is brief compared to the lifetime of the star, but the consequences are dramatic. AGB stars are bloated red giant stars, and since they are so large, their outer atmospheres are cool. The low temperatures allow for dust condensation and radiation pressure pushes the dust outwards, creating a dense stellar wind. Because almost every star goes through this phase, AGB stars may be a dominant source of interstellar dust.
AGB stars are unique in that they are able to form dust from new metals they formed themselves around their cores. This might make them efficient dust producers even in the early Universe. The DUSTiNGS survey aims to detect dust around metal-poor AGB stars to test whether metal-poor stars are able to produce dust early on.