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Two distinct scenarios for the origin of the ~ 4 \times 10^8 M\odot of dustobserved in the high-redshift (z = 6.4) quasar J1148+5251 have been proposed.The first assumes that this galaxy is much younger than the age of the universeat that epoch so that only supernovae (SNe) could have produced this dust. Thesecond scenario assumes a significantly older galactic age, so that the dustcould have formed in lower-mass asymptotic giant branch (AGB) stars. Presentingnew integral solutions for the chemical evolution of metals and dust ingalaxies, we offer a critical evaluation of these two scenarios, andobservational consequences that can discriminate between the two. We show thatAGB stars can produce the inferred mass of dust in this object, however, thefinal mass of surviving dust depends on the galaxy's star formation history(SFH). In general supernovae cannot produce the observed amount of dust unlessthe average SN event creates over ~ 1 M\odot of dust in its ejecta. However,special SFHs can be constructed in which SNe can produce the inferred dust masswith a reasonable average dust yield of ~ 0.15 M\odot. The two scenariospropose different origins for the galaxy's spectral energy distribution,different star formation efficiencies and stellar masses, and consequentlydifferent comoving number densities of J1148+5251-type hyperluminous infrared(IR) objects. The detection of diagnostic mid-IR fine structure lines, and morecomplete surveys determining the comoving number density of these objects candiscriminate between the two scenarios.

The Origin of Dust in the Early Universe: Probing the Star Formation History of Galaxies by their Dust Content