The Evolution of Dust in the Early Universe with Applications to the Galaxy SDSS J1148+5251

TL;DR

This paper models the evolution of dust, gas, and metals in early universe galaxies, focusing on SDSS J1148+5251, and finds supernovae must produce more dust than observed to explain the galaxy's dust content.

Contribution

It introduces analytical models for dust evolution in high-redshift galaxies and applies them to a specific quasar, highlighting the need for additional dust formation processes.

Findings

Supernovae must condense at least 1 solar mass of dust.

Observed dust exceeds typical supernova yields, implying other processes are involved.

Star formation history can be either intense and short or prolonged with lower rates.

Abstract

Dusty hyperluminous galaxies in the early universe provide unique environments for studying the role of massive stars in the formation and destruction of dust. At redshifts above ~ 6, when the universe was less than ~ 1 Gyr old, dust could have only condensed in the explosive ejecta of Type II supernovae (SNe), since most of the progenitors of the AGB stars, the major alternative source of interstellar dust, did not have time to evolve off the main sequence since the onset of star formation. In this paper we present analytical models for the evolution of the gas, dust, and metals in high redshift galaxies, with a special application to SDSS J1148+5251, a hyperluminous quasar at z = 6.4. We find that an average supernova must condense at least 1 Msun of dust to account for the observed dust mass in this quasar. Observationally, it is in excess of the largest dust yield of ~0.02 Msun found thus far in the ejecta of any SN. If future observations find this to be a typical supernova dust yield, then additional processes, such as accretion onto preexisting grains, or condensation around the AGN will need to be invoked to account for the large amount of dust in this and similar objects. The galaxy's star formation history is still uncertain, and current observations of the gas, metal, and dust contents of J1148 can be reproduced by either an intensive and short burst of star formation (~ 1000 Msun/yr) with a duration of ~ 100 Myr, or a much lower star formation rate (~ 100 Msun/yr) occurring over the lifetime of the galaxy.