  We measure the broad impact of galaxy structure on galaxy formation by
examining the ongoing star formation and integrated star formation history as
revealed through the stellar masses of galaxies at $z < 7$ based on JWST CEERS
data from the Extended Groth Strip (EGS). Using the morphological catalog of
3965 visually classified JWST galaxies from Ferreira et al. (2023), we
investigate the evolution of stars, and when they form, as a function of
morphological type as well as galaxies classified as passive and starburst
through spectral energy distributions. Although disk galaxies dominate the
structures of galaxies at $z < 7$, we find that these disks are in general
either `passive', or on the main-sequence of star formation, and do not contain
a large population of starburst galaxies. We also find no significant
correlation between morphological type and the star formation rate or colours
of galaxies at $z < 7$. In fact, we find that the morphologically classified
`spheroids' tend to be blue and are not found to be predominately passive
systems at $z > 1.5$. We also find that the stellar mass function for disk
galaxies does not evolve significantly during this time, whereas other galaxy
types, such as the peculiar population, evolve dramatically, declining at lower
redshifts. This indicates that massive peculiars are more common at higher
redshifts. We further find that up to $z \sim 7$, the specific star formation
rate (sSFR) does not vary with visual morphology, but strongly depends on
stellar mass and internal galaxy mass density. This demonstrates that at early
epochs galaxy assembly is a mass-driven, rather than a morphologically-driven,
process. Quenching of star formation is therefore a mass-dominated process
throughout the universe's history, likely due to the presence of supermassive
black holes.
