Global trends in morphology from massive to dwarf galaxies

The morphological properties of dwarf galaxies (⁠Mstar < 10^9.5 MSun⁠) remain largely unexplored, particularly outside the local neighbourhood. We explore how morphology changes across the massive to dwarf-galaxy regimes, using a mass-complete sample of 1000 galaxies, with stellar masses and redshifts in the ranges 10^9.5 MSun < Mstar < 10^12 MSun and z < 0.15, respectively. By combining James Webb Space Telescope-derived morphological parameters (concentration, asymmetry, and clumpiness; ‘CAS’) and visual morphological classifications, we explore: (1) how morphology changes with stellar mass and effective surface brightness, (2) the connection between morphology and recent star formation history, as a function of stellar mass, (3) how bar frequency changes between the massive and dwarf regimes, and (4) how well the CAS parameters perform in separating early- and late-type galaxies, as a function of stellar mass. We demonstrate that galaxies become less concentrated, more asymmetric, and less clumpy with decreasing stellar mass. In both mass regimes, galaxies that are more concentrated and less asymmetric are more likely to be red (i.e. quenched). The decrease in concentration towards lower stellar masses results in a loss of the leverage that this parameter can provide in separating early- and late-type galaxies. Thus, while the CAS system successfully separates early- and late-type systems in the massive-galaxy regime, these morphological classes become significantly more difficult to separate, using these parameters, in the dwarf regime. Finally, the bar fraction declines steadily with decreasing stellar mass and becomes consistent with zero at Mstar ~ 10^8 MSun⁠, suggesting a lower limit for the galaxy mass needed to induce bar formation.