Effects of feedback on galaxies in the VELA simulations: elongation, clumps, and compaction

The evolution of star-forming galaxies at high redshifts is very sensitive to the strength and nature of stellar feedback. Using two sets of cosmological, zoom-in simulations from the VELA suite, we compare the effects of two different models of feedback: with and without kinetic feedback from the expansion of supernovae shells and stellar winds. At a fixed halo mass and redshift, the stellar mass is reduced by a factor of similar to 1-3 in the models with stronger feedback, so the stellar mass-halo mass relation is in better agreement with abundance matching results. On the other hand, the three-dimensional shape of low-mass galaxies is elongated along a major axis in both models. At a fixed stellar mass, M-* < 10(10) M-circle dot, galaxies are more elongated in the strong-feedback case. More massive, star-forming discs with high surface densities form giant clumps. However, the population of round, compact, old (age(c) > 300 Myr), quenched, stellar (or gas-poor) clumps is absent in the model with strong feedback. On the other hand, giant star-forming clumps with intermediate ages (age(c) = 100-300 Myr) can survive for several disc dynamical times, independently of feedback strength. The evolution through compaction followed by quenching in the plane of central surface density and specific star formation rate is similar under the two feedback models.

Automated summary

The evolution of star-forming galaxies at high redshifts is significantly affected by the strength and nature of stellar feedback. This study compares the effects of two different feedback models using cosmological simulations. The models with stronger feedback show a reduction in stellar mass and a better agreement with abundance matching results. Additionally, low-mass galaxies in both models have an elongated shape. However, the presence of old, quenched clumps is absent in the model with strong feedback. On the other hand, giant star-forming clumps can survive for several disc dynamical times under both feedback models.