The slope and scatter of the star-forming main sequence at z ~ 5: Reconciling observations with simulations

Galaxies exhibit a tight correlation between their star formation rate (SFR) and stellar mass over a wide redshift range known as the star-forming main sequence (SFMS). With JWST, the SFMS can now be investigated at high redshifts down to masses of sim10⁶ M_⊙, using sensitive star formation rate tracers such as the Hα emission, which allow us to probe the variability in the star formation histories. We present inferences of the SFMS based on 316 Hα-selected galaxies at z _ with log (̊m M_⋆/M_⊙) = 6. 4 -10. 6. These galaxies were identified behind the Abell 2744 lensing cluster with NIRCam grism spectroscopy from the survey All the Little Things (ALT). At face value, our data suggest a shallow slope in the SFMS (SFR ∝ M_⋆ ^α, with α=0. 45). After we corrected this for the Hα-flux limited nature of our survey using a Bayesian framework, the slope steepened to α = 0. 59 +0. 10 -0. 09, whereas current data on their own are inconclusive on the mass dependence of the scatter. These slopes differ significantly from the slope of sim1 that is expected from the observed evolution of the galaxy stellar mass function and from simulations. When we fixed the slope to α=1, we found evidence for a decreasing intrinsic scatter with stellar mass (from ∼ 0. 5 dex at M_⋆=10⁸ M_⊙ to 0. 4 dex at M_⋆= 10^ 10 M_⊙). This difference might be explained by a (combination of) luminosity-dependent SFR (Hα) calibration, a population of (mini) -quenched low-mass galaxies, or underestimated dust attenuation in high-mass galaxies. Future deep observations with different facilities can quantify these processes, which will enable us to achieve better insights into the variability of the star formation histories.