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We present the evolution of the star-formation dispersion - stellar massrelation ($\sigma_{SFR}$-M$_{\star}$) in the DEVILS D10 region using newmeasurements derived using the ProSpect spectral energy distribution fittingcode. We find that $\sigma_{SFR}$-M$_{\star}$ shows the characteristic'U-shape' at intermediate stellar masses from 0.1<z<0.7 for a number ofmetrics, including using the deconvolved intrinsic dispersion. A physicalinterpretation of this relation is the combination of stochastic star-formationand stellar feedback causing large scatter at low stellar masses and AGNfeedback causing asymmetric scatter at high stellar masses. As such, the shapeof this distribution and its evolution encodes detailed information about theastrophysical processes affecting star-formation, feedback and the lifecycle ofgalaxies. We find that the stellar mass that the minimum ${\sigma}_{SFR}$occurs evolves linearly with redshift, moving to higher stellar masses withincreasing lookback time and traces the turnover in the star-forming sequence.This minimum ${\sigma}_{SFR}$ point is also found to occur at a fixed specificstar-formation rate (sSFR) at all epochs (sSFR~10$^{-9.6}$yr$^{-1}$). Thephysical interpretation of this is that there exists a maximum sSFR at whichgalaxies can internally self-regulate on the tight sequence of star-formation.At higher sSFRs, stochastic stellar processes begin to cause galaxies to bepushed both above and below the star-forming sequence leading to increased SFRdispersion. As the Universe evolves, a higher fraction of galaxies will dropbelow this sSFR threshold, causing the dispersion of the low-stellar mass endof the star-forming sequence to decrease with time.

monthly notices of the royal astronomical society

Deep Extragalactic VIsible Legacy Survey (DEVILS): Evolution of the  $\sigma_{\mathrm{SFR}}$-M$_{\star}$ relation and implications for  self-regulated star formation