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The scatter (${\rm\sigma_{\text{sSFR}}}$) of the specific star formationrates (sSFRs) of galaxies is a measure of the diversity in their star formationhistories (SFHs) at a given mass. In this paper we employ the EAGLE simulationsto study the dependence of the ${\rm \sigma_{\text{sSFR}}}$ of galaxies onstellar mass (${\rm M_{\star}}$) through the ${\rm \sigma_{\text{sSFR}}}$-${\rmM_{\star}}$ relation in $ {\rm z \sim 0-4}$. We find that the relation evolveswith time, with the dispersion depending on both stellar mass and redshift. Themodels point to an evolving U-shape form for the ${\rm\sigma_{\text{sSFR}}}$-${\rm M_{\star}}$ relation with the scatter beingminimal at a characteristic mass $M^{\star}$ of ${\rm 10^{9.5}}$ ${\rmM_{\odot}}$ and increasing both at lower and higher masses. This implication isthat the diversity of SFHs increases towards both at the low- and high-massends. We find that active galactic nuclei feedback is important for increasingthe ${\rm \sigma_{\text{sSFR}}}$ for high mass objects. On the other hand, wesuggest that SNe feedback increases the ${\rm \sigma_{\text{sSFR}}}$ ofgalaxies at the low-mass end. We also find that excluding galaxies that haveexperienced recent mergers does not significantly affect the ${\rm\sigma_{\text{sSFR}}}$-${\rm M_{\star}}$ relation. Furthermore, we employ thecombination of the EAGLE simulations with the radiative transfer code SKIRT toevaluate the effect of SFR/stellar mass diagnostics in the ${\rm\sigma_{\text{sSFR}}}$-${\rm M_{\star}}$ relation and find that the ${\rmSFR/M_{\star}}$ methodologies (e.g. SED fitting, UV+IR, UV+IRX-$\beta$) widelyused in the literature to obtain intrinsic properties of galaxies have a largeeffect on the derived shape and normalization of the ${\rm\sigma_{\text{sSFR}}}$-${\rm M_{\star}}$ relation.

An evolving and mass dependent ${\rm \sigma_{\text{sSFR}}}$-${\rm M_{\star}}$ relation for galaxies