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The dispersion of the star-formation main sequence (SFMS) reflects thediversity of star formation histories and variation in star formation rates(SFRs) in star-forming galaxies (SFGs) with similar stellar masses ($M^\ast$).We examine the dispersion of local SFMS using a complete sample of SloanDigital Sky Survey galaxies at 0.01$<z<$0.03 with $\log(M^\ast/M_\odot)>$8.8.The SFRs are estimated from H$\alpha$ in combination with 22$\mu m$ observationfrom WISE. The catalog of bulge+disk decomposition from Simard et al. (2011) isavailable for the sample galaxies. We measure the dispersion of specific SFR(SSFR) as a function of $M^*$. We confirm that the dispersion increases with$M^*$ from 0.37$\pm0.01$dex at $\log(M^\ast/M_\odot)<$9.6 to 0.51$\pm0.02$dexat $\log(M^\ast/M_\odot)>$10.2. Despite star formation is mostly associatedwith disks, the dispersion of disk SSFR still increases with $M^*$. We concludethat the presence of bulges/bars is likely responsible for the large dispersionof SSFR in massive SFGs while low-mass SFGs are mostly disk-dominated and thuswith small dispersion. Our results suggest that star formation on galacticscales is dramatically affected by central dense structures through bothenhancing and/or quenching processes; while lower-mass SFGs tend to have lessbursty star formation histories. However, the dispersion of SSFR becomessignificantly smaller and remains constant when only disk-dominated SFGs arecounted. This finding implies that the impact of stochastic stellar feedback onstar formation is likely to follow the same pattern in all disk galaxies,showing no correlation with halo potential.

The Star-Formation Main Sequence: The Dependence of Specific Star Formation Rate and Its Dispersion on Galaxy Stellar Mass