Star-forming galaxies have been found to follow a relatively tight relation between stellar mass ( M * ) and star formation rate (SFR), dubbed the “star formation sequence”. A turnover in the sequence has been observed, where galaxies with M * < 10 10 M ⊙ follow a steeper relation than their higher mass counterparts, suggesting that the low-mass slope is (nearly) linear. In this paper, we characterise the properties of the low-mass end of the star formation sequence between 7 ≤ log M * [ M ⊙ ] ≤ 10.5 at redshift 0.11 < z < 0.91. We use the deepest MUSE observations of the Hubble Ultra Deep Field and the Hubble Deep Field South to construct a sample of 179 star-forming galaxies with high signal-to-noise emission lines. Dust-corrected SFRs are determined from H β λ 4861 and H α λ 6563. We model the star formation sequence with a Gaussian distribution around a hyperplane between log M * , logSFR, and log(1 + z ), to simultaneously constrain the slope, redshift evolution, and intrinsic scatter. We find a sub-linear slope for the low-mass regime where log SFR [ M ⊙ yr −1 ] = 0.83 +0.07 −0.06 log M * [ M ⊙ ]+1.74 +0.66 −0.68 log(1 + z ), increasing with redshift. We recover an intrinsic scatter in the relation of σ intr = 0.44 +0.05 −0.04 , dex, larger than typically found at higher masses. As both hydrodynamical simulations and (semi-)analytical models typically favour a steeper slope in the low-mass regime, our results provide new constraints on the feedback processes which operate preferentially in low-mass halos.