The MUSE Hubble Ultra Deep Field Survey XI. Constraining the low-mass end of the stellar mass - star formation rate relation at $z<1$

Abstract: 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 $M_{} < 10^{10} {\rm M}{\odot}$ 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 $7 \leq \log M{}[{\rm M}{\odot}] \leq 10.5$ 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$\beta$ $\lambda 4861$ and H$\alpha$ $\lambda 6563$. We model the star formation sequence with a Gaussian distribution around a hyperplane between $\log M{}$, $\log {\rm SFR}$, 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 $\log {\rm SFR}[{\rm M}{\odot}/{\rm yr}] = 0.83^{+0.07}{-0.06} \log M_{*}[{\rm M}{\odot}] + 1.74^{+0.66}{-0.68} \log (1+z)$, increasing with redshift. We recover an intrinsic scatter in the relation of $\sigma_{\rm intr} = 0.44^{+0.05}_{-0.04}$ 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.