Disc-halo decomposition on rotationally supported star-forming galaxies (SFGs) at $z>1$ are often limited to massive galaxies ($M_star>10^{10}~M_odot$) and rely on either deep Integral Field Spectroscopy data or stacking analyses. We present a study
of the dark matter (DM) content of 9 $zapprox1$ SFGs selected Using the brightest [OII] emitters in the deepest Multi-Unit Spectrograph Explorer (MUSE) field to date, namely the 140hr MUSE Extremely Deep Field, we perform disk-halo decompositions on 9 low-mass SFGs (with $10^{8.5}<M_star<10^{10.5}~M_odot$) using a novel 3D modeling approach, which together with the exquisite S/N allows us to measure individual rotation curves to $3times R_e$. The DM component primarily uses the generalized $alpha,beta,gamma$ profile from Di Cintio et al., or a Navarro-Frenk-White (NFW) profile. The disk stellar masses $M_star$ obtained from the [OII] disk-halo decomposition agree with the values inferred from the spectral energy distributions. While the rotation curves show diverse shapes, ranging from rising to declining at large radii, the DM fractions within the half-light radius $f_{rm DM}(<R_e)$ are found to be 60% to 95%, extending to lower masses (densities) the results of Genzel et al., who found low DM fractions in SFGs with $M_star>10^{10}~M_odot$. The DM halos show constant surface densities of $sim100~M_odot$ pc$^{-2}$. Half of the sample shows a strong preference for cored over cuspy DM profiles. The presence of DM cores appears to be related to galaxies with stellar-to-halo mass $log M_star/M_{rm vir}approx-2.5$. In addition, the cuspiness of the DM profiles is found to be a strong function of the recent star-formation activity. Both of these results are interpreted as evidence for feedback-induced core formation in the Cold Dark Matter context.
