First gas-phase metallicity gradients of $0.1 \lesssim z \lesssim 0.8$
  galaxies with MUSE
  Galaxies at low-redshift typically possess negative gas-phase metallicity
gradients (centres more metal-rich than their outskirts). Whereas, it is not
uncommon to observe positive metallicity gradients in higher-redshift galaxies
($z \gtrsim 0.6$). Bridging these epochs, we present gas-phase metallicity
gradients of 84 star-forming galaxies between $0.08 < z < 0.84$. Using the
galaxies with reliably determined metallicity gradients, we measure the median
metallicity gradient to be negative ($-0.039^{+0.007}_{-0.009}$ dex/kpc).
Underlying this, however, is significant scatter: $(8\pm3)\%\ [7]$ of galaxies
have significantly positive metallicity gradients, $(38 \pm 5)\%\ [32]$ have
significantly negative gradients, $(31\pm5)\%\ [26]$ have gradients consistent
with being flat. (The remaining $(23\pm5)\%\ [19]$ have unreliable gradient
estimates.) We notice a slight trend for a more negative metallicity gradient
with both increasing stellar mass and increasing star formation rate (SFR).
However, given the potential redshift and size selection effects, we do not
consider these trends to be significant. Indeed, once we normalize the SFR
relative to that of the main sequence, we do not observe any trend between the
metallicity gradient and the normalized SFR. This is contrary to recent studies
of galaxies at similar and higher redshifts. We do, however, identify a novel
trend between the metallicity gradient of a galaxy and its size. Small galaxies
($r_d < 3$ kpc) present a large spread in observed metallicity gradients (both
negative and positive gradients). In contrast, we find no large galaxies ($r_d
> 3$ kpc) with positive metallicity gradients, and overall there is less
scatter in the metallicity gradient amongst the large galaxies. These large
(well-evolved) galaxies may be analogues of present-day galaxies, which also
show a common negative metallicity gradient.
