  The spectral line energy distribution of carbon monoxide contains information
about the physical conditions of the star forming molecular hydrogen gas;
however, the relation to local radiation field properties is poorly
constrained. Using ~ 1-2 kpc scale ALMA observations of CO(3-2) and CO(4-3), we
characterize the CO(4-3)/CO(3-2) line ratios of local analogues of main
sequence galaxies at z ~ 1-2, drawn from the DYNAMO sample. We measure
CO(4-3)/CO(3-2) across the disk of each galaxy and find a median line ratio of
$R_{43} = 0.54^{+0.16}_{-0.15}$ for the sample. This is higher than literature
estimates of local star-forming galaxies and is consistent with multiple lines
of evidence that indicate DYNAMO galaxies, despite residing in the local
Universe, resemble main-sequence galaxies at z ~ 1-2. Comparing to existing
lower resolution CO(1-0) observations, we find $R_{41}$ and $R_{31}$ values in
the range $\sim 0.2-0.3$ and $\sim 0.4-0.8$ respectively. We combine our
kpc-scale resolved line ratio measurements with HST observations of H$\alpha$
to investigate the relation to star formation rate surface density and compare
this relation to expectations from models. We find increasing CO(4-3)/CO(3-2)
with increasing star formation rate surface density; however, models
over-predict the line ratios across the range of star formation rate surface
densities we probe, particularly at the lower range. Finally, SOFIA
observations with HAWC+ and FIFI-LS reveal low dust temperatures and no deficit
of [CII] emission with respect to the total infrared luminosity.
