  Galaxy mergers are known to trigger both extended and central star formation.
However, what remains to be understood is whether this triggered star formation
is facilitated by enhanced star formation efficiencies, or an abundance of
molecular gas fuel. This work presents spatially resolved measurements of CO
emission collected with the Atacama Large Millimetre Array (ALMA) for 20
merging galaxies (either pairs or post-mergers) selected from the Mapping
Nearby Galaxies at Apache Point Observatory (MaNGA) survey. Eleven additional
merging galaxies are selected from the ALMA MaNGA QUEnching and STar formation
(ALMaQUEST) survey, resulting in a set of 31 mergers at various stages of
interaction and covering a broad range of star formation rates (SFR). We
investigate galaxy-to-galaxy variations in the resolved Kennicutt-Schmidt
relation (rKS: $\Sigma_{H_2}$ vs. $\Sigma_{SFR}$), the resolved molecular gas
main sequence (rMGMS: $\Sigma_{\star}$ vs. $\Sigma_{H_2}$), and the resolved
star-forming main sequence (rSFMS: $\Sigma_{\star}$ vs. $\Sigma_{SFR}$). We
quantify offsets from these resolved relations to determine if star formation
rate, molecular gas fraction, and/or star formation efficiency (SFE) is
enhanced in different regions of an individual galaxy. By comparing offsets in
all three parameters we can discern whether gas fraction or SFE powers an
enhanced $\Sigma_{SFR}$. We find that merger-induced star formation can be
driven by a variety of mechanisms, both within a galaxy and between different
mergers, regardless of interaction stage.
