  We utilize the ALMA-MaNGA QUEnch and STar formation (ALMaQUEST) survey to
investigate the kpc-scale scaling relations, presented as the resolved star
forming main sequence (rSFMS: $\Sigma_{\rm SFR}$ vs. $\Sigma_{*}$), the
resolved Schmidt-Kennicutt relation (rSK: $\Sigma_{\rm SFR}$ vs. $\Sigma_{\rm
H_{2}}$), and the resolved molecular gas main sequence (rMGMS: $\Sigma_{\rm
H_{2}}$ vs. $\Sigma_{*}$), for 11478 star-forming and 1414 retired spaxels
(oversampled by a factor of $\sim20$) located in 22 green valley (GV) and 12
main sequence (MS) galaxies. For a given galaxy type (MS or GV), the retired
spaxels are found to be offset from the sequences formed by the star-forming
spaxels on the rSFMS, rSK, and rMGMS planes, toward lower absolute values of
sSFR, SFE, and $f_{\rm H_{2}}$ by $\sim$ 1.1, 0.6, and 0.5 dex. The scaling
relations for GV galaxies are found to be distinct from that of the MS
galaxies, even if the analyses are restricted to the star-forming spaxels only.
It is found that for star-forming spaxels, sSFR, SFE, and $f_{\rm H_{2}}$ in GV
galaxies are reduced by $\sim$0.36, 0.14, and 0.21 dex, respectively, compared
to those in MS galaxies. Therefore, the suppressed sSFR/SFE/$f_{\rm H_{2}}$ in
GV galaxies are associated with not only an increased proportion of retired
regions in GV galaxies but also a depletion of these quantities in star-forming
regions. Finally, the reduction of SFE and $f_{\rm H_{2}}$ in GV galaxies
relative to MS galaxies is seen in both bulge and disk regions (albeit with
larger uncertainties), suggesting that statistically, quenching in the GV
population may persist from the inner to the outer regions.
