  In this paper, we report our high-resolution
($0^{\prime\prime}.20\times0^{\prime\prime}.14$ or $\sim$$70\times49$ pc)
observations of the CO(6-5) line emission, which probes warm and dense
molecular gas, and the 434 $\mu$m dust continuum in the nuclear region of NGC
7130, obtained with the Atacama Large Millimeter Array (ALMA). The CO line and
dust continuum fluxes detected in our ALMA observations are $1230\pm74$ Jy km
s$^{-1}$ and $814\pm52$ mJy, respectively, which account for 100% and 51% of
their total respective fluxes. We find that the CO(6-5) and dust emissions are
generally spatially correlated, but their brightest peaks show an offset of
$\sim$70 pc, suggesting that the gas and dust emissions may start decoupling at
this physical scale. The brightest peak of the CO(6-5) emission does not
spatially correspond to the radio continuum peak, which is likely dominated by
an Active Galactic Nucleus (AGN). This, together with our additional
quantitative analysis, suggests that the heating contribution of the AGN to the
CO(6-5) emission in NGC 7130 is negligible. The CO(6-5) and the
extinction-corrected Pa-$\alpha$ maps display striking differences, suggestive
of either a breakdown of the correlation between warm dense gas and star
formation at linear scales of $<$100 pc or a large uncertainty in our
extinction correction to the observed Pa-$\alpha$ image. Over a larger scale of
$\sim$2.1\,kpc, the double-lobed structure found in the CO(6-5) emission agrees
well with the dust lanes in the optical/near-infrared images.
