  This {\it supplement} paper presents the maps of HCN $J$=4-3, HNC $J$=1-0,
$\mathrm{H^{13}CN}$ $J$=1-0, and HC$_3$N $J$=10-9 for the Galactic central
molecular zone (CMZ), which have been obtained using the Atacama Submillimeter
Telescope Experiment and Nobeyama Radio Observatory 45-m telescope.
Three-dimensional maps (2-D in space and 1-D in velocity) of the gas kinetic
temperature ($T_\mathrm{kin}$), hydrogen volume density ($n_\mathrm{H_2}$), and
fractional abundances of eight molecules (HCN, HNC, $\mathrm{HC_3N}$, HCO$^+$,
$\mathrm{H_2CO}$, SiO, CS, and $\mathrm{N_2H^+}$) have been constructed from
our and archival data. We have developed a method with hierarchical Bayesian
inference for this analysis, which has successfully suppressed the artificial
correlations among the parameters created by systematic errors due to the
deficiency in the simple one-zone excitation analysis and the calibration
uncertainty. The typical values of $T_\mathrm{kin}$ and $n_\mathrm{H_2}$ are
$10^{1.8}\ $K and $10^{4.2}\ \mathrm{cm}^{-3}$, respectively, and the presence
of an additional cold/low-density component is also indicated. The distribution
of high-temperature regions is poorly correlated with known active star-forming
regions, while a few of them coincide with shocked clouds. Principal component
analysis has identified two distinct groups in the eight analyzed molecules:
one group with large PC1 and PC2 scores and the other with a large
$T_\mathrm{kin}$ dependence, which could be explained using two regimes of
shock chemistry with fast ($\gtrsim 20\ \mathrm{km\,s}^{-1}$) and slow
($\lesssim 20\ \mathrm{km\,s}^{-1}$) velocity shocks, respectively. This
supports the idea that the mechanical sputtering of dust grains and the
mechanical heating play primary roles in the chemical and thermal processes in
CMZ clouds.
