  The Central Molecular Zone (CMZ) of the Galactic Center has to date only been
fully mapped at mm wavelengths with singledish telescopes, with resolution
about 30$^{\prime\prime}$ (1.2 pc). Using CARMA, we mapped the innermost 0.25
square degrees of the CMZ over the region between -0$.\kern-.25em ^{^\circ}$2$
\leq l \leq $0$.\kern-.25em ^{^\circ}$5 and -0$.\kern-.25em ^{^\circ}$2$ \leq b
\leq $0$.\kern-.25em ^{^\circ}$2 (90$\times$50 pc) with spatial and spectral
resolution of $\sim$10$^{\prime\prime}$ (0.4 pc) and $\sim$2.5 km/s,
respectively. We provide a catalog of 3mm continuum sources as well as spectral
line images of SiO(J=2-1), HCO$^{+}$(J=1-0), HCN(J=1-0), N$_{2}$H$^{+}$(J=1-0),
and CS(J=2-1), with velocity coverage VLSR= -200 to 200 km/s. To recover the
large scale structure resolved out by the interferometer, the
continuum-subtracted spectral line images were combined with data from the
Mopra 22-m telescope survey, thus providing maps containing all spatial
frequencies down to the resolution limit. We find that integrated intensity
ratio of I(HCN)/I(HCO$^{+}$) is anti-correlated with the intensity of the 6.4
keV Fe K$\alpha$, which is excited either by high energy photons or low energy
cosmic rays, and the gas velocity dispersion as traced by HCO$^{+}$ is
correlated with Fe K$\alpha$ intensity. The intensity ratio and velocity
dispersion patterns are consistent with variation expected from the interaction
of low energy cosmic rays with molecular gas.
