  We add a suite of chemical abundances to the MACER (Massive AGN Controlled
Ellipticals Resolved) 2D code, by solving 12 additional continuity equations
for H, He, C, N, O, Ne, Mg, Si, S, Ca, Fe and Ni respectively with sources from
AGB stars and supernovae of type Ia and II with metal yields based on standard
stellar physics. New stars, formed in Toomre unstable circumnuclear disks (of a
size $\lesssim150$ parsec), are assumed to have a top-heavy initial mass
function with a power index of 1.65. The metal dilution effects due to cosmic
accretion are also included. With the high resolution of few parsecs in central
regions, resolved black hole accretion and AGN feedback, we can track the metal
enrichment, transportation and dilution throughout the modeled massive
elliptical galaxy of velocity dispersion $\sim280$ km/s. We retrieve the
chemical composition of the BAL winds launched by the central AGN, synthesize
the X-ray features of the hot ISM, and find that (1) the simulated metallicity
in the BAL winds could be up to $\sim 8 Z_\odot$, while that of the hot ISM in
the host galaxy is $\sim 2.3 Z_\odot$, matching well with SDSS observations of
BLR gas; (2) the X-ray emitting hot gas is metal enriched with a typical value
$\sim2.5 Z_\odot$; (3) the circumunuclear cold gas disk, where the metals are
condensed, further enriched and recycled, plays a critical role in the metal
enrichment; (4) the black hole accretion rate $\dot{M}_{\rm BH}$ linearly
correlates with the star formation rate $\dot{M}_\star^+$ in the circumnuclear
disk, i.e, $\dot{M}_\star^+ \sim 7.7 \dot{M}_{\rm BH}$, but lagged in time by
roughly $10^6$ years.
