  The chemical properties of high-z galaxies provide important information to
constrain galaxy evolutionary scenarios. However, widely-used metallicity
diagnostics based on rest-frame optical emission lines are not usable for
heavily dust-enshrouded galaxies (such as Sub-Millimeter Galaxies; SMGs),
especially at z>3. Here we focus on the flux ratio of the far-infrared
fine-structure emission lines [NII]205um and [CII]158um to assess the
metallicity of high-z SMGs. Through ALMA cycle 0 observations, we have detected
the [NII]205um emission in a strongly [CII]-emitting SMG, LESS J033229.4-275619
at z=4.76. The velocity-integrated [NII]/[CII] flux ratio is 0.043 +/- 0.008.
This is the first measurement of the [NII]/[CII] flux ratio in high-z galaxies,
and the inferred flux ratio is similar to the ratio observed in the nearby
universe (~0.02-0.07). The velocity-integrated flux ratio and photoionization
models suggest that the metallicity in this SMG is consistent with solar,
implying the chemical evolution has progressed very rapidly in this system at
z=4.76. We also obtain a tight upper limit on the CO(12-11) transition, which
translates into CO(12-11)/CO(2-1) <3.8 (3 sigma). This suggests that the
molecular gas clouds in LESS J033229.4-275619 are not affected significantly by
the radiation field emitted by the AGN in this system.
