Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties

Recent JWST observations have uncovered a population of compact, high-redshift ($z>6$) galaxies exhibiting extreme nebular conditions and enhanced nitrogen abundances that challenge standard chemical evolution paradigms. We present a joint UV and optical abundance analysis using a new suite of $\mathtt{\text{Cloudy}}$ photoionization models covering a wide density range ($n_e={10}^2-{10}^9$ cm${}^{-3}$), combined with HST and JWST spectroscopy for a sample of star-forming galaxies across $0.0\lesssim z\lesssim 10.6$. We find that assuming uniform, low-density conditions ($n_e\sim {10}^2$ cm${}^{-3}$) in high-density environments ($n_e\sim {10}^5$ cm${}^{-3}$) can bias nebular diagnostics by overestimating $T_e$ (up to 1800 K), overpredicting $\log U$ (by $>1$ dex), and underestimating O/H (up to 0.67 dex), while only modestly inflating N/O. Therefore, robust abundance determinations at high-$z$ require a multi-phase density model. Using this model, we recalculate O/H and N/O abundances for our sample and present the first $\log U$ diagnostics and ICFs for high-ionization UV N lines. We find that the UV tracers systematically overestimate N/O by $\sim 0.3-0.4$ dex relative to the optical benchmark. We find that N/O increases with redshift, correlating with both $n_e$ and star formation rate surface density (${\mathrm{\Sigma }}_{\mathrm{S}\mathrm{F}\mathrm{R}}$), suggesting that N/O is temporarily enhanced in compact, high-pressure environments. However, the $n_e$ evolution with $z$ is more gradual than the $(1+z{)}^3$ scaling of virial halo densities, suggesting that $n_e$evolution is shaped by both cosmological structure growth and baryonic processes. These trends point to prompt N/O enrichment potentially driven by very massive stars, with key implications for interpreting UV emission and determining reliable chemical abundances from JWST observations of the early universe.