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We present a theoretical study of intergalactic metal absorption linesimprinted in the spectra of distant quasars during and after the Epoch ofReionization (EoR). We use high resolution hydrodynamical simulations at highredshift ($4 <z<8$), assuming a uniform UV background Haardt--Madau 12,post-processing with CLOUDY photoionization models and Voigt profile fitting toaccurately calculate column densities of the ions CII, CIV, SiII, SiIV and OIin the intergalactic medium (IGM). In addition, we generate mock observationsof neutral Hydrogen (HI) at $z<6$. Our simulations successfully reproduce theevolution of the cosmological mass density ($\Omega$) of CII and CIV, with$\Omega_{CII}$ exceeding $\Omega_{CIV}$ at $z >6$, consistent with the currentpicture of the tail of the EoR. The simulated CII exhibits a bimodaldistribution with large absorptions in and around galaxies, and some traces inthe lower density IGM. We find some discrepancies between the observed andsimulated column density relationships among different ionic species at $z=6$,probably due to uncertainties in the assumed UV background. Finally, oursimulations are in good agreement with observations of the HI column densitydistribution function at $z = 4$ and the HI cosmological mass density$\Omega_{HI}$ at $4 < z < 6$.

Simulated metal and HI absorption lines at the conclusion of Reionization