  How do galaxies of different luminosities contribute to the metal absorber
populations of varying species and strength? We present our analysis of the
predicted metal contributions from galaxies as observed in quasar absorption
line spectra during the end of the Epoch of Reionization (EoR; $10 \geq z \geq
5.5$). This was done by implementing on-the-fly particle tracking into the
latest \textsc{Technicolor Dawn} simulation and then linking CII, CIV, SiII,
SiIV, OI, and MgII absorbers to host galaxies in post-processing. We define the
Host Galaxy Luminosity Distribution (HGLD) as the rest-frame ultraviolet
luminosity distribution of galaxies contributing ions to an absorber, weighted
by the fractional contribution, and compute its dependence on ion and absorber
strength. The HGLD shape is predicted to be indistinguishable from the field
luminosity function, indicating that there is no relationship between the
absorber strength or ion and the luminosity of the dominant contributing
galaxy. Switching from galaxy luminosity to stellar mass, the predicted host
galaxy mass distributions (HGMD) indicate that more-massive galaxies contribute
a higher fraction of metal ions to absorbers of each species, with the HGMD of
stronger absorbers extending out to higher masses. We conclude that the
fraction of absorbing metal ions contributed by galaxies increases weakly with
stellar mass, but the scatter in luminosity at fixed stellar mass obscures this
relationship. For the same reason, we predict that observational analyses of
the absorber-galaxy relationship will uncover stronger trends with stellar mass
than with luminosity.
