Evolution of C iv Absorbers. II. Where Does C iv Live?

We use the observed cumulative statistics of C iv absorbers and dark matter halos to infer the distribution of C iv-absorbing gas relative to galaxies at redshifts 0 <= z <= 5. We compare the cosmic incidence dN/dX of C iv absorber populations and galaxy halos, finding that massive L >= L halos alone cannot account for all the observed W ( r ) >= 0.05 angstrom absorbers. However, the dN/dX of lower-mass halos exceeds that of W ( r ) >= 0.05 angstrom absorbers. We also estimate the characteristic gas radius of absorbing structures required for the observed C iv dN/dX, assuming each absorber is associated with a single galaxy halo. The W ( r ) >= 0.3 angstrom and W ( r ) >= 0.6 angstrom C iv gas radii are similar to 30%-70% (similar to 20%-40%) of the virial radius of L (0.1L ) galaxies, and the W ( r ) >= 0.05 angstrom gas radius is similar to 100%-150% (similar to 60%-100%) of the virial radius of L (0.1L ) galaxies. For stronger absorbers, the gas radius relative to the virial radius rises across Cosmic Noon and falls afterwards, while for weaker absorbers, the relative gas radius declines across Cosmic Noon and then dramatically rises at z < 1. A strong luminosity-dependence of the gas radius implies highly extended C iv envelopes around massive galaxies before Cosmic Noon, while a luminosity-independent gas radius implies highly extended envelopes around dwarf galaxies after Cosmic Noon. From available absorber-galaxy and C iv evolution data, we favor a scenario in which low-mass galaxies enrich the volume around massive galaxies at early epochs and propose that the outer halo gas (>0.5 R ( v )) was produced primarily in ancient satellite dwarf galaxy outflows, while the inner halo gas (R ( v )) originated from the central galaxy and persists as recycled accreting gas.