Intervening C IV absorbers are key tracers of metal-enriched gas in galaxy haloes over cosmic time. Previous studies suggest that the CIV cosmic mass density (omega(CIV)) decreases slowly o v er 1.5 ? z ? 5 before declining rapidly at z ? 5, but the cause of this downturn is poorly understood. We characterize the omega(C IV) evolution over 4.3 ?z ? 6.3 using 260 absorbers found in 42 XSHOOTER spectra of z -similar to 6 quasars, of which 30 come from the ESO Large Program XQR-30. The large sample enables us to robustly constrain the rate and timing of the downturn. We find that omega(C IV) decreases by a factor of 4.8 +/- 2.0 over the similar to 300 Myr interval between z similar to 4.7 and similar to 5.8. The slope of the column density (log N ) distribution function does not change, suggesting that C IV absorption is suppressed approximately uniformly across 13.2 <= log N /cm (-2) < 15.0. Assuming that the carbon content of galaxy haloes evolves as the integral of the cosmic star formation rate density (with some delay due to stellar lifetimes and outflow travel times), we show that chemical evolution alone could plausibly explain the fast decline in omega(C IV )over 4.3 ? z ?6.3. However, the C IV /C II ratio decreases at the highest redshifts, so the accelerated decline in omega(C IV) at z ? 5 may be more naturally explained by rapid changes in the gas ionization state driven by evolution of the UV background towards the end of hydrogen reionization.
