Mg II and C IV cumulative covering fraction within R < 100 kpc. Upper panels: The results for strong (W_r ≥ 1 Å, left panel) and weak (0.4 ≤ W_r < 1.0 Å, right panel) Mg II absorbers observed around LAEs in MAGG (black) are consistent with the redshift evolution model calibrated at z ≲ 1.3 by Lan (2020) for star-forming galaxies with stellar mass log(M_⋆/M_⊙) = 9.0 − 9.5 and log(M_⋆/M_⊙) = 9.5 − 10. Also shown is the covering fraction of Mg II gas observed around [O III] emitters by Dutta et al. (2020) at z ≈ 1. Lower panels: Results for W_r ≥ 0.1 Å Mg II (right panel, black pentagon) and C IV (left panel, black diamond) samples, without any distinctions between weak and stronger absorbers. Also shown are the results from Nielsen et al. (2013) (crosses), Dutta et al. (2020) (pentagon) and Anand et al. (2021) (up triangle, W_r ≥ 0.4 Å), Dutta et al. (2021) (star), Rudie et al. (2019) (cross, log(N/cm⁻²)≥13.0) corresponding to W_r ≳ 0.04 Å in linear regime), and Banerjee et al. (2023) (down triangle, log(N/cm⁻²)≥12.5) corresponding to W_r ≳ 0.01 Å). Horizontal error bars mark the explored redshift range. The evolution of the C IV covering fraction is consistent with the star formation rate density as parametrized by Madau & Dickinson (2014) (dotted line, arbitrary normalization).