Dust attenuation parameters as a function of V-band attenuation, A_V. The left panel shows the UV-optical slope (S), and the right panel displays the UV bump strength (B) as a function of A_V. Gray stars represent individual measurements of S and B for galaxies of our sample, with corresponding 1σ error bars derived through a bootstrapping method. Black stars indicate the median values of S and B for galaxies binned by A_V, with errors representing the 1σ dispersion of each bin. The best-fit correlations and their 1σ uncertainties for the entire sample and the intermediate- and high-z subsets are shown by solid magenta lines, respectively. The shaded regions indicate the uncertainty ranges. Literature results for nearby (Decleir et al. 2019; Salim & Narayanan 2020) and intermediate-z galaxies (Buat et al. 2011, 2012; Scoville et al. 2015; Reddy et al. 2015; Shivaei et al. 2020a) are depicted as blue and green symbols, respectively. High-z objects (Boquien et al. 2022; Markov et al. 2023; Fisher et al. 2025; Ormerod et al. 2025) are shown as olive, orange, brown, and red symbols. The error bars indicate their 1σ uncertainties. The dotted blue and green lines indicate the average attenuation curve slopes and UV bump strengths for local starbursts with A_V ∼ 0.4 − 1.0 (Calzetti et al. 2000) and for galaxies at z ∼ 0.5 − 2.0 with A_V ∼ 0.5 − 2.25 (Kriek & Conroy 2013), respectively. Inset panel: Black lines represent the best-fit correlations and their 1σ uncertainties for the subsets grouped by redshift. The shaded regions indicate the uncertainty ranges. The S − A_V correlation from Salim & Narayanan (2020) for a nearby (z ∼ 0) sample is shown as a dashed blue line in the left panel.