Dependence of the predicted CS₂, CH₄, CO, and SO₂ abundances, quantified as the column density (molecules per square centimeter) integrated over the JWST-observable pressure region (P ≤ 2 mbar), across a sample of gas giant exoplanets spanning T_eq = 350–1120 K, assuming T_int = 100 K and K_zz = 10⁸ cm² s⁻¹ for both 1× and 10× Z_⊙. Colors denote different chemical species, while line styles indicate metallicity: solid lines represent 1​​​​​× Z_⊙ and dotted lines represent 10​​​​× Z_⊙. The predicted SO₂ column densities remain below 10¹⁶ molecules cm⁻² for all planets considered here, except for the 10​​× Z_⊙ model of WASP-39 b. For V1298 Tau b, additional models with T_int = 400 K were computed at both 1× and 10​​​​​​×  Z_⊙ and are denoted by diamond and star symbols, respectively. The predicted CS₂ and SO₂ column densities for the T_int = 400 K models are nearly identical and therefore overlap. The black horizontal dotted line indicates the estimated CS₂ detectability threshold column density of 10¹⁸ molecules cm⁻². This corresponds approximately to a VMR of 1 ppmv (10⁻⁶). Planets labeled along the top x-axis are gas giants (R ≥ 0.50 R_J, M ≤ 1.1 M_J) that have been or are planned to be observed with JWST using modes capable of probing CS₂ absorption (i.e., NIRSpec/G395M, G395H, or PRISM). Their corresponding T_eq values, ranging from 350 to 852 K, are also indicated. These targets represent potential candidates for future CS₂ detections.