Total [CII] luminosity as a function of SFR for the High-z model (red) and Schimek et al. (2024a,b) (purple). In the top panel we compare our models to observational values from Harikane et al. (2020) at z ∼ 6, Carniani et al. (2018) at z = 5 − 7, Capak et al. (2015) at z = 5.1 − 5.7, Ouchi et al. (2013) at z ≃ 6.6, Maiolino et al. (2015) at z = 6.8 − 7.1, Hashimoto et al. (2019) at z = 7.15, Witstok et al. (2022) at z = 6.7 − 7, Heintz et al. (2023) at z = 8.5, Algera et al. (2024) at z = 7.3, Bakx et al. (2020) at z = 8.31, Schaerer et al. (2020) (ALPINE) at z = 4 − 8, Fujimoto et al. (2021) at z = 6, Ren et al. (2023) at z = 7.2, Carniani et al. (2020) at z ∼ 7 − 9, Kanekar et al. (2013) at z = 6.56, González-López et al. (2014) at z = 6.5 − 11, Ota et al. (2014) at z = 6.9, Willott et al. (2015) at z = 6, Knudsen et al. (2016, 2017) at z = 6 − 7.6, Pentericci et al. (2016) at z = 6.6 − 7.1, Bradač et al. (2017) at z = 6.7, Decarli et al. (2017) at 6 − 6.6, Khusanova et al. (2022) at z = 6, Vanderhoof et al. (2022) at z = 4.5, CRISTAL (Posses et al. 2025) at z = 5.5, Rowland et al. (2024) at z = 7.31, Fujimoto et al. (2024) at z = 8.5 (upper limit), and Schouws et al. (2025a,b) at z = 14.2 (upper limit). We include relations from Carniani et al. (2020) at z > 6, De Looze et al. (2014) for local SB galaxies, Harikane et al. (2020) at z = 6 − 9 and Schaerer et al. (2020) at z = 4 − 8. In the bottom panel, we compare our models to simulated values from Katz et al. (2022) (z = 6), Pallottini et al. (2019) (z = 6), Lupi et al. (2020) (z = 6), Pallottini et al. (2022) (z = 7.7), and Ramos Padilla et al. (2023) (z = 6). The relations are from Arata et al. (2020) (z = 6 − 9), Vallini et al. (2015) (z ≈ 7), Olsen et al. (2017) (z ≃ 6), and Leung et al. (2020) (z ≃ 6).