[CII] line luminosity as a function of the SFR. In the left panel, our models are compared with observational constraints available from the literature at a similar redshift, while the right panel shows the comparison with other theoretical works. The circles represent the whole halo, crosses represent the main disc, and the pentagon the merging companions A and B. The CGM is shown using diamond symbols. The observational data are taken from: Kanekar et al. (2013) at z = 6.5, Ouchi et al. (2013) at z = 6.5, González-López et al. (2014) at z = 6.5 − 11, Ota et al. (2014) at z = 6.9, Schaerer et al. (2015)z = 6.8 − 7.5, Capak et al. (2015) for z = 5.1 − 5.7, Willott et al. (2015) for z = 6, Maiolino et al. (2015) for z = 6.8 − 7.1, Knudsen et al. (2016, 2017) for z = 6 − 7.6, Pentericci et al. (2016) for z = 6.6 − 7.1, Bradač et al. (2017) for z = 6.7, Decarli et al. (2017) for z = 6 − 6.6, Khusanova et al. (2022) for z = 6, Vanderhoof et al. (2022) for z = 4.5, Fujimoto et al. (2021) for z = 6, Witstok et al. (2022) for z = 6 − 7, Hashimoto et al. (2019) for z ∼ 7, Harikane et al. (2020) for z ∼ 6, the ALPINE data for z = 4 − 8, Schaerer et al. (2020), Algera et al. (2024) for z = 7.3, Fujimoto et al. (2022) for z = 8.4, Ren et al. (2023) for z = 7.2, and Carniani et al. (2018) for z = 5 − 7. The relation shown in grey is by De Looze et al. (2014) for SB galaxies, and the relation shown in purple by Carniani et al. (2020) for high-redshift galaxies. In addition, on the right panel, we compare our results to simulation data by Pallottini et al. (2019, 2022); Katz et al. (2022) and Lupi et al. (2020). The relation by Vallini et al. (2015) based on physical motivated models for a metallicity of Z = 0.5 Z_⊙ can be seen in grey dashed, the relation by Arata et al. (2020) in dot-dashed, the relation found by Leung et al. (2020) in purple, and the Olsen et al. (2018) data in grey dot-dashed.