Comparison between SFRD obtained by excluding the two [C II] emitters with optical/near-IR counterparts (red boxes and black circles, same as in Fig. 16) and that estimated by integrating the best fit curve to the 4.5 <  z <  6 LF obtained from all the continuum detections, including the two [C II] emitters (yellow boxes and brown open square). For comparison, we also report the results obtained by Loiacono et al. (2020) by integrating the [C II] LF of the serendipitous line emitters for field (i.e. lines separated by that of the ALPINE targets by > 2000 km s⁻¹: blue box and open up-side down triangle) and clustered sources (i.e. lines falling in the same spectral window of the ALPINE targets: green box and open triangle). The models by Madau & Dickinson (2014), Béthermin et al. (2017), and Pillepich et al. (2018) are also reported as black dashed, orange dot-dashed, and dark green solid curves, respectively. In addition, we plot the predictions obtained by modelling the CIB of Maniyar et al. (2018), as a light yellow dashed area, and by Lagache (2018) as violet triple-dot-dashed lines (pessimistic and optimistic cases).