1.1-mm cumulative (left panel) and differential (right panel) number counts derived using the corrections described in Sect. 5.4, for the sources detected at > 4.8σ in the main catalog. AGS19 is located at a position where the noise is artificially low, and has therefore not been taken into account. Previous (sub)millimeter cumulative number counts are also shown (Lindner et al. 2011; Scott et al. 2012; Karim et al. 2013; Hatsukade et al. 2013, 2016; Ono et al. 2014; Simpson et al. 2015b; Oteo et al. 2016; Carniani et al. 2015; Aravena et al. 2016; Fujimoto et al. 2016; Umehata et al. 2017; Geach et al. 2017; Dunlop et al. 2017). The different fluxes are scaled to 1.1 mm flux densities using S_1.1 mm/S_1.2 mm = 1.29, S_1.1 mm/S_1.3 mm = 1.48, S_1.1 mm/S_870 μm = 0.56. From the Umehata et al. (2017) study, we used only sources which do not have z = 3.09, (which means we are excluding the protocluster members). Results from single-dish surveys are shown with unfilled pentagon markers and are only indicative, they are not considered for model fitting. The gray curve shows the best-fit Schechter function (with 1-σ) uncertainties, the red curve shows the best-fit DPL function (with 1-σ).