The dust masses inferred for SN 2018bsz, compared with literature values for other CCSNe. We find that SN 2018bsz formed 10 times more dust than normal CCSNe at similar epochs. We fit the evolution of SN 2018bsz and all other CCSNe separately, using M_dust ∝ t^2.4 (adopting the SN 2010jl ejecta dust evolution from C. Gall et al. 2014), and show the evolution in black dashed–dotted and gray dotted lines, respectively. The gray areas indicate the 95% confidence level, incorporating dust mass uncertainties to fit the points for SN 2018bsz and other CCSNe. The blue dashed line shows the evolution of the dust mass in SN 1987A inferred by R. Wesson et al. (2015). See the webpage https://www.nebulousresearch.org/dustmasses/ for the full collection; the SNe and references we used in this figure are for SN 1987A (We note that E. Dwek & R. G. Arendt 2015 report high dust masses at early epochs for SN 1987A. However, we do not plot these here as they are incompatible with the observed gradual evolution of the emission-line profiles (R. Wesson & A. Bevan 2021).) (M. Matsuura et al. 2011; R. Indebetouw et al. 2014; M. Matsuura et al. 2015; R. Wesson et al. 2015; A. Bevan & M. J. Barlow 2016), SN 1993J (A. Bevan et al. 2017), SN 1998S (M. Pozzo et al. 2004), SN 1999em (A. Elmhamdi et al. 2003), SN 2003gd (B. E. K. Sugerman et al. 2006; W. P. S. Meikle et al. 2007), SN 2004dj (T. Szalai et al. 2011), SN 2004et (R. Kotak et al. 2009), SN 2005ad and SN 2005af (T. Szalai & J. Vinkó 2013), SN 2005ip (O. D. Fox et al. 2010; M. Stritzinger et al. 2012; A. Bevan et al. 2019), SN 2006bc (J. S. Gallagher et al. 2012), SN 2006jc (I. Sakon et al. 2009), SN 2006jd (M. Stritzinger et al. 2012), SN 2007it (J. E. Andrews et al. 2011), SN 2007od (J. E. Andrews et al. 2010), SN 2010jl. (For SN 2010jl, we show the dust masses assuming carbon dust in A. Sarangi et al. 2018a). (K. Maeda et al. 2013; A. Sarangi et al. 2018a; A. M. Bevan et al. 2020), SN 2011ja (J. E. Andrews et al. 2016), SN 2014C (S. Tinyanont et al. 2019a), ASASSN-14jb (N. Meza et al. 2019), and SN 2017eaw (S. Tinyanont et al. 2019b).