SN Ia rates measured at different redshifts and diverse fits to them. Red circles are D04 data from Dahlen et al. (2004); green squares come from the CANDELS program (Rodney et al. 2014); blue triangles are from the Subaru/XMM-Newton Deep Survey (Okumura et al. 2014); inverted black triangles correspond to the HST Cluster Supernova Survey (Barbary et al. 2012). The red long-dashed line is a fit to the D04 data, done as in AKH05. The green short-dashed line is the same fit to the CANDELS data shown in Figure 11 of Rodney et al. (2014), while the magenta dot-dashed line corresponds to the rates used by HB2010 (private communication). The solid black line is a fit to the rates given in Table 6 of Graur et al. (2014) (see next figure for details), and the two black dotted lines are its ±1σ limits. Finally, the blue solid line is the same fit as in Figure 11 of Okumura et al. (2014) to the Subaru/XMM-Newton Deep Survey data, and the two blue long-dashed–short-dashed lines its ±1σ limits. Note that the upper 1σ limit just fits the two highest measured rates. The ±1σ regions around the rates from Okumura et al. (2014) have been traced by calculating the error using the statistical and systematic errors of the points measured by these authors. Note that the upper systematic errors include 50% extinction by dust, which explains why the upper error line is more distant from the main fit than the lower one.