Fig. 12.
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ℱr2 as a function of x1 for SNe Ia in our cosmological sub-sample. We fit the population with a broken line (blue) and linear fit (black, dashed). We find the best-fit value of the stretch split to be at x10 = − 0.5 ± 0.2. The blue points show the data binned by stretch, taking the mean and standard error of the mean in each bin.
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