tokens: to estimate the host-galaxy reddening and preferred dust extinction law. First, following Goldhaber et al. (2001) , we measured the stretch factor s that multiplies the temporal axis of the light curve providing the best match of the Hsiao et al. (2007) SN Ia template to the observations. In our case, we restricted the fit to the first 15 days, to avoid the dependence of the light curve on secondary parameters and the light excess detected for SN 2016hnk at later times, and obtained an s = 0.59 ± 0.04. The modified decline rate Δ m 15, s ( B ) is then defined as the magnitude difference between the peak and the reference epoch, 15 days × s (measured in the template), divided by the s factor [Δ m 15, s = , which in our case is = = 1.803 ± 0.200 mag. The measured value of Δ m 15, s ( B ) determines the theoretical model from Höflich et al. (2017) that is used as a reference to correct the B - and V -band light curves, the B versus ( B − V ) and V versus ( B − V ) diagrams, and the ( B − V ) evolution of SN 2016hnk. In the CDMagic fit we fixed the to the value previously obtained with SN OO P Y and the distance modulus measured from the assumed cosmology ( μ = 34.195 mag), and only left as free parameters E ( B − V ) and R V . While the color excess is estimated from the shift between the uncorrected (as observed and Milky Way dust-corrected) and the corrected points that best match the template, the R V is measured from the direction of this shift in the color-magnitude diagrams. In Fig. 9 we show, as an example, the absolute V and vs. B − V diagram, including a number of SNe Ia from the Carnegie Supernova Project I (CSP-I; Krisciunas et al. 2017 ) and the 1991bg-like SN Ia 2005ke (empty triangles) for reference, models from Höflich et al. (2017) with different stretch factor (green lines), and SN 2016hnk data before (blue) and after corrections (red). We obtained an E ( B − V ) of 0.45 ± 0.08 mag, consistent with previous methods, and an R V = 2.1 ± 0.6, which we use hereafter; however, we note that our results are not significantly dependent on the particular choice of R V . Fig. 9. Representative panel for the CDMagic method, where a simultaneous fit in the B - and V -band light curves, the B vs. ( B − V ) and V vs. ( B − V ) diagrams, and the ( B − V ) evolution, is performed. More details are given in, for example, Fig. 13 in Höflich et al. (2017) . We show the absolute V -band vs. ( B − V ) diagram populated with eight normal SNe Ia from the CSP-I ( Krisciunas et al. 2017 ; SNe 2004ef, 2005eo, 2005el, 2005iq, 2005ki, 2005M, 2006bh, 2006D; in differnet symbols), the SN Ia 1991bg-like 2005ke (empty triangles), and the uncorrected (blue) and corrected (red) SN 2016hnk data points. Models from Höflich et al. (2017) are shown in green for reference; the two arrows are the reddening vectors representing the direction to which the data points are shifted when affected by R V = 3.2 and R V = 1.0. SN 2016hnk corrected data points lie on top of the
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