tokens: between the best-fit values obtained from fits of the F99 law to each object’s set of color excesses (see the last column of Tables 4 and 5 ) and the values inferred from individual color excess measurement and the F99 law (see Table 3 ). In doing so these comparisons are made for each of the four color excess combinations: (top-left panel), (top-right panel), (bottom-left panel), and (bottom-right panel). Included in each panel’s sub-plots is the root-mean-square (rms) difference between the two methods. In general the values obtained by the two methods are in good agreement, as indicated by the fact that the data follow the black lines in the plots. Fig. 17 from as given in Tables 4 and 5 versus . The Poznanski et al. (2012) relation is over-plotted as a solid blue line. Empty symbols indicate upper limits on . A linear fit between the two quantities (with intercept fixed to zero) is drawn as a black dashed line and the corresponding fit expression is reported in the top-left corner of the figure. This expression has been obtained by linearly fitting all the points including the limits. We find that the optical and NIR color combinations providing the smallest dispersion among the suite of , , , and color combinations considered in this work are as follows. In the case of and time relative to the and colors exhibit minimal dispersion in , while for and time relative to the and colors exhibit minimal dispersion. Moreover, for and time relative to the and colors exhibit minimal dispersion in , while for and time relative to the and colors exhibit minimal dispersion. Discrepancies between the two methods are largely due to different spectral lines affecting the measurement from a single color combination more than the global fit value. We now compare the value derived for each object in the sample to their measurement obtained from visual-wavelength spectra (Holmbo et al., in prep.). Specifically, average values given in Tables 4 and 5 are plotted in Fig. 17 vs. . Over-plotted in the figure is the relation (solid blue line) found between these parameters by Poznanski et al. (2012) , as well as a linear fit (dashed line) to the data assuming when . The latter of these is given by . As expected there is significant scatter between the two quantities (cf. Poznanski et al. 2011 ). Returning to the CDFs shown in Fig. 14 , it is interesting to note that the SNe Ic consistently exhibit higher extinction values compared to SNe IIb and SNe Ib, and this holds independent of the assume value of . This is consistent with the findings of Anderson et al. (2015) whom used pixel statistics based on emission to study the environments of SNe by tracing on-going (16 Myr old) star formation within SN host galaxies. Anderson et al. found that SNe Ic show a statistically significant preference for being located in regions of on-going star formation, while SNe Ib are located in regions that do not as closely follow ongoing star formation. The implications are that
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