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tokens: derived from CfA3 in red. 5.3 Comparison of light-curve fitter results To make any cosmological statements based on the results in the previous section is beyond the scope of this paper, as this would require a detailed study and justification of the utilized light-curve fitters and their parameters, among many other considerations. It is interesting and possible, however, to compare results from the two light-curve fitters we employ to check for consistency. As the principal quantity of interest when fitting the light curves of SNe Ia is distance, we will focus our comparison on the derived distance moduli. The left-hand plot in Fig. 12 compares the distance moduli from snoopy and mlcs2k2 after correcting to put the measurements on the same scale (so that relative distance moduli are compared, independent from assumptions about the Hubble constant). This correction consists of adding an offset to the distance moduli from each fitter such that the value of H 0 measured from each set of results yields 65 km s −1 Mpc −1 . We perform this comparison only for spectroscopically normal SNe Ia in our sample for which snoopy finds Δ m 15 1.7 mag and for which z > 0.01. Of course, further restrictions should be placed when selecting a sample for cosmological purposes, but our selection is reasonable for performing a general comparison. We find strong agreement between the two sets of corrected distance moduli – a Kolmogorov–Smirnoff test gives a P -value of 1.000. The median residual is −0.026 mag with a statistical dispersion of 0.135 mag. Figure 12. Comparison of the (scaled) distance modulus and host-galaxy reddening results from both light-curve fitters for the selected subset of our data set. If we were to ensure consistency in choosing the parameters for each light-curve fitter, the residuals would almost certainly decrease. In particular, when fitting with mlcs2k2 , we place an exponentially decaying prior on A V , but no such prior was imposed with snoopy . This difference may well manifest in statistically and systematically different results for host-galaxy reddening and distance moduli between the two fitters. We compare host-galaxy reddening results in the right-hand panel of Fig. 12 , where for mlcs2k2 we have converted to reddening using E ( B − V ) host = A V / R V , with R V = 1.7. The agreement is reasonable, with a median residual of −0.056 mag and statistical uncertainty of 0.055 mag. Furthermore, the facts that the median residual ( snoopy minus mlcs2k2 ) is negative and that the disagreement is most severe for small E ( B − V ) host are consistent with what one might expect given the prior imposed by mlcs2k2 . 6 CONCLUSION In this paper, we present BVRI (along with some unfiltered) light curves of 93 SNe Ia derived from images collected by the LOSS follow-up program primarily over the interval from 2009 to 2018, but with several instances as early as 2005. Careful and consistent observational and processing techniques ensure