tokens: only 13 SNe are removed as a result. The latter is much more impactful, however, removing ∼700 spectra (mostly from the SED Machine; Blagorodnova et al. 2018 ) and nearly as many SNe. In fact, this amounts to the most severe cut on SNe and the second most severe cut on spectra (after the ‘overlap’ cut). With future improvements to deepSIP it may be possible to revisit and lessen the extremity of this cut, but this will have to wait until those improvements can be realized. Irrelevant photometric passbands: After the cuts described above, the 60 140 photometric points that remain are in one of 62 different passbands, some of which are irrelevant to our analysis and must therefore be removed. By far, the primary factor in rendering observations in a given passband ‘irrelevant’ is if that band is too broad. For example, 4923 Gaia G -band (Jordi et al. 2010 ), 2104 Pan-STARRS w -band (Chambers Pan-STARRS Team 2018 ), 612 ATLAS c -band or o -band (Tonry et al. 2018 ), and many other wide-band observations are removed, along with a further 5061 unfiltered photometric points. A second factor in determining the relevance of a passband is the wavelengths of light that it passes. As our SDM uses a WLR implementation that is trained at optical and near-infrared wavelengths, we must discard passbands that lie outside this domain, thereby removing some Swift observations (Brown et al. 2014 ) among others. All told, 15 624 photometric points are removed, and those that remain are homogenized down to 21 distinct passbands. Photometric uncertainties: Of the remaining 44 516 photometric points, 10 429 do not include a symmetric uncertainty in the reported magnitude. We are able to ‘fix’ 6120 of these by taking the larger of their (asymmetric) lower and upper magnitude uncertainty estimates, but 4393 remain which have no identifiable quantitative uncertainty indicator. We take the conservative approach of removing these data, leaving us with just under 1200 SNe covered by ∼2900 spectra and ∼ 40 000 photometric points. 2 + Distinct passbands: As the SDM requires, at a minimum, two photometric points in different passbands (and a spectrum), we remove SNe that fail this requirement. This reduces the sample to 747 SNe with ∼2400 spectra and ∼ 35 000 photometric points. Literature search for photometric systems: While we have taken care above to homogenize the passbands in our sample (in the sense of resolving the differing names given to identical filters), we must also understand the photometric systems to which they belong. To do so, we visit the primary source provided by the OSC for each remaining point in our photometry sample (amounting to 248 sources) and attempt to determine the photometric system. We find that 26 SNe (covered by 5719 photometric points) are either not an SN Ia or are not an SN Ia subclass that can be handled by our WLR. These are dropped, as are an additional 7220 photometric points whose photometric system is either not clear or not
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