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Uncertainties in the calibration of the various samples comprise the largest systematic uncertainty in our analysis. In Fig, we show a schematic describing the calibration of the various subsamples. The overall systematic uncertainty in the calibration of our combined PS1+lz sample may be expressed as the combination of three uncertainties. The first component encompasses systematic uncertainties in the nightly photometry and how well the filter bandpasses are measured. For the PS1 sample, R14 presents analysis of the systematic uncertainty due to spatial and temporal uncertainties in the nightly photometry. T12 presents the uncertainty in how well the bandpasses are measured (uncertainty of filter edges.  Spatial and temporal variation of the filter bandpasses propagate into our total calibration uncertainty in three ways: how the catalog photometry is determined, how the photometry of the Calspec standards is determined, and how the photometry of the supernovae is determined. We expect that the uncertainty in the nightly zeropoints to be small. We find Figure \ref{fig:A} by comparing Pan-STARRs and SDSS photometry that any variation of the PS1 photometry across the focal plane for colors $0.4\cite{Winkel_2016}  The second major component of the total calibration uncertainty is in determining the flux zeropoints of each filter based on observations of astronomical standards. Since the accuracy of the internal PS1 measurements of the flux zeropoints is not better than $1\%$, the zeropoints are adjusted so that the observed photometry of HST Calspec standards (e.g., AB - HST Calspec