Historically, few astronomical measurements have required sub-percent accuracy in photometry. Measuring SNIa fluxes
in order to determine cosmological parameters, however, often requires the comparison of images from different
telescopes, and at different redshifts. This can introduce a myriad of sources of error. Conventional methods of data
reduction are intrinsically flawed, either making assumptions about the effects of wavelength dependence in the response
function of the system or, when K-corrections are not performed, neglecting them altogether. We consider the
advantages of a method utilizing a direct, spectrally-resolved measurement of the entire system's response function
relative to a calibrated photodiode.
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