Example PRISM spectrum (top left) and photometry (bottom left) for a galaxy in the Wide survey (3D-HST ID: UDS 22634). Both the spectrum and the photometry are fit with Bagpipes (Carnall et al. 2018, 2019), with the best-fit models and their dispersion overplotted. The right panels show posterior probability distributions for the stellar metallicity (top right) and age (bottom right) for an exponentially declining star formation history. The spectroscopic fit (filled histogram) results in better-constrained posteriors with a significantly different physical interpretation than would be possible with photometry alone (see also Kriek et al. 2006).