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We test whether we can predict optical spectra from deep-field photometry ofdistant galaxies. Our goal is to perform a comparison in data space,highlighting the differences between predicted and observed spectra. The LargeEarly Galaxy Astrophysics Census (LEGA-C) provides high-quality optical spectraof thousands of galaxies at redshift $0.6<z<1$. Broad-band photometry of thesame galaxies, drawn from the recent COSMOS2020 catalog, is used to predict theoptical spectra with the spectral energy distribution (SED) fitting codeProspector and the MILES stellar library. The observed and predicted spectraare compared in terms of two age and metallicity-sensitive absorption features(H$\delta_\mathrm{A}$ and Fe4383). The global bimodality of star-forming andquiescent galaxies in photometric space is recovered with the model spectra.But the presence of a systematic offset in the Fe4383 line strength and theweak correlation between the observed and modeled line strength imply thataccurate age or metallicity determinations cannot be inferred from photometryalone. For now we caution that photometry-based estimates of stellar populationproperties are determined mostly by the modeling approach and not the physicalproperties of galaxies, even when using the highest-quality photometricdatasets and state-of-the-art fitting techniques. When exploring a new physicalparameter space (i.e. redshift or galaxy mass) high-quality spectroscopy isalways needed to inform the analysis of photometry.

Less is less: photometry alone cannot predict the observed spectral indices of $z\sim1$ galaxies from the LEGA-C spectroscopic survey