Core-collapse supernovae are spectacular explosions that mark the deaths of massive stars and can briefly outshine their entire host galaxy. Observing the light from a core-collapse supernova — its light curve and spectra — can provide valuable clues about the progenitor star, stellar evolution, the explosion mechanism, element synthesis, and even the formation of neutron stars and black holes. However, interpreting these observations correctly is a formidable challenge, one that requires detailed and accurate computational modeling. In this talk, I will review our current theoretical understanding of core-collapse supernovae and present light curves and spectra for a suite of 62 core-collapse supernova models. I will categorize our light curves based on morphology and show that the categories relate to the radius of the star and the mass of the hydrogen envelope. Finally, I will describe the first-of-its-kind pipeline I developed in order to make these predictions possible, starting from a massive progenitor model, through a self-consistent explosion in spherical symmetry, to electromagnetic counterparts. This opens the door to more detailed analyses of the collective properties of core-collapse supernovae and their electromagnetic signatures.