Evolution of various powers as a function of the total decay power emitted (top-left panel) or absorbed (all other panels) by the ejecta for our set of simulations and over the time span from about 200 to about 500 d after explosion. From left to right and top to bottom, we show the fractional power absorbed in the ejecta, that fraction coming from positrons, and the fractions absorbed in the H-rich (He-star explosion models are excluded since H deficient), He-rich, O-rich ,and Fe/Si-rich material.