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Type Ia Supernovae are thermonuclear explosions of white dwarf stars. Theyplay a central role in the chemical evolution of the Universe and are animportant measure of cosmological distances. However, outstanding questionsremain about their origins. Despite extensive efforts to obtain natalinformation from their earliest signals, observations have thus far failed toidentify how the majority of them explode. Here, we present infant-phasedetections of SN 2018aoz from a brightness of -10.5 absolute AB magnitudes --the lowest luminosity early Type Ia signals ever detected -- revealing ahitherto unseen plateau in the $B$-band that results in a rapid redward colorevolution between 1.0 and 12.4 hours after the estimated epoch of first light.The missing $B$-band flux is best-explained by line-blanket absorption fromFe-peak elements in the outer 1% of the ejected mass. The observed $B-V$ colorevolution of the SN also matches the prediction from an over-density of Fe-peakelements in the same outer 1% of the ejected mass, whereas bluer colors areexpected from a purely monotonic distribution of Fe-peak elements. The presenceof excess nucleosynthetic material in the extreme outer layers of the ejectapoints to enhanced surface nuclear burning or extended sub-sonic mixingprocesses in some normal Type Ia Supernova explosions.

Infant-phase reddening by surface Fe-peak elements in a normal Type Ia Supernova