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To date, the question of which progenitor channel can reproduce the observedrate of Type Ia supernovae (SNe Ia) remains unresolved, with the single anddouble degenerate scenarios remaining the leading contenders. The formerimplies a large population of hot accreting white dwarfs with photospherictemperatures of T ~ 10^5-10^6 K during some part of their accretion history. Weshow that in early-type galaxies, a population of accreting white dwarfs largeenough to reproduce the SN Ia rate would contribute significantly to theionizing UV radiation expected from the stellar population. For mean stellarages < ~5 Gyr, single degenerate progenitors would dominate the ionizingbackground produced by stars, increasing the continuum beyond the HeII-ionizing limit more than ten-fold. This opens a new avenue for constrainingthe progenitors of SNe Ia, through consideration of the spatially extendedlow-ionization emission-line regions now found in many early-type galaxies.Modelling the expected emission, we show that one can constrain thecontribution of the single degenerate channel to the SN Ia rate in E/S0galaxies from upper limits on the luminosity of He II recombination lines inthe optical and FUV. We discuss future directions, as well as possibleimplications for the evolution of SNe Ia in old stellar populations.

He II recombination lines as a test of the nature of SN Ia progenitors in elliptical galaxies