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In our quest to identify the progenitors of Type Ia supernovae (SNe Ia), wefirst update the nucleosynthesis yields both for near-Chandrasekhar (Ch) andsub-Ch mass white dwarfs (WDs), for a wide range of metallicity, with ourtwo-dimensional hydrodynamical code and the latest nuclear reaction rates. Wethen include the yields in our galactic chemical evolution code to predict theevolution of elemental abundances in the solar neighborhood and dwarfspheroidal (dSph) galaxies: Fornax, Sculptor, Sextans, and Carina. In theobservations of the solar neighborhood stars, Mn shows an opposite trend to$\alpha$ elements, showing an increase toward higher metallicities, which isvery well reproduced by deflagration-detonation transition of Ch-mass WDs, butnever by double detonations of sub-Ch-mass WDs alone. The problem of Ch-massSNe Ia was the Ni over-production at high metallicities. However, we found thatNi yields of Ch-mass SNe Ia are much lower with the solar-scaled initialcomposition than in previous works, which keeps the predicted Ni abundancewithin the observational scatter. From the evolutionary trends of elementalabundances in the solar neighborhood, we conclude that the contribution ofsub-Ch-mass SNe Ia in chemical enrichment is up to 25\%. In dSph galaxies,however, larger enrichment from sub-Ch-mass SNe Ia than in the solarneighborhood may be required, which causes a decrease in [(Mg, Cr, Mn, Ni)/Fe]at lower metallicities. The observed high [Mn/Fe] ratios in Sculptor and Carinamay also require additional enrichment from pure deflagrations, possibly asType Iax supernovae. Future observations of dSph stars will provide morestringent constraints on the progenitor systems and explosion mechanism of SNeIa.

New Type Ia supernova Yields and the Manganese and Nickel Problems in the Milky Way and Dwarf Spheroidal Galaxies