In principle it is possible to predict the main astrophysical sources for a given nuclide in the solar system by considering the fraction of the yield contributed to the ISM by each of the sites mention in Iliadis. You would need to know (i) how many stars of a given mass and metallicity there are (since stellar evolution depends on both parameters), (ii) the efficiency of various nucleosynthetic processes in each star, (iii) the fraction of the expelled matter (via explosion or stellar wind), and so on.
A large number of nuclides originate in massive stars, and many predicted abundances depend strongly on the mass cut dividing the material that is ejected in the type II supernova explosion from material that falls back onto the remnant neutron star or black hole.
There are large uncertainties on these estimates, but the overall picture regarding the origin of the nuclides in the solar system seems well established.
A = 1-40
The origins of light nuclides with A less than 40 is shown in the table below. Only the dominant sources are listed for each species, and uncertain assignments are placed in square parantheses. An ’x’ denotes explosive burning.
The A=20-40 region are made in massive stars during various phases of their evolution, either in hydrostatic carbon burnin, explosive carbon, neon or oxygen burning, or during the weak s-process (hydrostatic helium burning).