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The production of the heavy stable proton-rich isotopes between 74Se and196Hg -- the p nuclides -- is due to the contribution from differentnucleosynthesis processes, activated in different types of stars. Whereas theseprocesses have been subject to various studies, their relative contributions toGalactic Chemical Evolution are still a matter of debate. We investigate forthe first time the nucleosynthesis of p nuclides in GCE by includingmetallicity and progenitor mass-dependent yields of core-collapse supernovae(ccSNe) into a chemical evolution model. We used a grid of metallicities andprogenitor masses from two different sets of stellar yields and followed thecontribution of ccSNe to the Galactic abundances as function of time. Incombination with previous studies on p-nucleus production in thermonuclearsupernovae (SNIa), and using the same GCE description, this allows us tocompare the respective roles of SNeIa and ccSNe in the production of p-nucleiin the Galaxy. The gamma process in ccSN is very efficient for a wide range ofprogenitor masses (13M_sun_- 25M_sun) at solar metallicity. Since it is asecondary process with its efficiency depending on the initial abundance ofheavy elements, its contribution is strongly reduced below solar metallicity.This makes it challenging to explain the inventory of the p nuclides in theSolar System by the contribution from ccSNe alone. In particular, we find thatccSNe contribute less than 10% of the solar p nuclide abundances, with only afew exceptions. Due to the uncertain contribution from other nucleosynthesissites in ccSNe, such as neutrino winds or $\alpha$-rich freeze out, we concludethat the light p-nuclides 74$Se,78$Kr, 84Sr, and 92Mo may either still becompletely or only partially produced in ccSNe.

Role of core-collapse supernovae in explaining Solar System abundances of p nuclides