Gamma-Ray Emission of 60 Fe and 26 Al Radioactivity in Our Galaxy

Abstract

The isotopes 60 Fe and 26 Al originate from massive stars and their supernovae, reflecting ongoing nucleosynthesis in the Galaxy. We studied the gamma-ray emission from these isotopes at characteristic energies 1173, 1332, and 1809 keV with over 15 yr of SPI data, finding a line flux in 60 Fe combined lines of and the Al line flux of above the background and continuum emission for the whole sky. Based on the exponential disk grid maps, we characterize the emission extent of 26 Al to find scale parameters and kpc; however, the 60 Fe lines are too weak to spatially constrain the emission. Based on a point-source model test across the Galactic plane, the 60 Fe emission would not be consistent with a single strong point source in the Galactic center or somewhere else, providing a hint of a diffuse nature. We carried out comparisons of emission morphology maps using different candidate source tracers for both 26 Al and 60 Fe emissions and suggest that the 60 Fe emission is more likely to be concentrated toward the Galactic plane. We determine the 60 Fe/ 26 Al γ -ray flux ratio at 18.4% ± 4.2% when using a parameterized spatial morphology model. Across the range of plausible morphologies, it appears possible that 26 Al and 60 Fe are distributed differently in the Galaxy. Using the best-fitting maps for each of the elements, we constrain flux ratios in the range 0.2–0.4. We discuss the implications for massive star models and their nucleosynthesis.