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Gamma-ray line emission from radioactive decay of 60Fe provides constraintson nucleosynthesis in massive stars and supernovae. We detect the gamma-raylines from 60Fe decay at 1173 and 1333 keV using three years of data from thespectrometer SPI on board INTEGRAL. The average flux per line is (4.4 \pm 0.9)\times 10^{-5} ph cm^{-2} s^{-1} rad^{-1} for the inner Galaxy region. Derivingthe Galactic 26Al gamma-ray line flux with using the same set of observationsand analysis method, we determine the flux ratio of 60Fe/26Al gamma-rays as0.15 \pm 0.05. We discuss the implications of these results for the widely-heldhypothesis that 60Fe is synthesized in core-collapse supernovae, and also forthe closely-related question of the precise origin of 26Al in massive stars.

60Fe and Massive Stars