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Gamma-ray line emission from radioactive decay of 60Fe provides constraintson nucleosynthesis in massive stars and supernovae. The spectrometer SPI onboard INTEGRAL has accumulated nearly three years of data on gamma-ray emissionfrom the Galactic plane. We have analyzed these data with suitableinstrumental-background models and sky distributions to produce high-resolutionspectra of Galactic emission. We detect the gamma-ray lines from 60Fe decay at1173 and 1333 keV, obtaining an improvement over our earlier measurement ofboth lines with now 4.9 sigma significance for the combination of the twolines. 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. Deriving the Galactic 26Algamma-ray line flux with using the same set of observations and analysismethod, we determine the flux ratio of 60Fe/26Al gamma-rays as 0.148 \pm 0.06.The current theoretical predictions are still consistent with our result.

SPI observations of the diffuse 60Fe emission in the Galaxy