Possible origin of the diffuse galactic 6.7 keV iron line, 511 keV annihilation line and of 1809 keV Al26 line

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Abstract
A recent measurement of the distribution of the 6.7 keV iron line flux along the galactic plane gives the opportunity to compare a model with the experimental results. The model is based on the assumption that supernova ejecta are responsible of the excitation of the interstellar iron and so of the 6.7 keV iron line. For that, we used the current supernova remnant distribution and a recent metallicity gradient. The result of the computation is well correlated with the observed iron flux versus the galactic longitude. The supernovae are progenitors of radioactive nuclei, some of which can decay via β+ emission, for example 56Co, 44Ti and 26Al. We assume that the Galactic source of 511 keV observed, in the direction of the Galactic Center are from two different origins: a steady diffuse component, and a variable point source at or near the Galactic Center. We will consider here the diffuse source of 511 keV only. The 1809 keV gamma‐ray line was discovered in 1982 and confirmed. We propose possible distributions for both 511 keV and 1809 keV galactic lines which seem to fit the data quite well.

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