Fig. 9


Properties of our preferred model. The top-left plot shows the adopted 26Al source distribution in the plane of the Milky Way as seen from above. Also indicated is the position of the Sun (8 kpc from the Galactic centre), the location of the bar (dashed), and several longitudinal directions of interest. The colour indicates the 26Al density (yellow: highest, black: lowest). The other plots show quantities derived from this source distribution as a function of Galactic longitude as solid black lines (top right: received flux in arbitrary units, bottom left: velocity centroid shift, bottom right: velocity width). Overplotted are the observed data points with error bars showing one standard deviation, and upper limits of three standard deviations in the case of the velocity width. The flux excess at l = −24° may be due to foreground emission from the Sco-Cen association (Diehl et al. 2010) leaking from higher latitudes into our ROI bin. The observational limits on the velocity width are not constraining and are compatible with expectations (see Sect. 2.2).

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