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Table 1:

Main gamma-ray lines expected from the GC region

Line energy
Nuclear FWHMa Fluxa
(MeV) Transition (keV) cm-2 s-1

0.718
10B *0.718 $\rightarrow$ g.s.b 30 $3.4\times10^{-6}$
0.847 56Fe *0.847 $\rightarrow$ g.s. 6 $1.4\times10^{-6}$
  27Al *0.844 $\rightarrow$ g.s.    
1.809 26Mg *1.809 $\rightarrow$ g.s. <2.7c $3.5\times10^{-7}$
  (26Al decay)    
4.44 12C *4.439 $\rightarrow$ g.s. 160 $1.2\times10^{-5}$
  11B *4.445 $\rightarrow$ g.s.    
$\sim $5.2 14N *5.106 $\rightarrow$ g.s. 280 $5.4\times10^{-6}$
  15O *5.181 $\rightarrow$ g.s.    
  15O *5.241 $\rightarrow$ g.s.    
  15N *5.270 $\rightarrow$ g.s.    
  15N *5.299 $\rightarrow$ g.s.    
$\sim $6.2 16O *6.130 $\rightarrow$ g.s. 180d $1.0\times10^{-5}$
  15O *6.176 $\rightarrow$ g.s.    
  15N *6.324 $\rightarrow$ g.s.    

a For $E_{\rm esc}=100$ MeV nucleon-1 and $\sigma =0.05 E_{\rm esc}$(see Eq. (4)). The fluxes are for the region of angular radius $\theta =5^\circ $ (see Fig. 3 for fluxes at 4.44 and $\sim $6.2 MeV calculated for lower values of $\theta$). b Ground state. c Assuming thermal broadening with T<10 keV. d A very narrow line component at 6.129 MeV could arise from excitation of 16O nuclei contained in micrometer-sized grains (see text).


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