All Figures

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Fg071_f1.eps} \end{figure}$ Figure 1: Model of the free electron density in the galactic plane (Taylor & Cordes 1993), used as ²⁶Al source density distribution. Dotted lines represent $-60\hbox {$^\circ $ }$ , $-30\hbox {$^\circ $ }$ , $-4\hbox {$^\circ $ }$ , 0 $^\circ$ , 4 $^\circ$ , 30 $^\circ$ and 60 $^\circ$ galactic longitude. Hatched areas illustrate the eastern/western parts of the inner galactic region.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fg071_f2.eps} \end{figure}$ Figure 2: ²⁶Al line intensity as a function of Galactic longitude and gamma-ray photon energy, with the source longitude profile superimposed.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{Fg071_f3.eps} \end{figure}$ Figure 3: Spectrum of the inner galaxy ( $l \in [-30\hbox {$^\circ $ }, 30\hbox {$^\circ $ }]$ . The full line is the source spectrum, the dotted line the best-fitting Gaussian, and the dashed line results from a convolution with a 2.8 keV FWHM Gaussian adopted for instrumental resolution of the measuring detector. $b \in [-5\hbox {$^\circ $ }, 5\hbox {$^\circ $ }]$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{Fg071_f4.eps} \end{figure}$ Figure 4: Illustrations of lines from different Galactic regions: The histograms (dotted/dashed lines) show the spectra of the eastern/western part of the inner galactic region (i.e. $\pm 5\hbox {$^\circ $ }$ in latitude, $\pm [4\hbox {$^\circ $ }{-}30\hbox {$^\circ $ }]$ in longitude) Energy-resolution limited spectra (obtained by convolving with 2.8 keV FWHM Gaussians) are shown as dash-dotted/long-dashed lines.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Fg071_f1.eps} \end{figure}$	Figure 1: Model of the free electron density in the galactic plane (Taylor & Cordes 1993), used as ²⁶Al source density distribution. Dotted lines represent $-60\hbox {$^\circ $ }$ , $-30\hbox {$^\circ $ }$ , $-4\hbox {$^\circ $ }$ , 0 $^\circ$ , 4 $^\circ$ , 30 $^\circ$ and 60 $^\circ$ galactic longitude. Hatched areas illustrate the eastern/western parts of the inner galactic region.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fg071_f2.eps} \end{figure}$	Figure 2: ²⁶Al line intensity as a function of Galactic longitude and gamma-ray photon energy, with the source longitude profile superimposed.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{Fg071_f3.eps} \end{figure}$	Figure 3: Spectrum of the inner galaxy ( $l \in [-30\hbox {$^\circ $ }, 30\hbox {$^\circ $ }]$ . The full line is the source spectrum, the dotted line the best-fitting Gaussian, and the dashed line results from a convolution with a 2.8 keV FWHM Gaussian adopted for instrumental resolution of the measuring detector. $b \in [-5\hbox {$^\circ $ }, 5\hbox {$^\circ $ }]$ ).
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