$\begin{figure} \par\includegraphics[height=4.7cm,width=8.6cm,clip]{Gd021_f1.ps} \end{figure}$ Figure 1: CR source density as function of Galactocentric radius R. Dotted: as used in Strong et al. (2000), solid line: based on pulsars (Lorimer 2004) as used in this work, vertical bars: SNR data points from Case & Bhattacharya (1998). Distributions are normalized at R = 8.5 kpc.
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In the text

$\begin{figure} \par\includegraphics[height=4.7cm,width=8.8cm,clip]{Gd021_f2.ps} \end{figure}$ Figure 2: $X_{\rm CO}$ as function of R. Dotted horizontal line, black: as used in Strong et al. (2000); Strong & Mattox (1996); solid line, black: as used for $\gamma$ -raysthis work; dashed, dark blue: from Sodroski et al. (1995); dash-dot, red: using metallicity gradient as described in the text, $X_{\rm CO}$ $\propto$ Z^-2.5 (Israel 2000), two lines for [O/H] = 0.04 and 0.07 dex/kpc; dash-dot-dot,light blue: using $X_{\rm CO}$ $\propto$ Z^-1.0 (Boselli et al. 2002) and [O/H] = 0.07 dex/kpc. The values using metallicity are normalized approximately to those from the $\gamma$ -ray.
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In the text

$\begin{figure} \par\includegraphics[height=7cm,width=8.7cm,clip]{Gd021_f3.ps} \end{figure}$ Figure 3: Longitude profile of $\gamma$ -rays1000-2000 MeV, averaged over $\vert b\vert<5.5^\circ$ . Vertical bars: EGRET data; lines are model components convolved with the EGRET point-spread function: green: inverse Compton emission, red: $\pi ^0$ -decay, light blue: bremsstrahlung, dark blue: total.
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In the text

$\begin{figure} \par\includegraphics[height=7cm,width=8.55cm,clip]{Gd021_f4.ps} \end{figure}$ Figure 4: Latitude profile of $\gamma$ -rays1000-2000 MeV, averaged over $330^\circ <l<30^\circ$ . Data and curves as in Fig. 3. The extragalactic background is shown as a black horizontal line.
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In the text

$\begin{figure} \par\includegraphics[height=7cm,width=8.5cm,clip]{Gd021_f5.ps} \end{figure}$ Figure 5: Spectrum of inner Galaxy, $330^\circ <l<30^\circ , \vert b\vert<5.5^\circ$ . Vertical bars: EGRET data (red), COMPTEL data (green). Curves: predicted intensities; inverse Compton (green), $\pi ^0$ -decay (red), bremsstrahlung (light blue), extragalactic background (black), total (dark blue).
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In the text

$\begin{figure} \par\includegraphics[height=4.7cm,width=8.6cm,clip]{Gd021_f1.ps} \end{figure}$	Figure 1: CR source density as function of Galactocentric radius R. Dotted: as used in Strong et al. (2000), solid line: based on pulsars (Lorimer 2004) as used in this work, vertical bars: SNR data points from Case & Bhattacharya (1998). Distributions are normalized at R = 8.5 kpc.
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$\begin{figure} \par\includegraphics[height=7cm,width=8.7cm,clip]{Gd021_f3.ps} \end{figure}$	Figure 3: Longitude profile of $\gamma$ -rays1000-2000 MeV, averaged over $\vert b\vert<5.5^\circ$ . Vertical bars: EGRET data; lines are model components convolved with the EGRET point-spread function: green: inverse Compton emission, red: $\pi ^0$ -decay, light blue: bremsstrahlung, dark blue: total.
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$\begin{figure} \par\includegraphics[height=7cm,width=8.55cm,clip]{Gd021_f4.ps} \end{figure}$	Figure 4: Latitude profile of $\gamma$ -rays1000-2000 MeV, averaged over $330^\circ <l<30^\circ$ . Data and curves as in Fig. 3. The extragalactic background is shown as a black horizontal line.
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$\begin{figure} \par\includegraphics[height=7cm,width=8.5cm,clip]{Gd021_f5.ps} \end{figure}$	Figure 5: Spectrum of inner Galaxy, $330^\circ <l<30^\circ , \vert b\vert<5.5^\circ$ . Vertical bars: EGRET data (red), COMPTEL data (green). Curves: predicted intensities; inverse Compton (green), $\pi ^0$ -decay (red), bremsstrahlung (light blue), extragalactic background (black), total (dark blue).
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