All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aah4145f1.eps} \end{figure}$ Figure 1: Map of the Galactic Center field, reconstructed from the RXTE/PCA scans in 1999-2000. Circles represent regions where the contribution of point sources dominates (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4145f2.ps}\end{figure}$ Figure 2: Exposure map of the Galactic scan observations during period March 1999-May 2000 (high voltage Epoch4).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4145f3.ps}\end{figure}$ Figure 3: Distribution of the 3-20 keV intensity of the Galactic ridge emission with longitude. The regions over which the brightness is averaged are 2 < |b| < 4 for the upper plot, and 4 <|b|<10 for the lower plot.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{h4145f4a.ps}\hspace*{1.1cm} \includegraphics[width=8cm,clip]{h4145f4b.ps}\end{figure}$ Figure 4: The profile of the brightness of the Galactic ridge emission with latitude in three energy bands constructed using March 1999-May 2000 data (Epoch4, left) and May 2000-July 2001 data (Epoch5, right). The solid line shows the convolution of the exponential model with the response of the RXTE/PCA collimator. There is a clear indication of the presence of an additional component within $\vert b\vert<1{-}2^\circ$ . Taking into account the observed spectral shape, the 1 cnts/s/PCU corresponds approximately to $1.2\times 10^{-11}$ erg/s/cm² in the 3-20 keV energy band, approximately to $2.3\times 10^{-11}$ erg/s/cm² in the 10-20 keV energy band and ${\sim } 10^{-10}$ erg/s/cm² in the 20-30 keV energy band. Here and below the bars represent $1-\sigma$ errors.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{h4145f5.ps} \end{figure}$ Figure 5: PCA spectrum of the Galactic ridge emission collected over $\vert b\vert>2^\circ$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{h4145f6.ps}\end{figure}$ Figure 6: Latitude distribution of parameters of spectral approximation of the Galactic ridge emission (combined data of Epoch4 and 5).
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{h4145f7.ps}\end{figure}$ Figure 7: Distribution of observed brightness of the Galactic ridge emission (crosses and open circles), the CO line intensity (short dashed line) and number of supernova remnants within 1 deg strips along the galactic plane within the field of scan of RXTE. The Y-axis has units cnts/s/PCU for the observed Galactic ridge X-ray emission (3-20 keV), K km s^-1 deg for CO line.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{aah4145f1.eps} \end{figure}$	Figure 1: Map of the Galactic Center field, reconstructed from the RXTE/PCA scans in 1999-2000. Circles represent regions where the contribution of point sources dominates (see text).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{h4145f2.ps}\end{figure}$	Figure 2: Exposure map of the Galactic scan observations during period March 1999-May 2000 (high voltage Epoch4).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{h4145f3.ps}\end{figure}$	Figure 3: Distribution of the 3-20 keV intensity of the Galactic ridge emission with longitude. The regions over which the brightness is averaged are 2 < \|b\| < 4 for the upper plot, and 4 <\|b\|<10 for the lower plot.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{h4145f5.ps} \end{figure}$	Figure 5: PCA spectrum of the Galactic ridge emission collected over $\vert b\vert>2^\circ$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{h4145f6.ps}\end{figure}$	Figure 6: Latitude distribution of parameters of spectral approximation of the Galactic ridge emission (combined data of Epoch4 and 5).
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{h4145f7.ps}\end{figure}$	Figure 7: Distribution of observed brightness of the Galactic ridge emission (crosses and open circles), the CO line intensity (short dashed line) and number of supernova remnants within 1 deg strips along the galactic plane within the field of scan of RXTE. The Y-axis has units cnts/s/PCU for the observed Galactic ridge X-ray emission (3-20 keV), K km s^-1 deg for CO line.
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