All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3199_f1.ps} \end{figure}$ Figure 1: Mosaic of 2MASS images centered on Sgr A^*. The thick box delineates our region of interest.
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In the text

$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{3199_f2.ps}} \end{figure}$ Figure 2: Slice of the 2MASS images through Sgr A^* parallel to the galactic longitude. Solid line: $K_{\rm S}$ band. Dashed line: H band. Dotted line: J band.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3199_f3.ps} \end{figure}$ Figure 3: Upper panel: a subfield of the original $K_{\rm S}$ band image. Lower panel: same image after subtraction of Lorentzian fits to the point sources. The offsets are given with respect to Sgr A^*.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{3199_f4.ps} \end{figure}$ Figure 4: $K_{\rm S}$ band images of a small subfield $\sim$ 5 pc north-east from Sgr A^*. Left panel: 2MASS image with 3'' effective resolution. Right panel: IRAC2B image with 1'' resolution (Philipp et al. 1999). The coordinates are offsets with respect to Sgr A^*.
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In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{3199_f5.ps}} \end{figure}$ Figure 5: Upper panel: $K_{\rm S}/H$ flux ratio distribution of the point sources as a function of their distance to Sgr A^*. Middle panel: $K_{\rm S}/H$ flux ratio distribution as a function of the $K_{\rm S}$ band flux. Lower panel: theoretical $K_{\rm S}/H$ flux ratio for stars with different effective temperatures. Solid line: no reddening. Dashed line: reddening corresponding to $A_{\rm V}=15$ mag. Dotted line: reddening corresponding to $A_{\rm V}=30$ mag.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3199_f6.ps} \end{figure}$ Figure 6: Radial profile of the blue point sources averaged over ellipsoids with an axis ratio of 1.4:1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3199_f7.ps} \end{figure}$ Figure 7: Solid line: radial profile of the red point sources averaged over ellipsoids with an axis ratio of 1.4:1. Dashed line: slice parallel to the galactic longitude through Sgr A^* through the $K_{\rm S}$ image where all point sources (red and blue) are subtracted.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3199_f8.ps} \end{figure}$ Figure 8: Sketch of the inner 30 pc of the Galaxy. The central black dot represents the He I star cluster surrounded by the Minispiral and the CND (where only the high velocity lobes are shown). The 20 and 50 km s^-1 giant molecular clouds are located at negative latitudes. Capital letters indicate structures discussed in the text. 1 pc corresponds to 24''.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.1cm,clip]{3199_f9a.ps}\pa... ...e*{5mm} \includegraphics[angle=-90,width=15.1cm,clip]{3199_f9b.ps} \end{figure}$ Figure 9: $K_{\rm S}$ band image of the Galactic Center region. Upper panel: only the blue point sources are subtracted. Lower panel: all distinguishable point sources are subtracted.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3199_f10.ps} \end{figure}$ Figure 10: Slices of the model intensities along the galactic longitude and latitude through Sgr A^* together with slices of the $K_{\rm S}$ data. Dotted line: Eq. (2)/(4) a=0, z₀=-50 pc. Dashed line: Eq. (2)/(4) a=0, z₀=-100 pc. Dash-dotted line: Eq. (3)/(4) a=0. 1 pc corresponds to 24''.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{3199_f11.ps} \end{figure}$ Figure 11: LOS distance z as a function of the ratio I_z/I₀ for 3 different projected distances: solid line: (2 pc, 0.5 pc), dashed line: (5 pc, 5 pc), dot-dashed line: (10 pc, 5 pc).
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3199_f12.ps} \end{figure}$ Figure 12: Reconstruction of the LOS distances for a slice at $\Delta b = -70''$ parallel to the galactic longitude using Eq. (2). Solid line: a=150 $\mu$ Jy/arcsec² and z₀=-50 pc. Dotted line: a=0 z₀=-50 pc. Dashed line: a=150 $\mu$ Jy/arcsec² and z₀=-100 pc. Dot-dashed line: a=0 z₀=-100 pc. Negative distances are in front of Sgr A^*.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3199_f13.ps} \end{figure}$ Figure 13: Reconstruction of the LOS distances for a slice at $\Delta b = -70''$ parallel to the galactic longitude using Eq. (3). Solid line: a=0 and z₀=-150 pc. Dashed line: a=150 $\mu$ Jy/arcsec² and z₀=-150 pc. Negative distances are in front of Sgr A^*.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=15.4cm,clip]{3199_f14a.ps}\p... ...*{6mm} \includegraphics[angle=-90,width=15.4cm,clip]{3199_f14b.ps} \end{figure}$ Figure 14: Map of the reconstructed LOS distances for the 2MASS $K_{\rm S}$ images. Upper panel: all blue point sources are subtracted. Lower panel: all point sources (blue and red) are subtracted.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3199_f15.ps} \end{figure}$ Figure 15: Contours: IRAM 30 m 1.2 mm observations of Zylka et al. (1998). Colors: LOS distance distribution filtered with a median filter of 11 pixels.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3199_f16.ps} \end{figure}$ Figure 16: Contours: IRAM 30 m CS(2-1) line observations (Güsten et al., in prep.) integrated over the whole velocity range. Colors: LOS distance distribution filtered with a median filter of 11 pixels.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3199_f17.ps} \end{figure}$ Figure 17: Contours: IRAM 30 m CS(2-1) line observations (Güsten et al., in prep.). The integrated flux over channels -140 km s ^-1 < v < -31 km s^-1 and 71 km s ^-1 < v < 115 km s^-1, i.e. the CND, are shown. Colors: LOS distance distribution filtered with a median filter of 11 pixels.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3199_f1.ps} \end{figure}$	Figure 1: Mosaic of 2MASS images centered on Sgr A^*. The thick box delineates our region of interest.
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$\begin{figure} \par\resizebox{8.3cm}{!}{\includegraphics[clip]{3199_f2.ps}} \end{figure}$	Figure 2: Slice of the 2MASS images through Sgr A^* parallel to the galactic longitude. Solid line: $K_{\rm S}$ band. Dashed line: H band. Dotted line: J band.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3199_f3.ps} \end{figure}$	Figure 3: Upper panel: a subfield of the original $K_{\rm S}$ band image. Lower panel: same image after subtraction of Lorentzian fits to the point sources. The offsets are given with respect to Sgr A^*.
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$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{3199_f4.ps} \end{figure}$	Figure 4: $K_{\rm S}$ band images of a small subfield $\sim$ 5 pc north-east from Sgr A^. Left panel: 2MASS image with 3'' effective resolution. Right panel: IRAC2B image with 1'' resolution (Philipp et al. 1999). The coordinates are offsets with respect to Sgr A^.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3199_f6.ps} \end{figure}$	Figure 6: Radial profile of the blue point sources averaged over ellipsoids with an axis ratio of 1.4:1.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3199_f7.ps} \end{figure}$	Figure 7: Solid line: radial profile of the red point sources averaged over ellipsoids with an axis ratio of 1.4:1. Dashed line: slice parallel to the galactic longitude through Sgr A^* through the $K_{\rm S}$ image where all point sources (red and blue) are subtracted.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3199_f8.ps} \end{figure}$	Figure 8: Sketch of the inner 30 pc of the Galaxy. The central black dot represents the He I star cluster surrounded by the Minispiral and the CND (where only the high velocity lobes are shown). The 20 and 50 km s^-1 giant molecular clouds are located at negative latitudes. Capital letters indicate structures discussed in the text. 1 pc corresponds to 24''.
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$\begin{figure} \par\includegraphics[angle=-90,width=15.1cm,clip]{3199_f9a.ps}\pa... ...e*{5mm} \includegraphics[angle=-90,width=15.1cm,clip]{3199_f9b.ps} \end{figure}$	Figure 9: $K_{\rm S}$ band image of the Galactic Center region. Upper panel: only the blue point sources are subtracted. Lower panel: all distinguishable point sources are subtracted.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3199_f10.ps} \end{figure}$	Figure 10: Slices of the model intensities along the galactic longitude and latitude through Sgr A^* together with slices of the $K_{\rm S}$ data. Dotted line: Eq. (2)/(4) a=0, z₀=-50 pc. Dashed line: Eq. (2)/(4) a=0, z₀=-100 pc. Dash-dotted line: Eq. (3)/(4) a=0. 1 pc corresponds to 24''.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{3199_f11.ps} \end{figure}$	Figure 11: LOS distance z as a function of the ratio I_z/I₀ for 3 different projected distances: solid line: (2 pc, 0.5 pc), dashed line: (5 pc, 5 pc), dot-dashed line: (10 pc, 5 pc).
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{3199_f12.ps} \end{figure}$	Figure 12: Reconstruction of the LOS distances for a slice at $\Delta b = -70''$ parallel to the galactic longitude using Eq. (2). Solid line: a=150 $\mu$ Jy/arcsec² and z₀=-50 pc. Dotted line: a=0 z₀=-50 pc. Dashed line: a=150 $\mu$ Jy/arcsec² and z₀=-100 pc. Dot-dashed line: a=0 z₀=-100 pc. Negative distances are in front of Sgr A^*.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3199_f13.ps} \end{figure}$	Figure 13: Reconstruction of the LOS distances for a slice at $\Delta b = -70''$ parallel to the galactic longitude using Eq. (3). Solid line: a=0 and z₀=-150 pc. Dashed line: a=150 $\mu$ Jy/arcsec² and z₀=-150 pc. Negative distances are in front of Sgr A^*.
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$\begin{figure} \par\includegraphics[angle=-90,width=15.4cm,clip]{3199_f14a.ps}\p... ...*{6mm} \includegraphics[angle=-90,width=15.4cm,clip]{3199_f14b.ps} \end{figure}$	Figure 14: Map of the reconstructed LOS distances for the 2MASS $K_{\rm S}$ images. Upper panel: all blue point sources are subtracted. Lower panel: all point sources (blue and red) are subtracted.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3199_f15.ps} \end{figure}$	Figure 15: Contours: IRAM 30 m 1.2 mm observations of Zylka et al. (1998). Colors: LOS distance distribution filtered with a median filter of 11 pixels.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3199_f16.ps} \end{figure}$	Figure 16: Contours: IRAM 30 m CS(2-1) line observations (Güsten et al., in prep.) integrated over the whole velocity range. Colors: LOS distance distribution filtered with a median filter of 11 pixels.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{3199_f17.ps} \end{figure}$	Figure 17: Contours: IRAM 30 m CS(2-1) line observations (Güsten et al., in prep.). The integrated flux over channels -140 km s ^-1 < v < -31 km s^-1 and 71 km s ^-1 < v < 115 km s^-1, i.e. the CND, are shown. Colors: LOS distance distribution filtered with a median filter of 11 pixels.
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