All Figures

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=8.7cm]{9240f01a.eps} \... ...0f01g.eps} \includegraphics[angle=-90,width=8.7cm]{9240f01h.eps} } \end{figure}$ Figure 1: Derived volume density distribution at R = 10, 12.5, 15, 17.5, 20, 22.5, 25, 30 kpc ( top to bottom). Locations affected by local emission with $\vert v_{\rm lsr}\vert < 10$ km s^-1 are flagged dark. We display densities n < 0.5 cm^-3. A logarithmic transfer function was chosen to emphasize low densities. The thin white lines indicate the average flaring at a $3 \sigma$ level and enclose the warped disk. The thick white lines indicate latitudes $\vert b\vert = 30 \hbox {$^\circ $ }\pm 0.5 \hbox {$^\circ $ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9240f02.eps}\end{figure}$ Figure 2: Milky Way velocity field at mid-plane for the mass distribution derived by Kalberla et al. (2007). The isophotes indicate velocities -190 $< v_{\rm lsr} < 190$ km s^-1 in steps of 10 km s^-1. The thick lines are at $\vert v_{\rm lsr}\vert = 50$ , 100 and 150 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f03.eps} \end{figure}$ Figure 3: Derived mean surface densities of the H I gas perpendicular to the disk (red). The dotted blue line gives $N_{\rm H}(R)$ in the northern, the dotted green line in the southern part of the Milky Way. The dashed black line reproduces the distribution published by Binney & Merrifield (1998, BM98) in Fig. 9.19. Wolfire et al. (2003) (thick black line) used partial data from Wouterloot et al. (1990, W90).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f04a.eps} \includegraphics[angle=-90,width=9cm,clip]{9240f04b.eps} \end{figure}$ Figure 4: Systematic variations of the average H I surface density distribution determined in $20\hbox {$^\circ $ }$ wide sectors for $30\hbox {$^\circ $ }< \phi < 150\hbox {$^\circ $ }$ (north) and $210\hbox {$^\circ $ }< \phi < 330\hbox {$^\circ $ }$ (south). For comparison with Fig. 3 the fit (black) and total averages for north and south (blue and green respectively) are given.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f05.eps} \end{figure}$ Figure 5: Derived average mid-plane volume density of the H I gas (red). The dotted blue line gives n(R) in the north ( $30\hbox {$^\circ $ }< \phi < 150\hbox {$^\circ $ }$ ), the dotted green line in the southern part of the Milky Way ( $210\hbox {$^\circ $ }< \phi < 330\hbox {$^\circ $ }$ ). The black line represents an exponential fit with a radial scale length of 3.15 kpc.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f06a.eps} \includegraphics[angle=-90,width=9cm,clip]{9240f06b.eps} \end{figure}$ Figure 6: Systematic variations of the average H I volume density distribution determined in $20\hbox {$^\circ $ }$ wide sectors for $30\hbox {$^\circ $ }< \phi < 150\hbox {$^\circ $ }$ (north) and $210\hbox {$^\circ $ }< \phi < 330\hbox {$^\circ $ }$ (south). For comparison with Fig. 5 the fit (black) and total averages for north and south (blue and green respectively) are given.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f07.eps} \end{figure}$ Figure 7: Derived mean flaring of the H I gas (red). The dotted blue line holds for the northern, the dotted green line for the southern part of the Milky Way. For comparison an exponential fit for R < 35 kpc is plotted (long dashed), also the flaring according to the model by Kalberla et al. (2007).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm]{9240f08.eps} \end{figure}$ Figure 8: Average mid-plane volume densities for $20\hbox {$^\circ $ }$ wide radial sectors in the Milky Way. For comparison the fitted distribution of the HVD gas is given (red solid lines).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm]{9240f09.eps}\end{figure}$ Figure 9: Average mid-plane surface densities for $20\hbox {$^\circ $ }$ wide radial sectors in the Milky Way. For comparison the fitted distribution of the HVD gas is given (red solid lines).
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=9cm]{9240f10a.eps} \in... ...240f10c.eps} \includegraphics[angle=-90,width=9cm]{9240f10d.eps} } \end{figure}$ Figure 10: Position-velocity diagrams for the Milky Way H I brightness termerature at latitudes -10 $^\circ$ , -5 $^\circ$ ( left) and 10 $^\circ$ , 5 $^\circ$ ( right). The white isophotes display HVD emission from the model (10% to 90% in steps of 10%), the red isophote marks an average disk emission of 100 mK. A logarithmic transfer function was used for $T_{\rm B} <30$ K.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{9240f11.eps} \end{figure}$ Figure 11: Asymmetry of mid-plane volume densities, surface densities, and scale heights characterized by their south/north ratios S/N. In addition the warp scalloping power in % is given.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f12.eps}\end{figure}$ Figure 12: Fraction of extra-planar gas observed outside the disk for - 15 < z < 20 kpc.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm]{9240f13.eps} \end{figure}$ Figure 13: Gravitational acceleration k_z at $R_{\hbox{$\odot$ }}~$ = 8.5 kpc, (solid red line) and gas pressure balance $\rho ^{-1} {\rm d}p/{\rm d}z$ (dotted green). For comparison we plot k_z according to Kuijken & Gilmore (1989) (dashed, blue) and Dehnen & Binney (1998, Galactic Model 2). The lower dotted line gives $\rho ^{-1} {\rm d}p/{\rm d}z$ for a multi-phase gas without halo components.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm]{9240f14.eps}\end{figure}$ Figure 14: Average H I emission to logarithmic scale for latitudes $b > 20\hbox {$^\circ $ }$ . The data are from the Bell Labs telescope (thick black line) and from the LAB survey (red). The step function shows the weights for each channel in dB. The thin red dotted line represents broad Gaussian components indicating baseline problems.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm]{9240f15.eps}\end{figure}$ Figure 15: Average H I emission in logarithmic scale for latitudes $\vert b\vert > 20\hbox {$^\circ $ }$ from the LAB survey. The red line is for the north polar cap, the dashed green line for the southern part. The thin dotted black line represents the model according to Table 1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=9cm]{9240f16.eps} \end{figure}$ Figure 16: Position velocity diagram along the major axis, observable for a galaxy like the Milky Way with an inclination of $80\hbox {$^\circ $ }$ . The thin contours represent normalized column densities in steps of 2 dB; the lowest contour is at -30 dB. The green dashed lines gives the rotation curve at z =0 kpc, the solid red line the mean rotation for the H I in the halo.
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In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9240f02.eps}\end{figure}$	Figure 2: Milky Way velocity field at mid-plane for the mass distribution derived by Kalberla et al. (2007). The isophotes indicate velocities -190 $< v_{\rm lsr} < 190$ km s^-1 in steps of 10 km s^-1. The thick lines are at $\vert v_{\rm lsr}\vert = 50$ , 100 and 150 km s^-1.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f04a.eps} \includegraphics[angle=-90,width=9cm,clip]{9240f04b.eps} \end{figure}$	Figure 4: Systematic variations of the average H I surface density distribution determined in $20\hbox {$^\circ $ }$ wide sectors for $30\hbox {$^\circ $ }< \phi < 150\hbox {$^\circ $ }$ (north) and $210\hbox {$^\circ $ }< \phi < 330\hbox {$^\circ $ }$ (south). For comparison with Fig. 3 the fit (black) and total averages for north and south (blue and green respectively) are given.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f05.eps} \end{figure}$	Figure 5: Derived average mid-plane volume density of the H I gas (red). The dotted blue line gives n(R) in the north ( $30\hbox {$^\circ $ }< \phi < 150\hbox {$^\circ $ }$ ), the dotted green line in the southern part of the Milky Way ( $210\hbox {$^\circ $ }< \phi < 330\hbox {$^\circ $ }$ ). The black line represents an exponential fit with a radial scale length of 3.15 kpc.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f06a.eps} \includegraphics[angle=-90,width=9cm,clip]{9240f06b.eps} \end{figure}$	Figure 6: Systematic variations of the average H I volume density distribution determined in $20\hbox {$^\circ $ }$ wide sectors for $30\hbox {$^\circ $ }< \phi < 150\hbox {$^\circ $ }$ (north) and $210\hbox {$^\circ $ }< \phi < 330\hbox {$^\circ $ }$ (south). For comparison with Fig. 5 the fit (black) and total averages for north and south (blue and green respectively) are given.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f07.eps} \end{figure}$	Figure 7: Derived mean flaring of the H I gas (red). The dotted blue line holds for the northern, the dotted green line for the southern part of the Milky Way. For comparison an exponential fit for R < 35 kpc is plotted (long dashed), also the flaring according to the model by Kalberla et al. (2007).
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm]{9240f08.eps} \end{figure}$	Figure 8: Average mid-plane volume densities for $20\hbox {$^\circ $ }$ wide radial sectors in the Milky Way. For comparison the fitted distribution of the HVD gas is given (red solid lines).
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm]{9240f09.eps}\end{figure}$	Figure 9: Average mid-plane surface densities for $20\hbox {$^\circ $ }$ wide radial sectors in the Milky Way. For comparison the fitted distribution of the HVD gas is given (red solid lines).
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$\begin{figure} \par\mbox{\includegraphics[angle=-90,width=9cm]{9240f10a.eps} \in... ...240f10c.eps} \includegraphics[angle=-90,width=9cm]{9240f10d.eps} } \end{figure}$	Figure 10: Position-velocity diagrams for the Milky Way H I brightness termerature at latitudes -10 $^\circ$ , -5 $^\circ$ ( left) and 10 $^\circ$ , 5 $^\circ$ ( right). The white isophotes display HVD emission from the model (10% to 90% in steps of 10%), the red isophote marks an average disk emission of 100 mK. A logarithmic transfer function was used for $T_{\rm B} <30$ K.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{9240f11.eps} \end{figure}$	Figure 11: Asymmetry of mid-plane volume densities, surface densities, and scale heights characterized by their south/north ratios S/N. In addition the warp scalloping power in % is given.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm,clip]{9240f12.eps}\end{figure}$	Figure 12: Fraction of extra-planar gas observed outside the disk for - 15 < z < 20 kpc.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm]{9240f14.eps}\end{figure}$	Figure 14: Average H I emission to logarithmic scale for latitudes $b > 20\hbox {$^\circ $ }$ . The data are from the Bell Labs telescope (thick black line) and from the LAB survey (red). The step function shows the weights for each channel in dB. The thin red dotted line represents broad Gaussian components indicating baseline problems.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm]{9240f15.eps}\end{figure}$	Figure 15: Average H I emission in logarithmic scale for latitudes $\vert b\vert > 20\hbox {$^\circ $ }$ from the LAB survey. The red line is for the north polar cap, the dashed green line for the southern part. The thin dotted black line represents the model according to Table 1.
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$\begin{figure} \par\includegraphics[angle=-90,width=9cm]{9240f16.eps} \end{figure}$	Figure 16: Position velocity diagram along the major axis, observable for a galaxy like the Milky Way with an inclination of $80\hbox {$^\circ $ }$ . The thin contours represent normalized column densities in steps of 2 dB; the lowest contour is at -30 dB. The green dashed lines gives the rotation curve at z =0 kpc, the solid red line the mean rotation for the H I in the halo.
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