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$\begin{figure} \par\includegraphics[angle=270,width=8.0cm,clip]{0389f01.ps} \end{figure}$ Figure 1: Types of H I shells. The first row shows examples of structures, that can be identified, the second row shows structures connected to the surroundings or with incomplete walls, which are undetectable by the code.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.5cm,clip]{0389f02a.ps} \includ... ...p]{0389f02e.ps} \includegraphics[width=5.5cm,clip]{0389f02f.ps} } \end{figure}$ Figure 2: H I shells in the LDS corresponding to different types as shown in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.0cm,clip]{0389f03.ps} \end{figure}$ Figure 3: Spectra through the central pixel of H I shell candidates. The upper row shows spectra where the presence of an H I hole is confirmed. The lower row shows spectra where the signature of an H I hole is not clear or not present. Solid lines are observed $T_{{\rm B}}$ spectra, dashed lines are $\Delta T_{{\rm B}}$ spectra, a dotted line shows the background level. Velocity channels in which the H I shell candidate (steps 1 and 2) are detected are plotted by the thick line. Numbers are coordinates of structures (lbv).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=16cm]{0389f04.ps} \end{figure}$ Figure 4: Positions of identified H I shells in the LDS. The cross-hatched region around $l=300^{\circ }$ is a region not accessible to the Dwingeloo telescope.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.0cm]{0389f05.ps} \end{figure}$ Figure 5: Angular dimensions $\Delta b$ against $\Delta l \cos b$ of shells identified in the 2nd Galactic quadrant. The dotted line corresponds to $\Delta b = \Delta l \cos b$ . The upper solid line gives the average values of $\Delta b / \Delta l \cos b$ in $\Delta l \cos b$ bins.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0389f06.ps} \end{figure}$ Figure 6: Radius of the shells $r_{{\rm sh}}$ versus their kinematic distances. The two solid lines give the minimum and maximum $r_{{\rm sh}}$ corresponding to $1.5^\circ /2$ and $45^\circ /2$ at the distance d. Dashed, dotted and dash-dotted lines give the average $r_{{\rm sh}}$ calculated for different models of size distribution of shells given by Eq. (2). The histogram gives the average radius $r_{{\rm sh}}$ of the observed shells in separate distance bins.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0389f07.ps} \end{figure}$ Figure 7: Expansion velocities of identified H I shells in the 2nd Galactic quadrant.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f08.ps} \end{figure}$ Figure 8: Radius of shell vs. expansion velocity for shells in the 2nd quadrant. Lines are analytical solutions after Weaver et al. (1977). Solid lines are lines of constant expansion time (1, 10, 50 Myr), dashed lines are lines of constant L/n (0.01, 0.1, 1, 10 ${\rm SN\ Myr^{-1}/cm^{-3}}$ ). Different symbols denote different energies of shells (according to Chevalier 1974), circles are shells with $E < E_{{\rm SN}}$ , crosses are shells with $E \ge E_{{\rm SN}}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f09.ps} \end{figure}$ Figure 9: An average H I density derived for shells at different positions in the Galaxy. The grey scale is logarithmic - the darkest color corresponds to 0.63 cm^-3, lightest color to 0.01 cm^-3, the white color denotes positions with no information about the density, i.e. without an H I shell.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f10.ps} \end{figure}$ Figure 10: The H I density versus size of the shells $r_{{\rm sh}}$ . Two dashed auxiliary lines are power-laws with indices of -1 and -2.
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In the text

$\begin{figure}\par\includegraphics[angle=270,width=8.5cm,clip]{0389f11.ps} \end{figure}$ Figure 11: The distribution of energy deposited in H I shells. The distribution of all shells (dotted line) and the distribution of shells with size $r_{{\rm sh}} > 0.1$ kpc (solid line). The distribution for the M 31 galaxy (dash-dotted line) is taken from Walter & Brinks (1999); it is scaled to the Milky Way values.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=270,width=7cm]{0389f12a.ps}\hspace*{3mm} \includegraphics[angle=270,width=7cm]{0389f12b.ps} } \end{figure}$ Figure 12: The radial and z-distribution of H I shells. The left panel shows recomputed numbers of shells derived from a DER sample by multiplication with a geometric factor (see the text) at different galactocentric radii and an exponential fit with $\sigma _{{\rm gsh}} = 3$ kpc (solid line). The dashed line gives the numbers from the DER sample (see the text). The right panel is the z-distribution of H I shells. Solid lines show the normalized cumulative number of shells at coordinates z lower than a given value, dashed lines show the normalized energy in these shells. Binned data are observations, lines are exponential profiles with a scale length of 760 pc (solid) and 380 pc (dashed). Corresponding HWHMs are 530 and 270 pc.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm]{0389f13.ps} \end{figure}$ Figure 13: The size distribution of H I shells. The number of shells with radius larger than 100 pc and smaller than a given value of $r_{{\rm sh}}$ vs. the radius $r_{{\rm sh}}$ is plotted, plus a theoretical value for three different power-laws.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f14.ps} \end{figure}$ Figure 14: The 2-D filling factor of H I holes in the $T_{\rm B}(l, b, v)$ datacube for $(l,b) \in (90^{\circ },180^{\circ };-10^{\circ },+10^{\circ })$ (solid line), $(l,b) \in (90^{\circ },180^{\circ }; -5^{\circ },+5^{\circ })$ (dashed line), and $(l,b) \in (90^{\circ },180^{\circ };-20^{\circ },+20^{\circ })$ (dotted line) as a function of the radial velocity.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=0,width=7.5cm]{0389f15a.ps} \inc... ...{0389f15c.ps} \includegraphics[angle=0,width=7.5cm]{0389f15d.ps} } \end{figure}$ Figure A.1: Re-identification of the shell GS 128+01-105 discovered by Heiles (1979) - left column, and a newly discovered shell GS145+02-048 (Table 1) - right column. The upper row shows lb-plots, the bottom row shows bv-diagrams.

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.0cm,clip]{0389f01.ps} \end{figure}$	Figure 1: Types of H I shells. The first row shows examples of structures, that can be identified, the second row shows structures connected to the surroundings or with incomplete walls, which are undetectable by the code.
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$\begin{figure} \par\mbox{\includegraphics[width=5.5cm,clip]{0389f02a.ps} \includ... ...p]{0389f02e.ps} \includegraphics[width=5.5cm,clip]{0389f02f.ps} } \end{figure}$	Figure 2: H I shells in the LDS corresponding to different types as shown in Fig. 1.
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$\begin{figure} \par\includegraphics[angle=270,width=16cm]{0389f04.ps} \end{figure}$	Figure 4: Positions of identified H I shells in the LDS. The cross-hatched region around $l=300^{\circ }$ is a region not accessible to the Dwingeloo telescope.
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$\begin{figure} \par\includegraphics[angle=270,width=8.0cm]{0389f05.ps} \end{figure}$	Figure 5: Angular dimensions $\Delta b$ against $\Delta l \cos b$ of shells identified in the 2nd Galactic quadrant. The dotted line corresponds to $\Delta b = \Delta l \cos b$ . The upper solid line gives the average values of $\Delta b / \Delta l \cos b$ in $\Delta l \cos b$ bins.
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$\begin{figure} \par\includegraphics[angle=270,width=8cm,clip]{0389f07.ps} \end{figure}$	Figure 7: Expansion velocities of identified H I shells in the 2nd Galactic quadrant.
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$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f09.ps} \end{figure}$	Figure 9: An average H I density derived for shells at different positions in the Galaxy. The grey scale is logarithmic - the darkest color corresponds to 0.63 cm^-3, lightest color to 0.01 cm^-3, the white color denotes positions with no information about the density, i.e. without an H I shell.
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$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f10.ps} \end{figure}$	Figure 10: The H I density versus size of the shells $r_{{\rm sh}}$ . Two dashed auxiliary lines are power-laws with indices of -1 and -2.
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$\begin{figure}\par\includegraphics[angle=270,width=8.5cm,clip]{0389f11.ps} \end{figure}$	Figure 11: The distribution of energy deposited in H I shells. The distribution of all shells (dotted line) and the distribution of shells with size $r_{{\rm sh}} > 0.1$ kpc (solid line). The distribution for the M 31 galaxy (dash-dotted line) is taken from Walter & Brinks (1999); it is scaled to the Milky Way values.
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$\begin{figure} \par\includegraphics[angle=270,width=8.5cm]{0389f13.ps} \end{figure}$	Figure 13: The size distribution of H I shells. The number of shells with radius larger than 100 pc and smaller than a given value of $r_{{\rm sh}}$ vs. the radius $r_{{\rm sh}}$ is plotted, plus a theoretical value for three different power-laws.
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$\begin{figure} \par\includegraphics[angle=270,width=8.5cm,clip]{0389f14.ps} \end{figure}$	Figure 14: The 2-D filling factor of H I holes in the $T_{\rm B}(l, b, v)$ datacube for $(l,b) \in (90^{\circ },180^{\circ };-10^{\circ },+10^{\circ })$ (solid line), $(l,b) \in (90^{\circ },180^{\circ }; -5^{\circ },+5^{\circ })$ (dashed line), and $(l,b) \in (90^{\circ },180^{\circ };-20^{\circ },+20^{\circ })$ (dotted line) as a function of the radial velocity.
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