All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=13.7cm,clip]{1864f01a.eps} \... ...01b.eps} \includegraphics[angle=-90,width=13.7cm,clip]{1864f01c.eps}\end{figure}$ Figure 1: Images of the H I sky contributed by emission in single channels centered near v = -35 km s^-1. Top: H I emission in a single channel, 5 km s^-1 wide, from data in the Bell Labs Survey (Stark et al. 1992). Middle: H I emission in a single channel, 1.3 km s^-1 wide, from data in the first edition of the LDS (Hartmann & Burton 1997). Bottom: H I emission in a single channel, 1.3 km s^-1 wide, from the LAB Survey of the entire Galactic sky, combining the IAR and LDS material and incorporating a refined determination of the stray-radiation properties. The intensity scale is logarithmic, emphasizing low level emission ( -0.21 < T < 50 K), and is the same in all maps of Figs. 1 and 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13.7cm,clip]{1864f02a.eps} \... ...02b.eps} \includegraphics[angle=-90,width=13.7cm,clip]{1864f02c.eps}\end{figure}$ Figure 2: Images of the H I sky contributed by emission in single channels centered near v = +35 km s^-1. Top: H I emission in a single channel, 5 km s^-1 wide, from data in the Bell Labs Survey (Stark et al. 1992). Middle: H I emission in a single channel, 1.3 km s^-1 wide, from data in the first edition of the LDS (Hartmann & Burton 1997). Bottom: H I emission in a single channel, 1.3 km s^-1 wide, from the LAB Survey of the entire Galactic sky, combining the IAR and LDS material and incorporating a refined determination of the stray-radiation properties. The intensity scale is logarithmic, emphasizing low level emission ( -0.21 < T < 50 K), and is the same in all maps of Figs. 1 and 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=13.3cm,clip]{1864f003.eps}\end{figure}$ Figure 3: H I emission integrated over the velocity range -400 < v < +400 km s^-1 in the LAB dataset, shown in an Aitoff projection. The Galactic center is in the middle. The integrated emission ( $0 < N_{\rm H} < 2 \times 10^{22}$ cm^-2, logarithmic scale) yields column densities under the assumption of optical transparency; this assumption may be violated at latitudes within about 10 $^\circ$ of the Galactic equator.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=11.7cm,clip]{1864f004.eps}\end{figure}$ Figure 4: Anticenter view of the H I emission integrated over the velocity range -400 < v < -100 km s^-1 in the LAB dataset, shown in an Aitoff projection. The integrated emission ( $0 < N_{\rm H} < 5 \times 10^{20}$ cm^-2, logarithmic scale) yields column densities under the assumption of optical transparency; this assumption may be violated at latitudes within about 10 $^\circ$ of the Galactic equator.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=11.7cm,clip]{1864f005.eps}\end{figure}$ Figure 5: Anticenter view of the H I emission integrated over the velocity range +100 < v < +400 km s^-1 in the LAB dataset, shown in an Aitoff projection. The integrated emission ( $0 < N_{\rm H} < 5 \times 10^{20}$ cm^-2, logarithmic scale) yields column densities under the assumption of optical transparency; this assumption may be violated at latitudes within about 10 $^\circ$ of the Galactic equator.
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In the text