All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{7309f1.ps} \end{figure}$ Figure 1: The Galactic rotation curve toward Galactic longitude of $339\hbox{$.\!\!^\circ$ }6$ using a Galactocentric radius of $R_\odot = 7.6$ kpc and a circular velocity of $\Theta _\odot = 214$ km s^-1 for the Sun. We assumed a flat rotation curve and purely circular rotation. The approximate locations of the spiral arms in radial velocity are indicated. Here the indices I and II indicate the first and second time the line of sight passes through that spiral arm (see also Fig. 2).
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{7309f2.eps} \end{figure}$ Figure 2: The spiral arm pattern of the Milky Way Galaxy (Cordes & Lazio 2002; Taylor & Cordes 1993). The names of the spiral arms and the line of sight (LOS) toward Wd 1 are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7309f3.eps} \end{figure}$ Figure 3: H I emission profile averaged over an area of a few arcminutes towards Wd 1. The locations of the spiral arms as listed in Table 1 are indicated. The Local arm is indicated at 0 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7309f4.ps} \end{figure}$ Figure 4: H I absorption profiles of four radio bright H II regions in the vicinity of Wd 1. To make the individual components better comparable we plotted the relative absorption - the ratio of absorbed emission to total emission - as a function of radial velocity. The dotted vertical lines indicate the systemic velocities of the H II regions (Russeil 2003), which, within their uncertainties, are in excellent agreement with the absorption peaks.
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In the text

$\begin{figure} \par\includegraphics[width=7.85cm,clip]{7309f5.ps} \end{figure}$ Figure 5: H I channels images averaged together to demonstrate in which spiral arms Wd 1 is absorbed. For the individual arms we averaged over: +5 to -1 km s^-1 (Local arm), -10 to -20 km s^-1 (Sagittarius arm), -32 to -45 km s^-1 (Scutum-Crux arm), -85 to -102 km s^-1 (Norma arm), and -110 to -125 km s^-1 (Tangent Point). In these images white denotes high and black weak emission. The radio continuum emission of Wd 1 is indicated by the white contours.
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In the text

$\begin{figure} \par\includegraphics[width=10.3cm,clip]{7309f6.ps} \end{figure}$ Figure 6: Three views of the two small expanding bubbles, B1 and B2, around Wd 1, indicated by dashed and dotted ellipses respectively. Longitude-velocity slices are displayed at the top and bottom and the velocity-latitude slices in the left and right panels. The HI channel map at about -55 km s^-1 in longitude-latitude is shown in the centre, with Wd 1 indicated by the white contours. The bright emission in the velocity slices mark the gas at the far edge of Scutum-Crux I. In these images black represents low and white high intensity.
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In the text

$\begin{figure} \par\includegraphics[width=7.45cm,clip]{7309f7.ps} \end{figure}$ Figure 7: H I channelmap at a radial velocity of -55 km s^-1 from the SGPS. Black contours go from 20 K to 90 K in steps of 10 K. Grayish contours indicate the 1420 MHz continuum emission. The location of Wd 1 is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.05cm,clip]{7309f8.ps} \end{figure}$ Figure 8: Radio continuum emission at 1420 MHz around Wd 1 taken from the end channels of the SGPS H I observations. Contours are at 11, 17, 23, and 40 K (black) and 80, 120, and 160 K (white). The dotted ellipses enclose SNRs and H II regions that are believed to be beyond the Tangent point. The location of Wd 1 is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7309f9.ps} \end{figure}$ Figure 9: H I absorption profiles of one radio bright H II region (G338.9+0.4) and three bright SNRs in the vicinity of Wd 1.
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In the text

$\begin{figure} \par\includegraphics[width=6.55cm,clip]{7309f10.ps} \end{figure}$ Figure 10: Radio continuum spectrum of the H II region, produced by the members of Wd 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{7309f2.eps} \end{figure}$	Figure 2: The spiral arm pattern of the Milky Way Galaxy (Cordes & Lazio 2002; Taylor & Cordes 1993). The names of the spiral arms and the line of sight (LOS) toward Wd 1 are indicated.
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$\begin{figure} \par\includegraphics[width=8.45cm,clip]{7309f3.eps} \end{figure}$	Figure 3: H I emission profile averaged over an area of a few arcminutes towards Wd 1. The locations of the spiral arms as listed in Table 1 are indicated. The Local arm is indicated at 0 km s^-1.
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$\begin{figure} \par\includegraphics[width=7.45cm,clip]{7309f7.ps} \end{figure}$	Figure 7: H I channelmap at a radial velocity of -55 km s^-1 from the SGPS. Black contours go from 20 K to 90 K in steps of 10 K. Grayish contours indicate the 1420 MHz continuum emission. The location of Wd 1 is indicated.
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$\begin{figure} \par\includegraphics[width=8.05cm,clip]{7309f8.ps} \end{figure}$	Figure 8: Radio continuum emission at 1420 MHz around Wd 1 taken from the end channels of the SGPS H I observations. Contours are at 11, 17, 23, and 40 K (black) and 80, 120, and 160 K (white). The dotted ellipses enclose SNRs and H II regions that are believed to be beyond the Tangent point. The location of Wd 1 is indicated.
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$\begin{figure} \par\includegraphics[width=7.55cm,clip]{7309f9.ps} \end{figure}$	Figure 9: H I absorption profiles of one radio bright H II region (G338.9+0.4) and three bright SNRs in the vicinity of Wd 1.
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$\begin{figure} \par\includegraphics[width=6.55cm,clip]{7309f10.ps} \end{figure}$	Figure 10: Radio continuum spectrum of the H II region, produced by the members of Wd 1.
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