All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=6cm,clip]{2617fig1.ps}\hspace*{2mm} \includegraphics[angle=-90,width=6cm,clip]{2617fig2.ps} \end{figure}$ Figure 1: Left panel: ATCA-3 cm radio continuum image towards WR 21a. The optical position of the star is marked with a cross. The contour levels are -0.20, 0.20 ( $2\sigma$ ), 0.30, 0.35, 0.40, 0.45, 0.50, and 0.55 mJy beam^-1. The synthesized beam ( $0.83\hbox {$^{\prime \prime }$ }\times 0.70\hbox {$^{\prime \prime }$ }$ ) is displayed at the bottom left corner. Right panel: ATCA-6 cm radio continuum image towards WR 21a. The contour levels are -0.12, 0.12 ( $2\sigma$ ), 0.18, 0.24, 0.30, and 0.33 mJy beam^-1. The synthesized beam ( $1.73\hbox {$^{\prime \prime }$ }\times 1.49\hbox {$^{\prime \prime }$ }$ ) is displayed at the bottom left corner.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2617fig3.eps} \end{figure}$ Figure 2: H I-brightness temperature distribution of the Galactic emission as measured with the IAR telescope ( HPBW = 30 arcmin) over a velocity range from -24 to +12 km s^-1, in steps of 4 km s^-1. The position of WR 21a is marked with a white star. The contour levels indicate H I brightness temperatures in steps of 5 Kelvin.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{2617fig4.eps} \end{figure}$ Figure 3: Neutral-hydrogen column density integrated over velocities from -21 to -14 km s^-1. The contour levels indicate H I brightness temperatures in steps of 4 Kelvin. The IAR telescope beam is displayed in the bottom left corner. The position of WR 21a is marked with a black star, and the black contours represent the 99, 95 and 50% probability contours for the location of the gamma-ray source 3EG J1027-5817.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2617fig5.eps} % \end{figure}$ Figure 4: 3.3 GHz radio recombination line H125 $\alpha$ towards RCW 49. ${\it HPBW} = 12.4^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2617fig6.eps} \end{figure}$ Figure 5: The history of WR 21a's 1-2 keV X-ray luminosity since its discovery in 1979 with the Einstein Observatory, through measurements in the early 1990s with ROSAT to the RXTE and ASCA measurements of 1997 and 1998. WR 21a is bright and the luminosity errors are usually smaller than the plotting symbols. The luminosities were calculated assuming the spectrum did not change shape and the range 1-2 keV was chosen to provide good overlap between instruments whose sensitivity ranges were different. The highest point is from RXTE which, as explained in the text, probably included a significant contribution from nearby unresolved point-source and diffuse emission.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{2617fig3.eps} \end{figure}$	Figure 2: H I-brightness temperature distribution of the Galactic emission as measured with the IAR telescope ( HPBW = 30 arcmin) over a velocity range from -24 to +12 km s^-1, in steps of 4 km s^-1. The position of WR 21a is marked with a white star. The contour levels indicate H I brightness temperatures in steps of 5 Kelvin.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{2617fig5.eps} % \end{figure}$	Figure 4: 3.3 GHz radio recombination line H125 $\alpha$ towards RCW 49. ${\it HPBW} = 12.4^{\circ }$ .
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