All Figures

$\begin{figure} \par\includegraphics[width=15.8cm,clip]{8339fig1.eps}\end{figure}$ Figure 1: Grey-scale images showing the H I gas distribution in the velocity range 64.4 to 43.8 $\rm km~s^{-1}$ observed with the VLA and the 100 m Effelsberg telescope. The position of WR 124 is indicated by a star symbol. Velocity resolution is 2.6 $\rm km~s^{-1}$ and the spatial resolution is 46 $.\!\!^{\prime\prime}$ 5 $\times$ 45 $.\!\!^{\prime\prime}$ 5 with a PA of 16 $.\!\!^\circ$ 6. The LSR velocity of each image is indicated in the top left corner. Letters A and B indicate the cavities described in the text. Contour levels with respect to the average over each image are - 13, -8, -3, 0 and 5 K. Noise is 0.3 K or 1.05 mJy beam^-1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{8339fig2.eps}\end{figure}$ Figure 2: Average H I brightness temperature within the LSR velocity interval 54.1 to 61.8 $\rm km~s^{-1}$ . Contour levels with respect to the average over the image (28 K) are -10, -6, -2, 0, 2 and 6 K. The cross indicates the position of WR 124.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{8339fig3.ps}\end{figure}$ Figure 3: a) Radio continuum image of M1-67 at 8.5 GHz with a resolution of $\sim$ 8 $^{\prime \prime }$ . The grey scale goes from 0 to 7 mJy beam^-1 (dark grey). b) HST-WFPC2 H $\alpha$ image of M 1-67 obtained by Grosdidier et al. (2001). Resolution is $\sim$ 0 $.\!\!^{\prime\prime}$ 2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=11.6cm,clip]{8339fig4.ps}\end{figure}$ Figure 4: MSX images towards WR 124 (star symbol). The lowest contour level represents a noise level of 4.5 $\sigma$ for band A and 3 $\sigma$ for the others bands. Low intensity regions are indicated by light greys. Top left panel: 8.28 $\mu$ m (band A) emission. The grey scale range is -2 to 35 MJy sr^-1. The contour lines are 6, 10, 14, 18, 26, 34, 42 and 50 MJy sr^-1. Top right panel: band C image (12.1 $\mu$ m). The grey scale spans -75 to 130 MJy sr^-1. The contour line is 57.7 MJy sr^-1. Bottom left panel: band D image at 14.65 $\mu$ m. The grey scale range is -47 to 80 MJy sr^-1. The contour line is 33.6 MJy sr^-1. Bottom right panel: band E image at 21.3 $\mu$ m. The grey scale covers the range -130 to 260 MJy sr^-1, contour lines are 79.5 and 159.0 MJy sr^-1.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{8339fig5.eps}\end{figure}$ Figure 5: Histograms of the random H I holes area and velocity extent identified in a region near the stellar position. The arrows indicate the area and velocity extent observed for cavity A.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8339fig6.eps}\end{figure}$ Figure 6: Schematic side view representation of the geometry of the bow shock model. The horizontal axis represents the symmetry axis of the bow shock and $l_{\rm o}$ is the stand-off distance.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{8339fig7.eps}\end{figure}$ Figure 7: a) H I emission distribution at v = 61.8, where cavity A is best delineated. b) H I emission distribution at v = 54.1 $\rm km~s^{-1}$ , where cavity B is best delineated. In both panels contour levels are -10, 0 and 5 K. The cross marks the position of WR 124. The 3D bow shock structure for $i = 30^{\circ }$ and $\phi = 170^{\circ }$ is shown in the bottom right corner.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=6.3cm,clip]{8339fig2.eps}\end{figure}$	Figure 2: Average H I brightness temperature within the LSR velocity interval 54.1 to 61.8 $\rm km~s^{-1}$ . Contour levels with respect to the average over the image (28 K) are -10, -6, -2, 0, 2 and 6 K. The cross indicates the position of WR 124.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=13.2cm,clip]{8339fig3.ps}\end{figure}$	Figure 3: a) Radio continuum image of M1-67 at 8.5 GHz with a resolution of $\sim$ 8 $^{\prime \prime }$ . The grey scale goes from 0 to 7 mJy beam^-1 (dark grey). b) HST-WFPC2 H $\alpha$ image of M 1-67 obtained by Grosdidier et al. (2001). Resolution is $\sim$ 0 $.\!\!^{\prime\prime}$ 2.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{8339fig5.eps}\end{figure}$	Figure 5: Histograms of the random H I holes area and velocity extent identified in a region near the stellar position. The arrows indicate the area and velocity extent observed for cavity A.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{8339fig6.eps}\end{figure}$	Figure 6: Schematic side view representation of the geometry of the bow shock model. The horizontal axis represents the symmetry axis of the bow shock and $l_{\rm o}$ is the stand-off distance.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=14.4cm,clip]{8339fig7.eps}\end{figure}$	Figure 7: a) H I emission distribution at v = 61.8, where cavity A is best delineated. b) H I emission distribution at v = 54.1 $\rm km~s^{-1}$ , where cavity B is best delineated. In both panels contour levels are -10, 0 and 5 K. The cross marks the position of WR 124. The 3D bow shock structure for $i = 30^{\circ }$ and $\phi = 170^{\circ }$ is shown in the bottom right corner.
Open with DEXTER