Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=6.2cm,clip]{0439fig1.eps} \end{figure}$ Figure 1: Schematic drawing of the observing mode for the bi-polar jet from RW Aur. The STIS slit is kept parallel to the flow axis, and stepped sequentially in seven different positions (labelled S1, S2...S7) each time by 0 $.\!\!^{\prime\prime}$ 07. The slit width is 0 $.\!\!^{\prime\prime}$ 1, so the apertures are slightly overlapping. The sense of rotation derived in the present paper is illustrated by the arrows around the symmetry axis.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0439fig2.eps} \end{figure}$ Figure 2: Example of a Gaussian fit to the line profile that yields the peak velocity. This plot shows [SII] $\lambda$ 6731 at slit position S3 and at a separation of $0\hbox{$.\!\!^{\prime\prime}$ }9$ from the star.
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In the text

$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0439fig3.eps} \end{figure}$ Figure 3: Peak velocities for different slit positions and separations from the star. Crosses denote [SII] $\lambda$ 6731, squares [SII] $\lambda$ 6716,circles [OI] $\lambda$ 6363, triangles [OI] $\lambda$ 6300, plus signs [NII] $\lambda$ 6548, asterisks [NII] $\lambda$ 6583, and diamonds H $\alpha$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0439fig4.eps} \end{figure}$ Figure 4: Peak radial velocity differences in the redshifted outflow lobe as a function of separation from the source. Upper panel: difference between the values measured at slits S7 and S1, or at 30 AU from the axis. Middle panel: S6 - S2, corresponding to 20 AU from the axis. Lower panel: S5 - S3, or 10 AU from the axis. The plot symbols have the same meaning as in Fig. 3. The large diamonds represent H $\alpha$ at the stellar position, the open one before the correction for uneven slit illumination and the filled one afterwards.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0439fig5.eps} \end{figure}$ Figure 5: Same as Fig. 4, but for the blueshifted outflow lobe.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0439fig6.eps}\end{figure}$ Figure 6: Sketch (not to scale) of the configuration of the flow/magnetic surfaces (solid thin lines) attached to the inner section of the accretion disk around RW Aur A, according to the disk-wind scenario. Thick grey arrows indicate the mass flows. Note the different distances of the footpoints for the blue and red flows seen at 0 $.\!\!^{\prime\prime}$ 4 above the disk. This is due to the asymmetry in the bipolar jet.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0439fig2.eps} \end{figure}$	Figure 2: Example of a Gaussian fit to the line profile that yields the peak velocity. This plot shows [SII] $\lambda$ 6731 at slit position S3 and at a separation of $0\hbox{$.\!\!^{\prime\prime}$ }9$ from the star.
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$\begin{figure} \par\includegraphics[width=14.3cm,clip]{0439fig3.eps} \end{figure}$	Figure 3: Peak velocities for different slit positions and separations from the star. Crosses denote [SII] $\lambda$ 6731, squares [SII] $\lambda$ 6716,circles [OI] $\lambda$ 6363, triangles [OI] $\lambda$ 6300, plus signs [NII] $\lambda$ 6548, asterisks [NII] $\lambda$ 6583, and diamonds H $\alpha$ .
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{0439fig5.eps} \end{figure}$	Figure 5: Same as Fig. 4, but for the blueshifted outflow lobe.
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