Astronomy & Astrophysics

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$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{Fj061.1.eps} \end{figure}$ Figure 1: Velocity components ( $V_{\rm p}$ , $V_{\phi }$ ) in the (R, Z) plane for the warm solution ( $\lambda = 13$ ). Dashed lines: $V_{\phi }$ varying from 4 to 16 km s^-1 by steps of 4 km s^-1. Greyscale: $V_{\rm p}$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Fj061.2a.eps}\vspace*{3mm} \includegraphics[width=8.8cm,clip]{Fj061.2b.eps} \end{figure}$ Figure 2: a) Synthetic transverse Position-Velocity (PV) diagram for the warm solution (integrated over $Z_{{\rm proj}} = 50$ -60 AU) in the [O I] $\lambda$ 6300 line, convolved with a 14 ${\rm AU} \times 50$ km s^-1 beam. $i = 45^{\circ }$ and $x_{{\rm e}} = 0.1 ~\times~ (0.1 ~{\rm AU}/R_{{\rm 0}})$ . Dashed lines are indicative of peak velocity shifts at 10 and 20 AU from the jet axis. b) Velocity profiles extracted from PV diagrams at $R_{{\rm proj}} = \pm 10$ AU, convolved with a spatial beam of 14 AU for $x_{{\rm e}} = 0.1 \times (0.1~{\rm AU}/R_{{\rm 0}})$ (solid lines) and $x_{{\rm e}} = 0.1 \times (R_{{\rm 0}}/1~{\rm AU})$ (dashed lines), c) and at $R_{{\rm proj}}=\pm 20$ AU, with spatial beams of 1 (dotted) and 14 AU (solid) for $x_{{\rm e}} = 0.1 \times (0.1~{\rm AU}/R_{{\rm 0}})$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{Fj061.3a.eps}\hs... ...*{3mm} \includegraphics[angle=-90,width=8.8cm,clip]{Fj061.3b.eps} \end{figure}$ Figure 3: Velocity shifts predicted by the disc wind models as a function of projected transverse radius $R_{{\rm proj}}$ . Left: cold solution with the thermal structure of Garcia et al. (2001a). Right: warm solution with two ionization fraction laws (see Sect. 2 for more details). $V_{{\rm shift}}$ are obtained by cross-correlating [O I] $\lambda$ 6300 line profiles at $\pm$ $R_{{\rm proj}}$ , extracted from a transverse PV diagram at $Z_{{\rm proj}} = 50$ -60 AU. Solid and dash-dotted lines: $V_{{\rm shift}}$ computed using the entire velocity profile, short-dashed and long-dashed lines: or restricting to the MVC. Dotted lines show the projected underlying true azimuthal profile extracted from the corresponding wind solution. $R_{{\rm jet}}$ is the outermost jet radius (for $R_{{\rm e}} = 1$ AU).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{Fj061.4.eps} \end{figure}$ Figure 4: Velocity shifts as a function of radius at four deprojected distances from the star, 17 to 91 AU, obtained by cross-correlation over the MVC. Symbols: DG Tau observations (Bacciotti et al. 2002). Curves: predictions for the cold (dashed; $R_{{\rm e}} = 1$ AU) and warm (solid; $R_{{\rm e}} = 3$ AU) disc wind solutions in [S II] $\lambda$ 6731 (light grey), [O I] $\lambda$ 6300 (dark grey) and [Fe II] 1.644 $\mu$ m (black), computed with the estimated inclination angle of DG Tau jet (45 $^{\circ }$ ; Pyo et al. 2003) and with the beam size of HST/STIS ( $0.1\hbox {$^{\prime \prime }$ }\times 50$ km s^-1).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.7cm,clip]{Fj061.1.eps} \end{figure}$	Figure 1: Velocity components ( $V_{\rm p}$ , $V_{\phi }$ ) in the (R, Z) plane for the warm solution ( $\lambda = 13$ ). Dashed lines: $V_{\phi }$ varying from 4 to 16 km s^-1 by steps of 4 km s^-1. Greyscale: $V_{\rm p}$ .
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