Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg01.eps} \end{figure}$ Figure 1: CW Tau: mosaic of the entire CW Tau outflow. The top and middle frames are in [SII] and the bottom frame is in H $\alpha$ as HH 827 is much stronger in H $\alpha$ . All known IRAS sources in the region are marked with white crosses. The individual knots can be seen more clearly in Figs. 2 to 4. Any information in the gaps between the CCDs (white strips) is lost. The northern edge of this image is the northern edge of the field of view of the CCD Mosaic. Note that the linear object to the east of HH 829 B is an asteroid trail. For all images in this paper, North is up and West is to the right.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg02.eps} \end{figure}$ Figure 2: CW Tau: left: our [SII] image showing CW Tau and the newly discovered HH 826 and HH 828 knots. The small white box superimposed on CW Tau marks the region shown on the right. Right: CW Tau and the HH220 jet taken from Dougados et al. (2000). A dotted line shows the PA of 144 $^\circ$ determined by Dougados et al. (2000) and a similar line at 144 $^\circ$ is superimposed on our [SII] image to show the slight change in direction of the outflow.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg03.eps} \end{figure}$ Figure 3: HH 827 H $\alpha$ : continuum subtracted H $\alpha$ image of HH 827 to the south of CW Tau. The trail of emission to the northeast is clearly seen and the fainter trail to the southwest extends for $\sim$ 31 $^{\prime \prime }$ from the southern end of the bright knot.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg04.eps} \end{figure}$ Figure 4: HH 829: image of HH 829 A, B and C to the north of CW Tau in [SII] ( left) and H $\alpha$ ( right). HH 829 C is stronger in H $\alpha$ emission and HH 829 B is stronger in [SII] emission, while HH 829 A is comparable in both.
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In the text

$\begin{figure} \par\includegraphics[width=17.2cm,clip]{0163fg05.eps} \end{figure}$ Figure 5: DG Tau: a) mosaic image of the region surrounding DG Tau and DG Tau B in H $\alpha$ : the new objects discovered in both the DG Tau outflow (HH 830) and the DG Tau B outflow (HH 836 and HH 837) are indicated here. HH 838 and HH 839 appear to be separate outflows in this region. A HST image of HH 158 is included here as an inset and has been rotated such that north is up. This inset is 21 $\hbox{$.\!\!^{\prime\prime}$ }$ 7 by 22 $\hbox{$.\!\!^{\prime\prime}$ }$ 05. The dotted line through the centre of the image is at 116 $^\circ$ and marks the blueshifted DG Tau B outflow. The three known IRAS sources in the region are marked with white crosses. b) HH 830 B and C in [SII]: HH 830 C can be seen here to be two distinct regions of emission, and HH 830 B is a small knot. Note that the left hand edge of the image is actually the eastern edge of our field of view of the CCD mosaic so it is quite possible that HH 830 C is more extended. c) HH 830 A in H $\alpha$ : HH 830 A is a faint, linear emission object extending $\sim$ 28 $^{\prime \prime }$ and dips southwards towards the western edge for another 16 $^{\prime \prime }$ . d) HH 702 in H $\alpha$ : an image taken in February 2001 is used here as it shows the whole of HH 702 in one CCD field. Knots A, B, C and D (discovered by Sun et al. 2003) can clearly be seen. The newly discovered Knot E and fainter Knots F and G are also marked here. There is a star to the north of Knot E but this knot can be seen clearly in the H $\alpha$ continuum subtracted image (inset). e) HH 839 in H $\alpha$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg06.eps} \end{figure}$ Figure 6: HH 836 and HH 837: the objects to the southeast of DG Tau B are shown here in both H $\alpha$ and [SII]. See Fig. 5a for the extended DG Tau B outflow. HH 836 A is only seen in H $\alpha$ , and HH 836 B is stronger in H $\alpha$ than in [SII]. There is a distinct difference between HH 837 in H $\alpha$ and [SII]. The nearby IRAS source, which is also marked in Fig. 5a, is marked here.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{0163fg07.eps} \end{figure}$ Figure 7: DO Tau/HV Tau: a) mosaic of the DO Tau and HV Tau C regions showing the newly discovered HH objects HH 831-HH 834. The positions of candidate sources for these HH objects are marked. HH 230 is not seen in our optical images because of the DO Tau nebulosity, however the dashed line from DO Tau is at 70 $^\circ$ marking the direction of the redshifted jet. There is also a dashed line at 25 $^\circ$ from HV Tau C marking the PA of its blueshifted "micro-jet''. HH 831 and HH 832 can be seen more clearly in Figs. 8 and 9. b) HH 705 in H $\alpha$ emission. c) HH 705 in [SII] emission. d) HH 834 in H $\alpha$ . Note that HH 834 is not seen in [SII] emission.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg08.eps} \end{figure}$ Figure 8: HH 831 and HH 832 [SII]: [SII] image of the newly discovered objects HH 831 and HH 832. Note that the morphology of HH 831 is quite different here to the H $\alpha$ image (Fig. 9) and that HH 832 is clearly seen in [SII] emission.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg09.eps} \end{figure}$ Figure 9: HH 831 H $\alpha$ : HH 831 as seen in H $\alpha$ emission. Note that this object is much fainter in H $\alpha$ emission than in [SII] (Fig. 8) and there is no indication of HH 832 here.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg10.eps} \end{figure}$ Figure 10: RW Aur H $\alpha$ : in this image of the RW Aur outflow, the HH 229 jet (and its direction) is clearly seen as is the newly discovered object HH 835, which is seen in more detail in Fig. 11.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg11.eps} \end{figure}$ Figure 11: HH 835 H $\alpha$ : HH 835 to the northwest of RW Aur. We suggest that this is the east/west wing of a bow shock, with the north/south wing being much fainter in our optical images.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg03.eps} \end{figure}$	Figure 3: HH 827 H $\alpha$ : continuum subtracted H $\alpha$ image of HH 827 to the south of CW Tau. The trail of emission to the northeast is clearly seen and the fainter trail to the southwest extends for $\sim$ 31 $^{\prime \prime }$ from the southern end of the bright knot.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg04.eps} \end{figure}$	Figure 4: HH 829: image of HH 829 A, B and C to the north of CW Tau in [SII] ( left) and H $\alpha$ ( right). HH 829 C is stronger in H $\alpha$ emission and HH 829 B is stronger in [SII] emission, while HH 829 A is comparable in both.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg08.eps} \end{figure}$	Figure 8: HH 831 and HH 832 [SII]: [SII] image of the newly discovered objects HH 831 and HH 832. Note that the morphology of HH 831 is quite different here to the H $\alpha$ image (Fig. 9) and that HH 832 is clearly seen in [SII] emission.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg09.eps} \end{figure}$	Figure 9: HH 831 H $\alpha$ : HH 831 as seen in H $\alpha$ emission. Note that this object is much fainter in H $\alpha$ emission than in [SII] (Fig. 8) and there is no indication of HH 832 here.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg10.eps} \end{figure}$	Figure 10: RW Aur H $\alpha$ : in this image of the RW Aur outflow, the HH 229 jet (and its direction) is clearly seen as is the newly discovered object HH 835, which is seen in more detail in Fig. 11.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0163fg11.eps} \end{figure}$	Figure 11: HH 835 H $\alpha$ : HH 835 to the northwest of RW Aur. We suggest that this is the east/west wing of a bow shock, with the north/south wing being much fainter in our optical images.
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