SpringerLink
Forum Springer Astron. Astrophys.
Forum Whats New Search Orders


Astron. Astrophys. 325, 542-550 (1997)

Previous Section Next Section Title Page Table of Contents

5. Conclusions

  1. We have presented 1300 µm continuum maps of the environment of 20 HH energy sources. The dust emission arises from a compact component surrounded by a diffuse envelope. The relative contributions of both components to the total flux from the area varies from very compact to rather diffuse sources.
  2. Half of the sources show a flattened shape of the dust emission contours. The orientations of these ellipsoids are not correlated to the optical jet axes of the HH flows.
  3. Within the HH 114 region we have detected a new mm-continuum source (HH 114 MMS) with a rather flat ([FORMULA]) SED from 350 to 2000 µm. Its ratio [FORMULA] qualifies this source as Class 0.
  4. Within the HH 1-2 region there are four mm-sources. MMS1 corresponds to the double source VLA 1/2 driving the HH 1-2 and HH 144 flows. There is a fainter ridge 17 [FORMULA], to the SSW of MMS1, located in a dense lobe of the flattened NH3 structure surrounding MMS1. MMS2 is associated with the VLA sources found near an H2 O maser SW of HH 1. A fainter source, MMS3, is found about 20 [FORMULA], SSW of MMS2; both of these sources are associated with an extended NH3 cloud. In the north-eastern part of the region we see the mm emission from the energy source of HH 147.
  5. Close to the driving source of HH 108-109 we have detected a new mm-continuum source (HH 108 MMS) which we suggest to be a further protostellar candidate.
  6. In the region of HH 7-11 we have detected three mm sources. MMS1 and MMS2 coincide with two mm sources previously detected by Grossman et al. (1987) while MMS3 is new. Comparison with the VLA observations of Rodríguez et al. (1997) suggests that their VLA 2 and our MMS3 coincide, and that their VLA 3 and our MMS1 are identical. The coincidence of a strong mm source with VLA 3 supports the suggestion of Rodríguez et al. (1997) that VLA 3, rather than SVS 13, is the driving source of the HH 7-11 outflow.
Previous Section Next Section Title Page Table of Contents

© European Southern Observatory (ESO) 1997

Online publication: April 28, 1998

helpdesk.link@springer.de