Image Digitisation of Outflows and the AAO/UKSTU Htex2html_wrap_inline59 Survey

W. J. Zealey, S. L. Mader, PASA, 15 (1), 165
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HH 49/50

Figure 1. shows IIIaJ, IIIaF, and IVN images of the region near the visible reflection nebula Ced 110 and objects HH 49/50. First discovered by Schwartz (1977) these objects are located in a high extinction region of the Cha I cloud at a distance of 140 pc. Cohen & Schwartz (1987) suggested IRAS 11054-7706C as a candidate energy source for HH 49/50, but Prusti et al. (1991) showed this source to be multiple and argued for the central component (hereafter IRS4) as the driving source. IRS4 also drives a molecular outflow inline with the axis defined by IRS4 and the HH objects (Mattila, Liljestróm & Toriseva 1989).

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Figure 1: IIIaJ [J], IIIaF [R], and IVN [I] images of the region near Ced 110 and HH 49/50.

The nebulosity associated with Ced 110 is clearly seen in the IIIaJ, IIIaF and IVN images. HH 49/50 are seen in the IIIaF image, but not in the IVN image thus indicating they are dominated by line-emission. As IRS4 is highly obscured, we do not see any reddened sources at its location (indicated by a cross) in the IVN image. The IIIaJ/IIIaF images show a reflection nebulosity located slightly north-east of IRS4 which could be associated with the embedded source and not Ced 110.

By comparing Htex2html_wrap_inline59 survey plates with existing ESO/SERC material, we do not have to resort to CCD cameras with small fields of view to study morphological properties of new and existing outflow features, although follow-up observations are vital for deeper studies. The direct comparison of the Htex2html_wrap_inline59 and ESO/SERC plates will also determine if nebulosities are dominated by line-emission seen in shocked regions of HH objects and Supernova remnants. The scale of outflows from low-mass YSOs is only now being realised with the discovery of parsec-scale HH flows using wide field of view (up to 1tex2html_wrap_inline89) CCD cameras (Bally & Devine 1994). The 6tex2html_wrap_inline89 fields of the Htex2html_wrap_inline59 survey and ESO/SERC material will provide new insights into these giant HH flows and their smaller (< 1 pc) counterparts.


Next Section: Conclusions & Future Directions
Title/Abstract Page: Image Digitisation of Outflows
Previous Section: Introduction
Contents Page: Volume 15, Number 1

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