Dent, W.R.F. and Cunningham, C.T. and Hayward, R.H and Davies, S.R. and Wade, D. and Avery, L.W. and Mayer, C.J. and Masuda, N.T. (1993) HCO+ emission in the HH7-11 region - the slowest component of the outflow. Monthly Notices of the Royal Astronomical Society, 262 (1). L13-L18. ISSN 0035-8711. (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)
The region of the high-velocity outflow in HH7-11 has been mapped in the J = 4-3 transition of HCO+. The results are compared with published optical, CO and J = 1-0 HCO+ maps. Unlike the latter interferometric data, we see a bright compact source associated with the exciting star, plus weaker emission throughout the region. Extended emission surrounds the line of HH objects, and has a structure very similar to that of the blueshifted CO outflow. Spectra of the J = 4-3 and 3-2 lines in selected positions within the flow region indicate two physical components: (i) cool gas at a density of a few x 10(6) cm-3 at the velocity of SSV13 and the ambient cloud; and (ii) warm (35 K) gas at a few x 10(5) cm-3 blueshifted by almost-equal-to 1 km s-1. The close agreement between the HCO+ and higher velocity CO suggests that the former arises from the densest, slowest component of the molecular flow. The structure appears to favour a confined jet rather than a shocked cloudlet model.
|Subjects:||Q Science > QB Astronomy|
|Divisions:||Faculties > Science Technology and Medical Studies > School of Engineering and Digital Arts|
|Depositing User:||R.F. Xu|
|Date Deposited:||15 Jul 2009 09:50|
|Last Modified:||09 Jul 2014 09:23|
|Resource URI:||https://kar.kent.ac.uk/id/eprint/20873 (The current URI for this page, for reference purposes)|