HCO+ emission in the HH7-11 region - the slowest component of the outflow

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)

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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.

Item Type: Article
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)
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