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

Dent, W.R.F., Cunningham, C.T., Hayward, R.H, Davies, S.R., Wade, D., Avery, L.W., Mayer, C.J., 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 full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided. (Contact us about this Publication)

Abstract

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 > Sciences > School of Engineering and Digital Arts
Depositing User: R.F. Xu
Date Deposited: 15 Jul 2009 09:50 UTC
Last Modified: 28 May 2019 13:59 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/20873 (The current URI for this page, for reference purposes)
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