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Astron. Astrophys. 362, L33-L36 (2000)

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Letter to the Editor

The origin of the HH 7-11 outflow *

R. Bachiller 1, F. Gueth 2, S. Guilloteau 3, M. Tafalla 1 and A. Dutrey 3

1 IGN Observatorio Astronómico Nacional, Apartado 1143, 28800 Alcalá de Henares, Spain (bachiller@oan.es)
2 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
3 Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine, 38406 Saint Martin d'Hères, France

Received 15 August 2000 / Accepted 26 September 2000

Abstract

New, high-sensitivity interferometric CO J=2-1 observations of the HH 7-11 outflow show that despite previous doubts, this system is powered by the Class I source SVS 13. The molecular outflow from SVS 13 is formed by a shell with a large opening angle at the base, which is typical of outflows from Class I sources, but it also contains an extremely-high-velocity jet composed of "molecular bullets", which is more typical of Class 0 outflows. This suggests that SVS 13 could be a very young Class I, which still keeps some features of the previous evolutionary stage. We briefly discuss the nature of some sources in the SVS 13 vicinity which are emitters of cm-wave continuum, but have no counterpart at mm wavelengths.

Key words: stars: formation – ISM: individual objects: HH7-11, NGC1333 – ISM: jets and outflows – ISM: molecules

* Based on observations carried out with the IRAM Plateau de Bure Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).

Send offprint requests to: R. Bachiller

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© European Southern Observatory (ESO) 2000

Online publication: October 24, 2000
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