Astron. Astrophys. 339, L49-L52 (1998)

Astron. Astrophys. 339, L49-L52 (1998)

Letter to the Editor

A molecular jet from SVS 13B near HH 7-11

R. Bachiller ¹, S. Guilloteau ², F. Gueth ³, M. Tafalla ¹, A. Dutrey ², C. Codella ¹ and A. Castets ⁴

¹ IGN Observatorio Astronómico Nacional, Apartado 1143, E-28800 Alcalá de Henares, Spain
² Institut de Radio Astronomie Millimétrique, 300 rue de la Piscine, F-38406 Saint Martin d'Hères, France
³ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, D-53121 Bonn, Germany
⁴ Laboratoire d'Astrophysique, Observatoire de Grenoble, BP53, F-38041 Grenoble Cedex 9, France

Received 2 September 1998 / Accepted 5 October 1998

Abstract

We present interferometric images of the [FORMULA] 1.3 and 3.5 mm continuum and the SiO emission towards the SVS 13/HH 7-11 vicinity. The continuum data resolve SVS 13 into two components separated by 145 ( 4300 AU) and having very similar millimeter properties: each of them has about 1 of circumstellar material and its emission is characterized by a spectral index of [FORMULA] 2.5. One of the components, SVS 13B, lacks optical, near infrared, or cm-wave counterpart, and is only detectable at millimeter waves, a fact that suggests it represents an extremely embedded, Class 0 object. This source, in addition, powers a remarkably collimated molecular outflow as seen by a high velocity SiO jet. HH 12, HH 16, and HH 352 lie along the line of this jet, suggesting they are also excited by SVS 13B. Our observations highlight the star-formation richness of the HH 7-11 region which contains in a small area some of the youngest and most extraordinary outflows known.

Key words: stars: formation interstellar medium: individual objects: SVS13B, HH7-11, NGC1333 interstellar medium: jets and outflows interstellar medium: molecules radio lines: molecular: interstellar

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Online publication: October 22, 1998
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A molecular jet from SVS 13B near HH 7-11

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