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A molecular jet from SVS13B near HH7-11

R. Bachiller tex2html_wrap_inline1123 , S. Guilloteau tex2html_wrap_inline1115 , F. Gueth tex2html_wrap_inline1121 , M. Tafalla tex2html_wrap_inline1123 , A. Dutrey tex2html_wrap_inline1115 , C. Codella tex2html_wrap_inline1123 , A. Castets tex2html_wrap_inline1117
tex2html_wrap_inline1123 IGN Observatorio Astronomico Nacional, Apartado 1143, E-28800 Alcalá de Henares (Madrid), Spain
tex2html_wrap_inline1115 IRAM, 300 rue de la Piscine, F-38406 Saint Martin d'Hères, France
tex2html_wrap_inline1121 MPIfR, Auf dem Hügel 69, D-53121 Bonn, Germany
tex2html_wrap_inline1117 LAOG, BP53, F-38041 Grenoble Cedex 9, France
Abstract: We present interferometric images of the tex2html_wrap_inline1023  1.3 and 3.5 mm continuum and the SiO J = 2 tex2html_wrap_inline1029 1 emission towards the SVS13/HH7-11 vicinity (see Fig 7). The continuum data resolve SVS13 into two components separated by 14 tex2html_wrap_inline1401 .5 ( tex2html_wrap_inline1229 4300 AU) and having very similar millimeter properties: each of them has about 1 M tex2html_wrap_inline1405 of circumstellar material and its emission is characterized by a spectral index of tex2html_wrap_inline1229 2.5. One of the components, SVS13B, 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. HH12, HH16, and HH352 lie along the line of this jet, suggesting they are also excited by SVS13B. Our observations highlight the star-formation richness of the HH7-11 region which contains in a small area some of the youngest and most extraordinary outflows known.

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