, S. Guilloteau 
, F. Gueth 
,
M. Tafalla ,
A. Dutrey , C. Codella , A. Castets 
IGN Observatorio Astronomico Nacional,
Apartado 1143, E-28800 Alcalá de Henares (Madrid), Spain IRAM,
300 rue de la Piscine, F-38406 Saint Martin d'Hères, France MPIfR,
Auf dem Hügel 69, D-53121 Bonn, Germany LAOG, BP53,
F-38041 Grenoble Cedex 9, France 
1.3 and 3.5 mm continuum
and the SiO J = 2 
1 emission towards the SVS13/HH7-11 vicinity
(see Fig 7).
The continuum data resolve SVS13 into two components separated by
14 
.5 ( 
4300 AU) and having very similar millimeter properties:
each of them has about 1 M 
of circumstellar material and its
emission is characterized by a spectral index of 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.
Astronomy & Astrophysics Lett. in press Preprint requests: bachiller@oan.es