Volume 584, December 2015
|Number of page(s)||9|
|Section||Interstellar and circumstellar matter|
|Published online||04 December 2015|
Jet multiplicity in the proto-binary system NGC 1333-IRAS4A
Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5,
2 Osservatorio Astronomico di Roma, via di Frascati 33, 00040 Monteporzio Catone, Italy
3 LERMA, Observatoire de Paris, PSL Research University, CNRS, UMR 8112, 75014 Paris, France
4 Sorbonne Universités, UPMC Univ. Paris 6, UMR 8112, LERMA, 75005 Paris, France
5 Univ. Grenoble Alpes, IPAG, 38000 Grenoble, France
6 CNRS, IPAG, 38000 Grenoble, France
7 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS – Université Paris Diderot, CE-Saclay, 91191 Gif-sur-Yvette, France
8 IRAM, 300 rue de la Piscine, 38406 Saint Martin d’Hères, France
9 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
10 ESO, Karl-Schwarzschild-Strasse 2, 85748 Garching bei München, Germany
Received: 15 April 2015
Accepted: 14 August 2015
Context. Owing to the paucity of sub-arcsecond (sub)mm observations required to probe the innermost regions of newly forming protostars, several fundamental questions are still being debated, such as the existence and coevality of close multiple systems.
Aims. We study the physical and chemical properties of the jets and protostellar sources in the NGC 1333-IRAS4A proto-binary system using continuum emission and molecular tracers of shocked gas.
Methods. We observed NGC 1333-IRAS4A in the SiO(6−5), SO(65−54), and CO(2−1) lines and the continuum emission at 1.3, 1.4, and 3 mm using the IRAM Plateau de Bure Interferometer in the framework of the CALYPSO large program.
Results. We clearly disentangle for the first time the outflow emission from the two sources A1 and A2. The two protostellar jets have very different properties: the A1 jet is faster, has a short dynamical timescale (≲103 yr), and is associated with H2 shocked emission, whereas the A2 jet, which dominates the large-scale emission, is associated with diffuse emission, bends, and emits at slower velocities. The observed bending of the A2 jet is consistent with the change of propagation direction observed at large scale and suggests jet precession on very short timescales (~200−600 yr). In addition, a chemically rich spectrum with emission from several complex organic molecules (e.g. HCOOH, CH3OCHO, CH3OCH3) is only detected towards A2. Finally, very high-velocity shocked emission (~50 km s-1) is observed along the A1 jet. An LTE analysis shows that SiO, SO, and H2CO abundances in the gas phase are enhanced up to (3−4)×10-7, (1.4−1.7)×10-6, and (3−7.9)×10-7, respectively.
Conclusions. The intrinsic different properties of the jets and driving sources in NGC 1333-IRAS4A suggest different evolutionary stages for the two protostars, with A1 being younger than A2, in a very early stage of star formation previous to the hot-corino phase.
Key words: stars: formation / stars: low-mass / ISM: jets and outflows / ISM: individual objects: NGC 1333-IRAS4A / 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).
Appendices are available in electronic form at http://www.aanda.org
© ESO, 2015
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