First results from the CALYPSO IRAM-PdBI survey
1 INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy ;
2 Harvard-Smithsonian Center for Astrophysics, 60 Garden street, Cambridge, MA 02138, USA
3 ESO, Karl Schwarzchild Str. 2, 85748 Garching bei München, Germany
4 IRAM, 300 rue de la Piscine, 38406 Saint Martin d’Hères, France
5 UJF-Grenoble1/CNRS-INSU, Institut de Planétologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France
6 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
7 LERMA, Observatoire de Paris, CNRS, ENS, UPMC, UCP, 61 Av. de l’Observatoire, 75014 Paris, France
8 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu – CNRS -Université Paris Diderot, CE Saclay, 91191 Gif-sur-Yvette Cedex, France
Received: 11 November 2013
Accepted: 22 January 2014
Context. The earliest evolutionary stages of low-mass protostars are characterised by hot and fast jets which remove angular momentum from the circumstellar disk, thus allowing mass accretion onto the central object. However, the launch mechanism is still being debated.
Aims. We would like to exploit high-angular (~08) resolution and high-sensitivity images to investigate the origin of protostellar jets using typical molecular tracers of shocked regions, such as SiO and SO.
Methods. We mapped the inner 22″ of the NGC 1333–IRAS2A protostar in SiO(5–4), SO(65–54), and the continuum emission at 1.4 mm using the IRAM Plateau de Bure Interferometer in the framework of the CALYPSO IRAM large program.
Results. For the first time, we disentangle the NGC 1333–IRAS2A Class 0 object into a proto-binary system revealing two protostars (MM1, MM2) separated by ~560 AU, each of them driving their own jet, while past work considered a single protostar with a quadrupolar outflow. We reveal (i) a clumpy, fast (up to | V − VLSR | ≥ 50 km s-1), and blueshifted jet emerging from the brightest MM1 source; and (ii) a slower redshifted jet, driven by MM2. Silicon monoxide emission is a powerful tracer of high-excitation (Tkin ≥ 100 K; nH2 ≥ 105 cm-3) jets close to the launching region. At the highest velocities, SO appears to mimic SiO tracing the jets, whereas at velocities close to the systemic one, SO is dominated by extended emission, tracing the cavity opened by the jet.
Conclusions. Both jets are intrinsically monopolar, and intermittent in time. The dynamical time of the SiO clumps is ≤30–90 yr, indicating that one-sided ejections from protostars can take place on these timescales.
Key words: stars: formation / ISM: jets and outflows / ISM: molecules / planetary nebulae: individual: NGC 1333-IRAS2A
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
SiO and SO maps reported in Fig. 1 are available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/563/L3
© ESO, 2014