Volume 601, May 2017
|Number of page(s)||5|
|Published online||04 May 2017|
Oxygen budget in low-mass protostars: the NGC 1333-IRAS4A R1 shock observed in [O i] at 63 μm with SOFIA-GREAT
1 Centre for Star and Planet Formation, Niels Bohr Institute and Natural History Museum of Denmark, University of Copenhagen, Øster Voldgade 5-7, 1350 Copenhagen K, Denmark
2 LERMA, Observatoire de Paris, École normale supérieure, PSL Research University, CNRS, Sorbonne Universités, UPMC Univ. Paris 06, 75231 Paris, France
3 Max-Planck Institute for Astronomy, Königstuhl 17, 69117 Heidelberg, Germany
4 Centre for Astronomy, Nicolaus Copernicus University, Faculty of Physics, Astronomy and Informatics, Grudziadzka 5, 87100 Torun, Poland
5 European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany
6 Max-Planck-Institute for Radioastronomy, Auf dem Hügel 69, 53121 Bonn, Germany
7 I. Physikalisches Institut der Universität zu Köln, Zülpicher Strasse 77, 50937 Köln, Germany
Received: 21 December 2016
Accepted: 11 April 2017
In molecular outflows from forming low-mass protostars, most oxygen is expected to be locked up in water. However, Herschel observations have shown that typically an order of magnitude or more of the oxygen is still unaccounted for. To test if the oxygen is instead in atomic form, SOFIA-GREAT observed the R1 position of the bright molecular outflow from NGC 1333-IRAS4A. The [O i] 63 μm line is detected and spectrally resolved. From an intensity peak at +15 km s-1, the intensity decreases until +50 km s-1. The profile is similar to that of high-velocity (HV) H2O and CO 16–15, the latter observed simultaneously with [O i]. A radiative transfer analysis suggests that ~15% of the oxygen is in atomic form toward this shock position. The CO abundance is inferred to be ~10-4 by a similar analysis, suggesting that this is the dominant oxygen carrier in the HV component. These results demonstrate that a large portion of the observed [O i] emission is part of the outflow. Further observations are required to verify whether this is a general trend.
Key words: stars: formation / ISM: molecules / ISM: jets and outflows / ISM: individual objects: NGC 1333-IRAS4A R1
© ESO, 2017
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