Volume 507, Number 2, November IV 2009
|Page(s)||L25 - L28|
|Published online||27 October 2009|
Letter to the Editor
Methyl cyanide as tracer of bow shocks in L1157-B1
INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy e-mail: firstname.lastname@example.org
2 INAF, Istituto di Fisica dello Spazio Interplanetario, via Fosso del Cavaliere 100, 00133 Roma, Italy
3 IRAM, 300 rue de la Piscine, 38406 Saint-Martin-d'Hères, France
4 Department of Physics and Astronomy, University College London, Gower Street, London WC1E6BT, UK
5 Observatorio Astrónomico Nacional (IGN), Alfonso XII, 28014 Madrid, Spain
6 LERMA, UMR 8112 du CNRS, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France
7 Laboratoire d'Astrophysique de l'Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex, France
Accepted: 20 October 2009
Context. L1157-mm is a low-mass protostar driving an outflow which is considered the proto-type of the so-called chemically active outflows. In particular, the blue-shifted lobe B1 stands out for its rich mm-wave spectrum.
Aims. Our aim is to infer the physical conditions of the molecular gas within L1157-B1.
Methods. We carried out CH3CN(8K–7K) observations at 2 mm with the IRAM Plateau de Bure Interferometer to map L1157-B1.
Results. The CH3CN image shows a clumpy structure superimposed to the classical B1 arch-like shape, displaying a unique continuous structure tracing the propagation of a large bow shock. The CH3CN spatial distribution well agrees with that of CH3OH, one of the most abundant species evaporated from dust grain mantles. Thanks to the present CH3CN observations at unprecedented spatial resolution, we determine for the first time the temperature distribution of the B1 bow shock. We obtain values between 57 and 132 K, with the highest temperature at the shock apex, thus confirming the association of CH3CN with gas affected by the passage of a shock wave. The column densities are 8-40 1012 cm-2, depending on the position, leading to CH3CN/CH3OH abundance ratios 0.2-1.3 10-3, i.e. values on average smaller than those found in hot-corinos. This suggests that a significant amount of CH3CN is formed in the gas phase: in the shocked L1157-B1 regions the CH3CN abundance may not have reached its maximum yet.
Key words: ISM: individual objects: L1157 / ISM: molecules / stars: formation
© ESO, 2009
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