| Issue |
A&A
Volume 552, April 2013
|
|
|---|---|---|
| Article Number | L9 | |
| Number of page(s) | 4 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361/201321303 | |
| Published online | 29 March 2013 | |
HH 114 MMS: a new chemically active outflow⋆
1
Observatorio Astronómico Nacional (IGN),
Alfonso XII 3,
28014
Madrid,
Spain
e-mail:
m.tafalla@oan.es
2
Institute for Astrophysics, University of Vienna,
Türkenschanzstrasse 17,
1180
Vienna,
Austria
e-mail:
alvaro.hacar@univie.ac.at
Received: 15 February 2013
Accepted: 12 March 2013
Context. A small group of bipolar protostellar outflows display strong emission from shock-tracer molecules such as SiO and CH3OH, and are generally referred to as “chemically active”. The best-studied outflow from this group is the one in L 1157.
Aims. We study the molecular emission from the bipolar outflow powered by the very young stellar object HH 114 MMS and compare its chemical composition with that of the L 1157 outflow.
Methods. We have used the IRAM 30 m radio telescope to observe a number of transitions from CO, SiO, CH3OH, SO, CS, HCN, and HCO+ toward the HH 114 MMS outflow. The observations consist of maps and a two-position molecular survey.
Results. The HH 114 MMS outflow presents strong emission from a number of shock-tracer molecules that dominate the appearance of the maps around the central source. The abundance of these molecules is comparable to the abundance in L 1157.
Conclusions. The outflow from HH 114 MMS is a spectacular new case of a chemically active outflow.
Key words: stars: formation / ISM: abundances / ISM: jets and outflows / ISM: individual objects: HH 114 MMS / ISM: molecules / radio lines: ISM
© ESO, 2013
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