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High-resolution Ammonia Mapping of the Protostellar Core Cha-MMS1

Published online by Cambridge University Press:  21 March 2013

Miikka Väisälä ,
Jorma Harju ,
Maarit Mantere ,
Oskari Miettinen  and
Malcolm Walmsley
Miikka Väisälä
Affiliation:
Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Helsinki, Finland email: [email protected]
Jorma Harju
Affiliation:
Finnish Centre for Astronomy with ESO, University of Turku, Väisäläntie 20, FI-21500, Piikkiö, Finland
Maarit Mantere
Affiliation:
Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Helsinki, Finland email: [email protected]
Oskari Miettinen
Affiliation:
Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Helsinki, Finland email: [email protected]
Malcolm Walmsley
Affiliation:
Dublin Institute for Advanced Studies, 10 Burlington Road, Dublin 4, Ireland INAF - Osservatorio Astrofisico di Arcetri, Largo Enrico Fermi 5, I-50125, Firenze, Italia
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Abstract

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The nearby protostellar core Cha-MMS1 has been mapped in the NH3 (1, 1) line and the 1.2 cm continuum using the Australia Telescope Compact Array, ATCA. In addition, observations from Spitzer Space Telescope and Herschel Space Observatory are used to help the interpretation. An elongated condensation with a maximum length of 9000 AU is seen in ammonia. The condensation has a clear velocity gradient directed perpendicularly to the axis of elongation. The gradient can be interpreted as rotation around this axis. We suggest that the observed ammonia structure delineates a rotating envelope and dense gas entrained by a very young protostellar outflow.

Keywords

stars: formation — ISM: clouds — ISM: jets and outflows
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S292: Molecular Gas, Dust, and Star Formation in Galaxies , August 2012 , pp. 61
Copyright
Copyright © International Astronomical Union 2013