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VLBI maser kinematics in high-mass SFRs: G23.01–0.41

Published online by Cambridge University Press:  24 July 2012

Alberto Sanna ,
Luca Moscadelli ,
Riccardo Cesaroni  and
Ciriaco Goddi
Alberto Sanna
Affiliation:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany email: [email protected]
Luca Moscadelli
Affiliation:
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy email: [email protected]; [email protected]
Riccardo Cesaroni
Affiliation:
INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy email: [email protected]; [email protected]
Ciriaco Goddi
Affiliation:
European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching bei München, Germany email: [email protected]
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Abstract

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Very Long Baseline Interferometry studies of different maser species observed at multiple epochs allow complementary measurements of the 3-dimensional velocity field of gas close (≲ 103 AU) to massive young stellar objects. Here, we review our recent results toward the high-mass star-forming region G23.01–0.41, where all the strongest molecular maser transitions known to date cluster within 2000 AU from the center of an hot molecular core and are associated with a so called extended green object. The overall maser kinematics reveals a common outflowing motion from a central object; the details of the spatial distribution and velocity field of each maser species hint at the presence of different dynamical structures: a collimated jet, a wide-angle wind, and a flattened rotating core. We further compare the simultaneous presence of maser emission from different molecular species with a recent evolutionary sequence for masers associated with massive young stellar objects.

Keywords

maserstechniques: high angular resolutionstars: formationstars: individual (G23.01–0.41)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S287: Cosmic Masers - from OH to H0 , January 2012 , pp. 396 - 400
Copyright
Copyright © International Astronomical Union 2012

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