Evidence supporting the kinematic interpretation of water maser proper motions

Free access article

Issue		A&A Volume 447, Number 2, February IV 2006


Page(s)		L9 - L12
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:200500230

A&A 447, L9-L12 (2006)
DOI: 10.1051/0004-6361:200500230

Letter

Evidence supporting the kinematic interpretation of water maser proper motions

C. Goddi¹, L. Moscadelli¹, J. M. Torrelles², L. Uscanga³ and R. Cesaroni⁴

¹ INAF, Osservatorio Astronomico di Cagliari, Loc. Poggio dei Pini, Str. 54, 09012 Capoterra (CA), Italy
e-mail: cgoddi@ca.astro.it
² Instituto de Ciencias del Espacio (CSIC)-IEEC, Gran Capitá 2, 08034 Barcelona, Spain
³ Instituto de Astronomía, UNAM, Apdo. Postal 70-264, 04510 México, D.F., México
⁴ INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy

(Received 7 December 2005 / Accepted 21 December 2005)

Abstract
We have analyzed multi-epoch 22 GHz water maser observations performed with the Very Long Baseline Array (VLBA) towards the high-mass star forming region (SFR) G24.78+0.08. The spatial structure of the water maser integrated intensity has been obtained at three different epochs and found to maintain a very remarkable persistent morphology over the three epochs. Evidence of systematic (expanding) motions for the whole structure traced by the maser emission is also reported. In addition, we have obtained, from previously reported data, the integrated emission of a cluster of water masers spread over $\simeq$ 10 mas within the expanding shell of $\simeq$ 0.16'' size around the young stellar object W75 N (B)-VLA 2. As in G24.78+0.8, we also find that the morphology of the integrated intensity of the water masers of this cluster persists over different observed epochs. These results strongly support the interpretation that the measured proper motions of the water masers are due to real physical motions of distinct blobs of maser-emitting gas, rather than to other effects, such as a travelling background illuminating wave or turbulence in the circumstellar medium. This result is crucial in astrophysical applications of maser proper-motion measurements, including distance determinations and studies of circumstellar gas kinematics in SFRs and late-type stars.

Key words: masers -- stars: formation -- ISM: kinematics and dynamics

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