14 research outputs found
Maser action in methanol transitions
We report the detection with the ATCA of 6.7 GHz methanol emission towards
OMC-1. The source has a size between 40'' and 90'', is located to the
south-east of Ori-KL and may coincide in position with the 25 GHz masers. The
source may be an example of an interesting case recently predicted in theory
where the transitions of traditionally different methanol maser classes show
maser activity simultaneously. In addition, results of recent search for
methanol masers from the 25 and 104.3 GHz transitions are reported.Comment: To appear in the Proceedings of the 2004 European Workshop: "Dense
Molecular Gas around Protostars and in Galactic Nuclei", Eds. Y.Hagiwara,
W.A.Baan, H.J. van Langevelde, 2004, a special issue of ApSS, Kluwer; author
list has been corrected, text is unchange
Model of the W3(OH) environment based on data for both maser and 'quasi-thermal' methanol lines
In studies of the environment of massive young stellar objects, recent
progress in both observations and theory allows a unified treatment of data for
maser and 'quasi-thermal' lines. Interferometric maser images provide
information on the distribution and kinematics of masing gas on small spatial
scales. Observations of multiple masing transitions provide constraints on the
physical parameters.
Interferometric data on 'quasi-thermal' molecular lines permits an
investigation of the overall distribution and kinematics of the molecular gas
in the vicinity of young stellar objects, including those which are deeply
embedded. Using multiple transitions of different molecules, one can obtain
good constraints on the physical and chemical parameters.
Combining these data enables the construction of unified models, which take
into account spatial scales differing by orders of magnitude.
Here we present such a combined analysis of the environment around the
ultracompact HII region in W3(OH). This includes the structure of the methanol
masing region, physical structure of the near vicinity of W3(OH), detection of
new masers in the large-scale shock front and embedded sources in the vicinity
of the TW young stellar object.Comment: To appear in the Proceedings of the 2004 European Workshop: "Dense
Molecular Gas around Protostars and in Galactic Nuclei", Eds. Y.Hagiwara,
W.A.Baan, H.J. van Langevelde, 2004, a special issue of ApSS, Kluwe
Supernova Interaction with a Circumstellar Medium
The explosion of a core collapse supernova drives a powerful shock front into
the wind from the progenitor star. A layer of shocked circumstellar gas and
ejecta develops that is subject to hydrodynamic instabilities. The hot gas can
be observed directly by its X-ray emission, some of which is absorbed and
re-radiated at lower frequencies by the ejecta and the circumstellar gas.
Synchrotron radiation from relativistic electrons accelerated at the shock
fronts provides information on the mass loss density if free-free absorption
dominates at early times or the size of the emitting region if synchrotron
self-absorption dominates. Analysis of the interaction leads to information on
the density and structure of the ejecta and the circumstellar medium, and the
abundances in these media. The emphasis here is on the physical processes
related to the interaction.Comment: 22 pages, 7 figures, to appear as a Chapter in "Supernovae and
Gamma-Ray Bursts," edited by K. W. Weiler (Springer-Verlag