Hostname: page-component-78c5997874-ndw9j Total loading time: 0 Render date: 2024-11-11T02:26:35.476Z Has data issue: false hasContentIssue false
  • English
  • Français

Nebular emission lines in IRAS 17347–3139

Published online by Cambridge University Press:  15 December 2006

F. M. Jiménez-Esteban ,
J. V. Perea-Calderón ,
O. Suárez ,
M. Bobrowsky  and
P. García-Lario
F. M. Jiménez-Esteban
Affiliation:
Hamburger Sternwarte, Hamburg, Germany email: francisco.jimenez-esteban@hs.uni-hamburg.de
J. V. Perea-Calderón
Affiliation:
European Space Astronomy Centre (ESAC), Madrid, Spain
O. Suárez
Affiliation:
Laboratorio de Astrofísica Espacial y Física Fundamental-INTA, Madrid, Spain
M. Bobrowsky
Affiliation:
Computer Science Corporation/Space Telescope Science Institute, Baltimore MD, USA
P. García-Lario
Affiliation:
ESAC, Research and Scientific Support Deparment of ESA, Madrid, Spain
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We report the detection of nebular emission lines in the optical and mid-infrared spectra of IRAS 17347–3139, a heavily obscured OH/IR star which may be rapidly evolving from the AGB to the PN stage. The presence of emission lines is interpreted as a clear indication that the ionization of its circumstellar envelope has already started. This source belongs to the rare class of objects known as ‘OHPNe’ displaying both OH maser and radio continuum emission. However, unlike the rest of stars in this class, prominent C-rich dust features are detected in its mid-infrared spectrum, which makes the analysis of this star particularly interesting.

Keywords

stars: AGB and post-AGB
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 437 - 438
Copyright
© 2006 International Astronomical Union