Hostname: page-component-78c5997874-lj6df Total loading time: 0 Render date: 2024-11-05T05:26:20.206Z Has data issue: false hasContentIssue false
  • English
  • Français

High spatial resolution observations of OH 231.8+4.2

Published online by Cambridge University Press:  15 December 2006

M. Matsuura ,
O. Chesneau ,
A. A. Zijlstra ,
W. Jaffe ,
L. B. F. M. Waters ,
J. A. Yates ,
E. Lagadec  and
T. M. Gledhill
M. Matsuura
Affiliation:
University of Manchester, Sackville Street, P.O. Box 88, Manchester M60 1QD, UK Queen's University of Belfast, Belfast BT7 1NN, Northern Ireland, UK National Astronomical Observatory of Japan, Tokyo 181-8588, Japan email: mikako@optik.mtk.nao.ac.jp
O. Chesneau
Affiliation:
Observatoire de la Côte d'Azur, Department of Gemini-CNRS-UMR 6203, F-06130, Grasse, France
A. A. Zijlstra
Affiliation:
University of Manchester, Sackville Street, P.O. Box 88, Manchester M60 1QD, UK
W. Jaffe
Affiliation:
Leiden Observatory, P.B. 9513, Leiden 2300 RA, The Netherlands
L. B. F. M. Waters
Affiliation:
University of Amsterdam, Kruislaan 403, 1098 SJ, Amsterdam, The Netherlands Katholieke Universiteit Leuven, Celestijnenlaan 200B, 3001 Heverlee, Belgium
J. A. Yates
Affiliation:
University College London, Gower street, London, WC1E 6BT, United Kingdom
E. Lagadec
Affiliation:
University of Manchester, Sackville Street, P.O. Box 88, Manchester M60 1QD, UK
T. M. Gledhill
Affiliation:
Centre for Astrophysics Research, University of Hertfordshire, Hertfordshire AL10 9AB, UK
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 have observed the bipolar post-AGB candidate OH 231.8+4.2, using the mid-infrared interferometer MIDI and the infrared camera with the adaptive optics system NACO on the Very Large Telescope. The NACO images at 2.12 and 3.8 $\mu$m show a bipolar outflow and a flared disk or torus. An unresolved core ($<$200 mas in FWHM) is found at the centre of OH 231.8+4.2 in the 3.8 $\mu$m image. This compact source is resolved with the interferometer. The fringes from the four baselines consistently show the presence of a compact circumstellar material with an inner radius of 30–40 mas, which is equivalent to 40–50 AU at 1.3 kpc. This clearly shows that the mid-infrared compact source is not the central star (3 AU) but circumstellar material.

Keywords

stars: AGB and post-AGB(stars:) circumstellar matterinfrared: starsinfrared: ISMstars: imaging stars: mass loss
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 457 - 458
Copyright
© 2006 International Astronomical Union