Hostname: page-component-84b7d79bbc-g78kv Total loading time: 0 Render date: 2024-07-30T01:05:44.572Z Has data issue: false hasContentIssue false
  • English
  • Français

OH and H2O Maser Distribution in Orion KL

Published online by Cambridge University Press:  12 April 2016

S. Horiuchi  and
V. Migenes
S. Horiuchi
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan
V. Migenes
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181, Japan

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.

In order to study the powering source behind KL nebula, we made a map of OH and H2O masers from VLA observations of this region, and compared their spatial distribution and velocity structure with that of the SiO masers. The distribution of the OH masers consists of a multi-stream structure and seems to be related to the Hot Core molecular emission. The low velocity H2O masers may be classified as two groups: i) an inner clump of maser spots surrounding the SiO maser disc and continuum source “I”, and ii) component associated with the Hot Core represented by HDO emission peaks.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 164: Radio Emission from Galactic and Extragalactic Compact Sources , 1998 , pp. 373 - 374
Copyright
Copyright © Astronomical Society of the Pacific 1998

References

Genzel, R. et al. 1981. ApJ, 244, 884–902.CrossRefGoogle Scholar
Menten, K.M., & Reid, M.J. 1995. ApJ, 445, L157–160.Google Scholar
Plambeck, R.L., & Wright, M.C.H. 1987. ApJ, 317, L101–105.Google Scholar
Plambeck, R.L., Wright, M.C.H., & Carlstrom, J.E. 1990. ApJ, 348, L65–68.Google Scholar