Hostname: page-component-7c8c6479df-24hb2 Total loading time: 0 Render date: 2024-03-27T16:25:59.488Z Has data issue: false hasContentIssue false

Observational constraints on the formation of interstellar methanol

Published online by Cambridge University Press:  01 February 2008

E. S. Wirström
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, SE-43992 Onsala, Sweden email: eva.wirstrom@chalmers.se
C. M. Persson
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, SE-43992 Onsala, Sweden email: eva.wirstrom@chalmers.se
Å. Hjalmarson
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, SE-43992 Onsala, Sweden email: eva.wirstrom@chalmers.se
J. H. Black
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, SE-43992 Onsala, Sweden email: eva.wirstrom@chalmers.se
P. Bergman
Affiliation:
Onsala Space Observatory, Chalmers University of Technology, SE-43992 Onsala, Sweden email: eva.wirstrom@chalmers.se ESO, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago, Chile
W. D. Geppert
Affiliation:
Physics Department, Stockholm University, S-10691 Stockholm, Sweden
M. Hamberg
Affiliation:
Physics Department, Stockholm University, S-10691 Stockholm, Sweden
E. Vigren
Affiliation:
Physics Department, Stockholm University, S-10691 Stockholm, Sweden
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.

The processes by which methanol, one of the most abundant interstellar organics, is formed in the interstellar medium are not yet accurately known. Pure gas-phase chemistry models fail to reproduce observed abundances by orders of magnitude, pointing to formation on grains and subsequent desorption.

Observations of methanol and its isotopologue 13CH3OH in several sources have been used to trace the origin, and thus the formation routes of methanol on interstellar grains, by means of isotope labelling a posteriori.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Boogert, A. C. A., et al. 2000, A&A, 353, 349Google Scholar
Garrod, R., Park, I. H., Caselli, P., & Herbst, E. 2006, Faraday Discussions, Chemical Evolution of the Universe, 133, 51CrossRefGoogle Scholar
Geppert, W. D., Hamberg, M., Thomas, R. D., et al. 2006, Faraday Discussions, Chemical Evolution of the Universe, 133, 177CrossRefGoogle Scholar
Gibb, E. L., Whittet, D. C. B., Boogert, A. C. A., & Tielens, A. G. G. M. 2004, ApJS, 151, 35CrossRefGoogle Scholar
Langer, W. D., Graedel, T. E., Frerking, M. A., & Armentrout, P. B. 1984, ApJ, 277, 581CrossRefGoogle Scholar
Langer, W. D. & Penzias, A. A. 1990, ApJ, 357, 477CrossRefGoogle Scholar
Nagaoka, A., Watanabe, N., & Kouchi, A. 2005, ApJ (Letters), 624, L29CrossRefGoogle Scholar
Persson, C. M., et al. 2007, A&A, 476, 807Google Scholar
Wada, A., Mochizuki, N., & Hiraoka, K. 2006, ApJ, 644, 300CrossRefGoogle Scholar