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Magellanic Diffuse Interstellar Bands and Carbon Chemistry

Published online by Cambridge University Press:  30 March 2016

P. Ehrenfreund ,
N. Cox ,
J. Cami ,
B.H. Foing ,
L. Kaper ,
L. d’Hendecourt ,
J.P. Maier ,
F. Salama ,
P. Sarre  and
T. Snow
...Show all authors
P. Ehrenfreund
Affiliation:
Leiden Observatory, P O Box 9513, 2300 RA Leiden, Netherlands
N. Cox
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands
J. Cami
Affiliation:
Space Science Division, NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035, USA
B.H. Foing
Affiliation:
Research Support Division, ESA, ESTEC SCI-SR, 2200 AG Noordwijk, Netherlands
L. Kaper
Affiliation:
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, Netherlands
L. d’Hendecourt
Affiliation:
Institut d’Astrophysique Spatiale, Campus d’Orsay, 91405 Orsay, France
J.P. Maier
Affiliation:
Institute for Physical Chemistry, Klingelbergstrasse 80, University of Basel CH-4053, Switzerland
F. Salama
Affiliation:
Space Science Division, NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035, USA
P. Sarre
Affiliation:
School of Chemistry, University of Nottingham, University Park, Nottingham NG7 2RD, UK
T. Snow
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado at Boulder, 389 UCB, Boulder, CO 80309-0389, USA
P. Sonnentrucker
Affiliation:
Department of Physics and Astronomy, Johns Hopkins University, Charles and 34th Street, Bloomberg Center, Baltimore, MD 21218-2686, USA

Abstract

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With the Ultraviolet Visual Echelle Spectrograph mounted at the Very Large Telescope, we have observed at unprecedented spectral resolution the absorption spectrum toward reddened stars in the Magellanic Clouds over the wavelength range of 3500-10500 Å. This range covers the strong transitions associated with neutral and charged large carbon molecules of varying sizes and structures. We report the first detection of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the Small Magellanic Cloud and the variation of those DIBs toward several targets in the Large Magellanic Cloud. The variation of DIBs in the Magellanic Clouds compared with Galactic targets may be governed by a combination of the different chemical processes prevailing in low-metallicity regions and the local environmental conditions. The analysis of high-resolution absorption spectra allows us to reveal the global effects in the chemistry and recycling of cosmic dust in the Magellanic Clouds which are relevant for the chemical pathways forming large organic molecules in external galaxies.

Type
I. Joint Discussions
Information
Highlights of Astronomy , Volume 13 , 2005 , pp. 864 - 866
Copyright
Copyright © Astronomical Society of Pacific 2005

References

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