Volume 395, Number 1, November III 2002
|Page(s)||223 - 226|
|Published online||29 October 2002|
An upper limit to the interstellar abundance in translucent clouds*
Special Astrophysical Observatory, Nizhnij Arkhyz 369167, Russia e-mail: email@example.com
2 Center for Astronomy, Nicholas Copernicus University, Gagarina 11, 87-100 Toruń, Poland e-mail: firstname.lastname@example.org
3 Isaac Newton Institute of Chile, SAO Branch, Russia
4 Laboratorie d'Astrophysique de Marseille, Traverse du Siphon, Les trois Lucs, BP 8, 13376 Marseille Cedex 12, France e-mail: Claire.Moutou@oamp.fr
5 European Southern Observatory, Alonso de Cordova 3107 – Vitacura, Santiago, Chile e-mail: email@example.com
Corresponding author: J. Krełowski, firstname.lastname@example.org
Accepted: 27 August 2002
We have analyzed high resolution spectra of several slightly to moderately reddened stars collected at two observatories: ESO (La Silla) and Terskol (Northern Caucasia), to estimate the abundance of the C5 molecule in the interstellar medium. We confirm the presence of a feature near 4975 Å which appears to be a weak DIB rather than the predicted C5 band since the origin band near 5109 Å remains invisible even in spectra of high signal–to–noise ratio (~2500) and spectral resolution (). This confirms that the C5 abundance in translucent interstellar clouds is very low. We estimate its limit as low as 1011 cm-2 in the scale for “zeta" type objects that is two times lower than that of Maier et al. (2002).
Key words: ISM: clouds / molecules
© ESO, 2002
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