| Issue |
A&A
Volume 395, Number 1, November III 2002
|
|
|---|---|---|
| Page(s) | 223 - 226 | |
| Section | The Sun | |
| DOI | https://doi.org/10.1051/0004-6361:20021237 | |
| Published online | 29 October 2002 | |
An upper limit to the interstellar 
abundance in translucent clouds*
1
Special Astrophysical Observatory, Nizhnij Arkhyz 369167, Russia e-mail: faig@sao.ru
2
Center for Astronomy, Nicholas Copernicus University, Gagarina 11, 87-100 Toruń, Poland e-mail: jacek@astri.uni.torun.pl
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: glocurto@eso.org
Corresponding author: J. Krełowski, gala@sao.ru
Received:
26
June
2002
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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