EDP Sciences
Free access
Volume 495, Number 1, February III 2009
Page(s) 189 - 194
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:200810348
Published online 14 January 2009
A&A 495, 189-194 (2009)
DOI: 10.1051/0004-6361:200810348

Observational test of the CH cation oscillator strengths

T. Weselak1, G. A. Galazutdinov2, F. A. Musaev3, Y. Beletsky4, and J. Krełowski5

1  Institute of Physics, Kazimierz Wielki University, Weyssenhoffa 11, 85-072 Bydgoszcz, Poland
    e-mail: towes@gazeta.pl
2  Korea Astronomy and Space Science Institute, Optical Astronomy Division, 61-1, Hwaam-Dong, Yuseong-Gu, Daejeon, 305-348, Korea
    e-mail: gala@kasi.re.kr
3  Special Astrophysical Observatory, Nizhnij Arkhyz, 369167, Russia
    e-mail: faig@sao.ru
4  European Southern Observatory (ESO), Alonso de Cordova 3107, Santiago, Chile
    e-mail: ybialets@eso.org
5  Center for Astronomy, Nicolaus Copernicus University, Gagarina 11, 87-100 Toruń, Poland
    e-mail: jacek@astri.uni.torun.pl

Received 9 June 2008 / Accepted 21 November 2008

We revise measurements of the positions and oscillator strengths using spectral features in the CH+ A-X system, and by using high-resolution, echelle spectra of 36 stars and assuming that its wavelength and oscillator strength as given in the literature for the (0, 0) transition, i.e. 4232.548 Å and 0.00545 respectively, are correct. The recommended oscillator strengths of the lines at 3957.689, 3745.308, 3579.024, and 3447.077 Å are found to be (in units of 10-5) 342, 172, 75, and 40, respectively. The estimated column densities of the CH cation toward the observed targets are also presented.

Key words: ISM: molecules -- ISM: abundances

© ESO 2009