Free Access
Astron. Astrophys. Suppl. Ser.
Volume 137, Number 1, May II 1999
Page(s) 157 - 163
Published online 15 May 1999
DOI: 10.1051/aas:1999242

Astron. Astrophys. Suppl. Ser. 137, 157-163

Recombination coefficients for the 5g - 4f transitions of OIII at nebular temperatures and densities[*]

R. Kisielius - P.J. Storey

Send offprint request: P.J. Storey

Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

Received February 1; accepted February 22, 1999


We calculate effective recombination coefficients for the formation of the 5g - 4f lines of OIII in the intermediate coupling scheme. Photoionization data for the 5g levels calculated using the R-matrix method are used to derive their recombination coefficients. Cascading from higher states is included, allowing for the effects of finite electron density in a hydrogenic approximation. We explicitly include the distribution of population between the two ground levels of O3+ in the calculation of the line intensities. The results are presented as a simple programmeable formula allowing the calculation of recombination line intensities for electron temperatures, $T_{\mathrm e}$ in the range $5000~-~20\,000$ K and electron densities, $N_{\mathrm e}$ in the range 102-106 cm-3.

Key words: atomic data -- atomic processes -- line: formation -- ISM: H II regions -- ISM: planetary nebulae: general

Tables at the CDS

Copyright The European Southern Observatory (ESO)

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.