A&A 438, 743-744 (2005)

DOI: 10.1051/0004-6361:20053312e

*Erratum*

**O. Zatsarinny ^{1} - T. W. Gorczyca^{1} - K. T.
Korista^{1} - J. Fu^{1} - N. R. Badnell^{2} - W. Mitthumsiri^{3} - D. W. Savin^{3}**

1 - Department of Physics, Western Michigan University,
Kalamazoo, MI 49008, USA

2 -
Department of Physics, University of Strathclyde,
Glasgow G4 0NG, UK

3 -
Columbia Astrophysics Laboratory, Columbia University, New York, NY 10027, USA

A&A, 412, 587-595 (2003), DOI: 10.1051/0004-6361:20031462

**Key words: **atomic data - atomic processes - plasmas - errata, addenda

Mistakes in an earlier publication (Zatsarinny et al. 2003) have been discovered and are corrected below (in boldface). The first is a missing exponent in an equation, the second is some wrong fitting coefficients for several ions, the third and fourth are an incorrect caption and an incorrect label in a figure, and the fifth is an inaccuracy in high-temperature radiative recombination rate coefficients.

In Eq. (4), we inadvertently omitted an exponent of 1+*b* in the second parenthesized term in the square brackets. The correct equation should read

The original RR fitting coefficients are correct and are applicable to this corrected Eq. (4).

In Table 1, some of the DR fitting coefficients are incorrect
due to initially undetected human errors in the postprocessing of
the atomic data. As a result, we have refitted our archived totals for the entire sequence
using up to seven terms in the summation of Eq. (3). We have retabulated in Table 1 only results for those ions that showed significant differences, which occur at lower temperatures,
from those of our initial fitting procedure. We emphasize that these
few errors were not in the atomic physics calculations, which are
accurate for the entire sequence i.e. the *adf09* files are unchanged,
but rather only in the fitting algorithm.

In Fig. 4, there were two typographical errors. First, in
Fig. 4a, the caption states that the rate coefficients shown are
for
DR, that is, from all
states;
in fact, what has been plotted is DR only to the
*n*>3states. This does not affect our conclusion that even though
DR does not scale smoothly along an isoelectronic sequence,
DR does.
Second, in Fig. 4b, the labels for Na^{3+} and Al^{5+} were erroneously
interchanged and should be reversed.

Finally, we have discovered that the electron energy range over which our photoionization
cross sections were calculated was accidentally restricted. Thus, the extrapolation
of the cross sections to higher energies before convolution with a Maxwellian distribution
to form RR rate coefficients was applied at much lower energies than usual and before
it was accurate to do so. Consequently, the *T*^{-3/2} asymptotic behaviour of the RR rate
coefficient comes in at too low a temperature. Thus, our fitting coefficients for RR should
not be used for
eV, where *Z* is the residual charge of the electron target.
This limited temperature region of validity also is the case
for our earlier RR work on the C-like (Zatsarinny et al. 2004a) and Ne-like (Zatsarinny et al. 2004b) sequences.

**Table 1:**
Fitting coefficients of Eq. (3) for dielectronic recombination of selected O-like ions forming F-like systems. The *c*_{i} are in units of 10^{-11} cm^{3} s^{-1} eV^{1.5} and
the *E*_{i} are in eV.

- Zatsarinny, O., Gorczyca, T. W., Korista, K., Badnell, N. R., & Savin, D. W. 2003, A&A, 412, 587 [EDP Sciences] [NASA ADS] [CrossRef] (In the text)
- Zatsarinny, O., Gorczyca, T. W., Korista, K., Badnell, N. R., & Savin, D. W. 2004a, A&A, 417, 1173 [EDP Sciences] [NASA ADS] [CrossRef] (In the text)
- Zatsarinny, O., Gorczyca, T. W., Korista, K., Badnell, N. R., & Savin, D. W. 2004b, A&A, 426, 699 [EDP Sciences] [NASA ADS] [CrossRef] (In the text)

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