1. This release corrects the wavelengths for the Ni L-shell lines. Wavelength errors are given for lines directly obtained from the NIST compilation of Shirai et al. (2000).
2. Ni L-shell data are scaled from Fe L-shell data. The energy scaling now preserves the energy order and matches the energies derived from the observed wavelengths in the NIST database.
3. Additional energy levels, and corresponding emission lines, are added for Li-like ions, bringing them up from principal quantum number n=5 to n=7. Ions which are now complete up to n=7 are Li-like Ne, Mg, Si, S, Ar, Ca, Ni, and Fe.
4. Accurate wavelengths are also included for Li-like Ne VIII, Mg X, Si XII, and S XIV from the new NIST compilations of Podobedova et al. (2002, private communication). Wavelength errors are not yet available for all the compiled data; for the observed lines from the NIST group we have used 0.003 A as the estimated error, on recommendation from the NIST group.
5. We've included many more references, using the ADS bibcode format for these new references, many of which can be immediately downloaded from ADS.
6. The wavelengths of Al XIII used in v1.1.0 were effectively redshifted by 0.05 Angstroms due to a typing error. We have fixed this problem, and thank Rachel Osten for bringing it to our attention.
7. Dielectronic recombination (DR) satellite lines of Fe XVII have had their upper level index changed to a number larger than 9999. Previously, values over 999 were used leading to confusion between autoionizing levels and bound levels for Fe XVII. Thanks to Jan-Uwe Ness for alerting us of this.
1. We have very little data on the delta n >= 1 transitions from L-shell ions of Ne, Mg, Al, Si, S, Ar, or Ca, with the exception of Lithium-like ions. X-rays from these lines are largely below 0.25 keV, and as a result, our spectral calculations in this range are very deficient. We are working on this problem.
2. Only for some of the strongest lines do we include lines from levels above n=5.
3. Few innershell transitions are included. This primarily affects the so-called iron K-alpha line, which is actually a large number of lines arising from a K-shell hole in an Fe I-Fe XXIV ion. We are also missing some inner shell excitation transitions, for example from Fe XVI, and O VI. We expect to include these data in the next release.
4. These models are derived from theoretical atomic data for which few experimental measurements have been made. Most emissivities are thought to be good to better than 30 percent; however, larger discrepancies are being found in some caes, likely the result of incomplete atomic physics. Such cases are under investigation as part of the Emission Line Project.
5. We note that the line ratio of Fe XVII 15.014 to Fe XVII 15.261 is about 15 to 20 percent larger than the measured ratio (see Brown et al. 1998, ApJ, 502, 1015). While the discrepancy is within our expected uncertainties, it is quite likely that this discrepancy will be noticeable even at moderate (CCD) resolution.
PLEASE NOTE: prior to the ATOMDB v1.2.0 release, the ATOMDB files contained the version number. With the v1.2.0 release, we set up links from a canonical name for the files to the currently-released version. This makes future updates easier. However, the releases of GUIDE, Sherpa and XSPEC at the time of the ATOMDB v1.2.0 release expected to find the data in files containing the old (version 1.1.0) filename. We therefore re-used the old filenames, linking them to the new release. This admittedly confusing situation was remedied with the CIAO 2.3 release on 12 November 2002.