Energy levels, wavelengths, transition probabilities
Atomic data for permitted resonance lines of atoms and
ions from H to Si, and S, Ar, Ca and Fe.
Abstract. We list vacuum wavelengths, energy levels, statistical
weights, transition probabilities and oscillator strengths for permitted
resonance spectral lines of all ions of 18 astrophysically important elements
(H through Si, S, Ar, Ca, Fe). Using a compilation of experimental energy
levels, we derived accurate wavelengths for 5599 lines of 1828 ground-term
multiplets which have gf-values calculated in the Opacity Project. We recalculated
the Opacity Project multiplet gf-values to oscillator strengths and transition
probabilities of individual lines. For completeness, we added 372 resonance
lines of NeI, ArI, FeI and FeII ions which are not covered by the Opacity
Project. Intercombination and forbidden lines are not included in the present
D. A. Verner, E. M. Verner, and G. J. Ferland, 1996, Atomic Data Nucl.
Data Tables, 64, 1
PostScript files: Text
(88.2 K), Tables
A and B (24.7 K), Figure
1 (12.9 K).
of Tables 1 and 2 (3.0 K).
Table 1. Wavelengths and Oscillator Strengths of Permitted Resonance
Absorption Lines. ASCII
(941.8 K), PostScript
Table 2. Finding List of Lines. ASCII
(179.1 K), PostScript
Atomic data for absorption lines from the ground level at wavelengths greater
than 228 A.
Abstract. We list wavelengths, statistical weigths and oscillator
strengths for 2249 spectral lines arising from the ground states of atoms
and ions. The compilation covers all wavelengths longward of the He II
Lyman limit at 227.838 A and all the ion states of all elements from hydrogen
to bismuth (Z=83) for which reliable data are known. We assign experimental
wavelengths to 1086 lines which have oscillator strengths calculated in
the Opacity Project, and add 1163 lines which have critically evaluated
oscillator strengths from previous compilations. The presented data are
to be used for quasar absorption spectra interpretation. We use solar abundances
to calculate the expected relative strengths of all absorption lines, and
list separately the strongest lines above 228 A expected in QSO absorption
systems, many of which are listed here for the first time. The great majority
of strong lines expected in quasar spectra are at \lambda < 912 A. We
also list the strongest absorption lines of various ions without wavelength
D. A. Verner, P. D. Barthel, & D. Tytler. 1994, A&AS, 108, 287
file 36.0 K, PostScript
file 133.1 K (text only), Description
of tables (6.7 K).
Table 1. Strong lines above 228 A expected in quasar absorption
(3.4 K), PostScript
Table 2. Strongest lines above 228 A without experimental wavelengths.
ASCII (3.0 K),
Table 3. Atomic weights and solar-system abundances. ASCII
(2.2 K), PostScript
Table 4. Ionization thresholds and strongest lines of atoms and
ions. ASCII (51.3
Table 5. Resonance absorption lines above 228 A ordered by element.
Table 6. Resonance absorption lines above 228 A ordered by wavelength.
Atomic Line Database compiled by Peter
Kurucz line list. Search
Kelly line list. Search
Atomic data for resonance absorption lines. Morton
Observed lines and lines in the CHIANTI database between
50 and 1100 A Dere
et al. 1997
Line energy catalog. Kallman
Elemental edge energies. Kallman
Atomic spectral lines data OII, Mg, Al, S, Sc. Martin
et al. II
Atomic transition probabilities, Sc to Ni. Martin
et al. III
Electron binding energies. Williams
C and O isoelectronic sequences, forbidden trasitions. Galavis
et al. 1997
C II, C III, and C IV, high-nl Rydberg states.
O VIII and Fe XVII, atomic data for resonance lines and their satellites.
et al. 1994
Fe II, semiempirical gf values. Kurucz
Fe II, allowed transition probabilities. Nahar
Fe III, wavelengths and transition probabilities. Ekberg
Fe III, transition probabilities for forbidden lines.
Fe XXIV and XXV, fine structure oscillator strengths.
& Pradhan 1999
Co II, transition probabilities for forbidden lines.
Ni I and Ni II, transition probabilities for forbidden
& Le Dourneuf 1996
As II and Tl II, wavelengths and gf values. The
Dima Verner (firstname.lastname@example.org)
Last updated: 1996 November 12
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