Energy levels, wavelengths, transition probabilities

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Atomic data for permitted resonance lines of atoms and ions from H to Si, and S, Ar, Ca and Fe.
D. A. Verner, E. M. Verner, and G. J. Ferland, 1996, Atomic Data Nucl. Data Tables, 64, 1

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 compilation.
PostScript files: Text (88.2 K), Tables A and B (24.7 K), Figure 1 (12.9 K).
Description of Tables 1 and 2 (3.0 K).

Atomic data for absorption lines from the ground level at wavelengths greater than 228 A.
D. A. Verner, P. D. Barthel, & D. Tytler. 1994, A&AS, 108, 287

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 restriction.
LaTeX file 36.0 K, PostScript file 133.1 K (text only), Description of tables (6.7 K).

Atomic Line Database compiled by Peter van Hoof.

Other sites:

NIST. Atomic Spectroscopic Database

Atomic spectral line list. Hirata & Horaguchi 1995

Semiempirical gf values. Kurucz & Peytremann 1975

Kurucz line list. Search

Kelly line list. Search

Line spectra of the elements. Reader & Corliss 1980-81

ILLSS catalogue. Coluzzi 1993

UVILLSS catalogue. Coluzzi 1996

Finding list for multiplet tables. Adelman et al. 1985

Atomic data for resonance absorption lines. Morton 1991

Observed lines and lines in the CHIANTI database between 50 and 1100 A Dere et al. 1997

Line energy catalog. Kallman I

Elemental edge energies. Kallman II

Atomic energy level data. Martin et al. I

Atomic spectral lines data OII, Mg, Al, S, Sc. Martin et al. II

Atomic transition probabilities, Sc to Ni. Martin et al. III

X-ray emission lines. Bearden 1967

Electron binding energies. Williams 1995

C and O isoelectronic sequences, forbidden trasitions. Galavis et al. 1997

C II, C III, and C IV, high-nl Rydberg states. Quinet 1998

O VIII and Fe XVII, atomic data for resonance lines and their satellites. Cornille et al. 1994

S I, oscillator strengths. Biemont et al. 1993

Mn I, a multiplet table. Adelman et al. 1985

Mn III, transition probabilities. Uylings & Raassen 1997

Fe I, multiplet tables. Nave et al. 1994

Fe I, highly-excited levels. Nave & Johansson 1993

Fe II, semiempirical gf values. Kurucz 1981

Fe II, allowed transition probabilities. Nahar 1995

Fe II, forbidden transition probabilities. Quinet, Le Dourneuf, & Zeippen 1996

Fe III, wavelengths and transition probabilities. Ekberg 1993

Fe III, transition probabilities. Nahar & Pradhan 1996

Fe III, transition probabilities for forbidden lines. Quinet 1996

Fe XXIV and XXV, fine structure oscillator strengths. Nahar & Pradhan 1999

Co II, oscillator strengths. Raassen et al. 1998

Co II, transition probabilities for forbidden lines. Quinet 1998

Ni I and Ni II, transition probabilities for forbidden lines. Quinet & Le Dourneuf 1996

As II and Tl II, wavelengths and gf values. The SAM project

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Last updated: 1996 November 12
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