Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La <scp>ii</scp>

Abstract Branching fractions of 86 La ii lines in the spectral range of 243.340–626.229 nm have been measured using a grating spectrometer based on the emission spectra of a lanthanum hollow cathode lamp. Combining these branching fractions with previously measured radiative lifetimes using the time-resolved laser-induced fluorescence technique, transition probabilities and oscillator strengths were determined for 86 lines belonging to transitions 5 d 2 –4 f 5 d , 5 d 6 s –4 f 5 d , 4 f 6 s –5 d 7s, 4 f 5 d –5 d 7s, 5 d 6 p –5 d 7s, 4 f 6 s –5 d 6 d , 4 f 5 d –5 d 6 d , 5 d 6 p –5 d 6 d , 6 s 6 p –5 d 6 d , 4 f 5 d –4 f 2 , and 5 d 6 p –4 f 2 . These fundamental atomic parameters are important for deriving chemical abundances from astronomical spectra by the method of equivalent widths or synthetic spectra.

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Publication Details

Journal
The Astrophysical Journal Supplement Series
Published
2025-05-01
DOI
https://doi.org/10.3847/1538-4365/adc927
Primary Topic
Astrophysics and Star Formation Studies
Type
article
Field-Weighted Citation Impact
0.00

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article

Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La ii

B. J. Liu, Xue Shang, Chunxiao Zhou, Binfang Cao et al.
The Astrophysical Journal Supplement Series
Astrophysics and Star Formation Studies
article

Experimental Branching Fractions, Transition Probabilities, and Oscillator Strengths of La ii

B. J. Liu, Xue Shang, Chunxiao Zhou, Binfang Cao, Naosheng Qiao
article en

Abstract

Abstract Branching fractions of 86 La ii lines in the spectral range of 243.340–626.229 nm have been measured using a grating spectrometer based on the emission spectra of a lanthanum hollow cathode lamp. Combining these branching fractions with previously measured radiative lifetimes using the time-resolved laser-induced fluorescence technique, transition probabilities and oscillator strengths were determined for 86 lines belonging to transitions 5 d 2 –4 f 5 d , 5 d 6 s –4 f 5 d , 4 f 6 s –5 d 7s, 4 f 5 d –5 d 7s, 5 d 6 p –5 d 7s, 4 f 6 s –5 d 6 d , 4 f 5 d –5 d 6 d , 5 d 6 p –5 d 6 d , 6 s 6 p –5 d 6 d , 4 f 5 d –4 f 2 , and 5 d 6 p –4 f 2 . These fundamental atomic parameters are important for deriving chemical abundances from astronomical spectra by the method of equivalent widths or synthetic spectra.

The Astrophysical Journal Supplement SeriesVol. 278(1)
Hunan University of Arts and Science (CN), Anhui East China Institute of Optoelectronic Technology (China) (CN)
National Natural Science Foundation of China, Hunan University
Openalex Percentile: Top 93%
Astrophysics and Star Formation Studies
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