Spectral lines of Br and Sb detected in three He-rich white dwarfs.
|Ion||Transition||J− J||λlab /Å||loggifik||Ei/cm−1||RE 0503−289||PG 0109+111||HD 149499 B|
|Br VI||4s2 1S–4s4p 3Po||0–1||945.96||−2.193||0.0||×||×|
|4s4p 1Po–4p2 3P||1–2||981.42||−0.600||151 285.0||×||×|
|Sb V||5s 2S–5p 2Po||1/2–3/2||1104.20||0.052||0.0||×||×|
|Sb VI||5s 3D–5p 3Fo||3–4||999.40||0.440||242 916.8||×|
|5s 3D–5p 3Po||1–0||1043.07||0.520||242 916.8||×|
Notes. Excitation energies Ei for Br VI from Riyaz et al. (2012), for Sb V from Chan (1966), and for Sb VI from Churilov et al. (2000). Oscillator strengths fik for Br VI from Riyaz et al. (2012), for Sb V from Morton (2000). For Sb VI, we used the fik values of the respective lines in the isoelectronic Ge V ion from Rauch et al. (2012). gi is the statistical weight of lower level i. An entry “×” in the last three columns indicates which line was detected in which star.
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