从HR 6000和46 Aql的UVES光谱中新识别的Fe II的（3 H）4d -（3 H）4f跃迁
New identified (3H)4d - (3H)4f transitions of Fe II from UVES spectra of HR 6000 and 46 Aql
摘要：
对CP星HR 6000和46 Aql的高分辨率UVES光谱的分析揭示了大量未识别线的存在，特别是在5000 - 5400 A区域。由于大量的4d-4f跃迁的铁II位于这个光谱范围内，因为这两颗星都是铁过剩，我们调查了是否未识别的线可以是由于铁II。分别计算了HR 6000和46 Aql各自丰度的ATLAS 12模型大气参数[13450 K，4.3]和[12560 K，3.8]，以便使用恒星作为光谱源来识别Fe II线并确定Fe II gf值。在确定了恒星光谱中的几条未知谱线是由于Fe II的（3 H）4d -（3 H）4f跃迁引起的之后，我们通过比较观测和计算的轮廓来推导出它们的恒星对数GF。根据实验室铁谱和预测的能级，对上能级的能量进行了归属。我们确定了Fe Ⅱ的21个新能级，能量在122910.9 cm^-1和123441.1 cm^-1之间。它们使我们能够在Fe II谱线列表中增加1700条810 - 15011 A范围内的新谱线。
英文摘要：
The analysis of the high-resolution UVES spectra of the CP stars HR 6000 and 46 Aql revealed the presence of an impressive number of unidentified lines, in particular in the 5000 - 5400 A region. Because numerous 4d-4f transitions of FeII lie in this spectral range, and because both stars are iron overabundant, we investigated whether the unidentified lines can be due to FeII. ATLAS12 model atmospheres with parameters [13450K, 4.3] and [12560K, 3.8] were computed for the individual abundances of HR 6000 and 46 Aql, respectively, in order to use the stars as spectroscopic sources to identify FeII lines and to determine FeII gf-values. After having identified several unknown lines in the stellar spectra as due to (3H)4d - (3H)4f transitions of FeII, we derived stellar log gf's for them by comparing observed and computed profiles. The energies of the upper levels were assigned on the basis of both laboratory iron spectra and predicted energy levels. We fixed 21 new levels of FeII with energies between 122910.9 cm^-1 and 123441.1 cm^-1. They allowed us to add 1700 new lines to the Fe II line list in the range 810 - 15011 A.
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