Ward J W, Raassen A J J, Kramida A, Nave G
National Institute of Standards and Technology, Gaithersburg, MD 20899-8422, USA.
University of Maryland College Park, College Park, MD 20742, USA.
Astrophys J Suppl Ser. 2019;245(2). doi: 10.3847/1538-4365/ab4ea3.
This work presents 97 remeasured Fe V wavelengths (1200-1600 Å) and 123 remeasured Ni V wavelengths (1200-1400 Å) with uncertainties of approximately 2 mÅ. An additional 67 remeasured Fe V wavelengths and 72 remeasured Ni V wavelengths with uncertainties greater than 2 mÅ are also reported. A systematic calibration error is also identified in the previous Ni V wavelengths and is corrected in this work. Furthermore, a new energy level optimization of Ni V is presented that includes level values as well as Ritz wavelengths. This work improves upon the available data used for observations of quadruply ionized nickel (Ni V) in white dwarf stars. This compilation is specifically targeted toward observations of the G191-B2B white dwarf spectrum that has been used to test for variations in the fine structure constant, , in the presence of strong gravitational fields. The laboratory wavelengths for these ions were thought to be the cause of inconsistent conclusions regarding the variation limit of as observed through the white dwarf spectrum. These inconsistencies can now be addressed with the improved laboratory data presented here.
这项工作给出了97条重新测量的铁V波长（1200 - 1600 Å）和123条重新测量的镍V波长（1200 - 1400 Å），不确定度约为2 mÅ。还报告了另外67条重新测量的铁V波长和72条重新测量的镍V波长，其不确定度大于2 mÅ。在先前的镍V波长中还识别出了系统校准误差，并在本工作中进行了校正。此外，还给出了镍V的新能级优化结果，包括能级值以及里兹波长。这项工作改进了用于观测白矮星中四重电离镍（Ni V）的现有数据。该汇编专门针对G191 - B2B白矮星光谱的观测，该光谱已被用于在强引力场存在的情况下测试精细结构常数α的变化。这些离子的实验室波长被认为是通过白矮星光谱观测α变化极限时得出不一致结论的原因。现在可以用这里给出的改进后的实验室数据来解决这些不一致问题。
