望远镜RR的禁戒线和互组合线：波长测量和能级
Forbidden and intercombination lines of RR Telescopii: wavelength measurements and energy levels
摘要：
望远镜座RR共生新星的紫外和可见光谱被用来导出元素C、N、O、Ne、Na、Mg、Al、Si、P、S、Cl、Ar、K和Ca的+1至+6离子的禁戒和互组合跃迁的参考波长。然后使用波长来确定离子的基态构型或第一激发构型内的能级的新能量值。光谱分别由哈勃太空望远镜的空间望远镜成像摄谱仪和欧洲南方天文台的紫外中阶梯摄谱仪于2000年和1999年测量，覆盖1140 ~ 6915 A特别注意评估两种仪器之间波长标度的准确度。对发射线轮廓的研究表明，星云至少由两种不同速度的等离子体成分组成。这些谱线的成分具有不同的密度，一个简单的谱线发射模型表明，大多数谱线主要来自高密度成分。只有这些谱线用于波长研究。
英文摘要：
Ultraviolet and visible spectra of the symbiotic nova RR Telescopii are used to derive reference wavelengths for many forbidden and intercombination transitions of ions +1 to +6 of elements C, N, O, Ne, Na, Mg, Al, Si, P, S, Cl, Ar, K and Ca. The wavelengths are then used to determine new energy values for the levels within the ions' ground configurations or first excited configuration. The spectra were measured by the Space Telescope Imaging Spectrograph of the Hubble Space Telescope and the UltraViolet Echelle Spectrograph of the European Southern Observatory in 2000 and 1999, respectively, and cover 1140 to 6915 A. Particular care was taken to assess the accuracy of the wavelength scale between the two instruments. An investigation of the profiles of the emission lines reveals that the nebula consists of at least two plasma components at different velocities. The components have different densities, and a simple model of the lines' emissions demonstrates that most of the lines principally arise from the high density component. Only these lines were used for the wavelength study.
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