We present the spectrum analysis of the hot Am star HR 3383 (A1 Vm). Hubble Space Telescope STIS and Nordic Optical Telescope SOFIN data are modelled with synthetic spectra, and abundances are investigated for 78 elements. Most light elements up through oxygen show deficiencies, compared to solar abundances, followed by the general trend of increasing abundance enhancement with atomic number that levels off at a 30-fold enhancement at the lanthanide group and heavier elements. The derived element distribution is generally consistent with what is observed in other hot Am stars. Abundances for HR 3383 are also similar to what is seen for the cooler HgMn stars, with the exception of the platinum-group elements that generally show dramatic enhancements in the HgMn stars. Current theory and calculations are able to predict most observed abundances and abundance trends through the iron group. The large number of derived element abundances in this study provides a constraint for theoretical calculations attempting to explain the heavy element abundances in chemically peculiar stars. This paper includes a comprehensive description of spectral lines useful for an abundance analysis of late B and A type stars, and comments are provided on the atomic data. New data for hyperfine structure components for three lines in Lu iii and a single line in Lu ii are presented, based on laboratory spectra. In addition to the stellar spectrum, lines from the interstellar medium are noted for several of the strongest Fe ii ultraviolet transitions.

中文翻译：

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高温Am star HR 3383的高分辨率光谱

我们介绍了热的Am ​​star HR 3383（A1 Vm）的光谱分析。哈勃太空望远镜STIS和北欧光学望远镜用合成光谱对SOFIN数据进行建模，并研究了78种元素的丰度。与太阳的丰度相比，通过氧气向上传播的大多数轻元素都表现出不足，其次是总体趋势是，随着镧系元素和较重元素的原子序数增加到30倍，原子序数趋于平稳，从而增加了丰度。导出的元素分布通常与在其他热美星中观察到的一致。HR 3383的丰度也与较冷的HgMn恒星相似，但铂族元素通常会在HgMn恒星中显着增强。当前的理论和计算能够通过铁族预测大多数观察到的丰度和丰度趋势。本研究中大量的衍生元素丰度为试图解释化学特殊恒星中的重元素丰度的理论计算提供了限制。本文对光谱线进行了全面的描述，可用于后期B和A型恒星的丰度分析，并提供了有关原子数据的注释。Lu中三条线的超精细结构组件的新数据 根据实验室光谱，给出了iii和Lu ii中的一行 。除恒星光谱外，星际介质中的谱线还记录了一些最强的Fe  ii紫外线跃迁。