Redshift-dependent decomposition of theoptical spectrum of the quasar HE 0413−4031

The redshift determination in quasars with only broad emission line present creates a problem when high accuracy is needed. This in tern affects the decoposition of the spectrum into continuum, line emission (here Mg II line) and Fe II pseudo-continuum. Here we enclose the data behind the Figure 3, middle panel, from Zajacek et al. (20240, A&A, 683, Article Number A140. It presents the results based on the Southern African Large Telescope data, our Observation 14 of the quasar HE 0413−4031 The four sets show the Fe II net contribution according to the following models in the observedframe: two models for the old redshift z = 1.37648, d12 and VW01 templates with extra broadening, and two for the new redshift z = 1.39117,the KDP15 template, shift = 0, FWHM = 4200 km s−1, and the VW01 template with additional broadening. See the article for more detailed description. a) tytuł zbioru danych; Redshift-dependent decomposition of theoptical spectrum of the quasar HE 0413−4031 b) autora(ów) i ich afiliacje; Michal Zajaˇcek,, Swayamtrupta Panda, Ashwani Pandey, Raj Prince, Alberto Rodríguez-Ardila,, VikramJaiswal, Bo˙zena Czerny, Krzysztof Hryniewicz, Maciej Urbanowicz, Piotr Trzcionkowski, Marzena ´Sniegowska,Zuzanna Fałkowska, Mary Loli Martínez-Aldama, and Norbert Werner c) datę powstania danych i/lub daty gromadzenia; 2019 d) opis metodologii badawczej i narzędzi użytych do pozyskania danych: The data were collected using the Southern Africal Large Telescope. Following the previous studies on this source, we assume a single kinematic component for the MgII line shape (Za-jaˇcek et al. 2020; Prince et al. 2023). However, we take into account that MgII is a doublet, and this is included in our modeling, assuming the same widths for the two components, fixed separation. The value of the doublet ratio was optimized by Zajaˇceket al. (2020) using the mean spectrum. We use the same value of 1.9 in the current paper. The kinematic width, line position, and normalization are free parameters of the model. The underlying continuum is described as a power law with an arbitrary normal-ization and a slope. e) format i struktura danych; file has 7 columns, the first column gives the wavelength, the remaining columns give the data, the total model, and the model components. f) warunki udostępniania i licencjonowania danych; Creative Commons Attribution License g) adnotację o finansowaniu ze środków projektu i poprawny nr rejestracyjny projektu (Narodowe Centrum Nauki, numer projektu). The project waspartially supported by the Polish Funding Agency National Science Centre,project 2017/26/A/ST9/00756 (MAESTRO 9). BC and MZ acknowledge the OPUS-LAP/GA ˇCR-LA bilateral project (2021/43/I/ST9/01352/OPUS 22 andGF23-04053L).仅存在宽发射线（broad emission line）的类星体（quasar）的红移（redshift）测定在需要高精度时会面临难题，这进而会影响光谱分解为连续谱（continuum）、线发射（此处为Mg II线）以及Fe II伪连续谱（Fe II pseudo-continuum）的过程。 本数据集附带了Zajacek等人（2024，《天文学与天体物理学》（A&A），683卷，文章编号A140）中图3中间面板对应的原始数据。该数据基于南非大望远镜（Southern African Large Telescope）的观测结果，对应类星体HE 0413−4031的第14次观测。四组数据展示了观测帧下不同模型对应的Fe II净贡献：两组基于旧红移z=1.37648，分别为添加了额外展宽的d12和VW01模板；另外两组基于新红移z=1.39117，分别为KDP15模板（偏移量=0，半高全宽FWHM=4200 km s⁻¹）以及添加额外展宽的VW01模板。详细描述请参阅原文。 a) 数据集标题：类星体HE 0413−4031光学光谱的红移依赖分解 b) 作者及其所属机构：Michal Zajaček、Swayamtrupta Panda、Ashwani Pandey、Raj Prince、Alberto Rodríguez-Ardila、Vikram Jaiswal、Bożena Czerny、Krzysztof Hryniewicz、Maciej Urbanowicz、Piotr Trzcionkowski、Marzena Śniegowska、Zuzanna Fałkowska、Mary Loli Martínez-Aldama 以及 Norbert Werner c) 数据生成和/或采集日期：2019年 d) 研究方法学及数据获取工具：本研究使用南非大望远镜采集数据。参考此前针对该源的研究，我们假设Mg II线轮廓仅包含单一运动学成分（Zajaček et al. 2020; Prince et al. 2023）。但我们考虑到Mg II是双线结构，将其纳入建模过程，假设两个成分具有相同的宽度和固定的波长间隔。双线强度比的取值由Zajaček等人（2020）通过平均光谱优化得到，本研究沿用其1.9的取值。运动学展宽、线位置以及归一化均为模型的自由参数。本底连续谱采用任意归一化和斜率的幂律模型描述。 e) 数据格式与结构：数据文件包含7列，第一列为波长，其余列依次为观测数据、总模型拟合结果以及各模型成分的贡献。 f) 数据共享与授权协议：知识共享署名许可协议（Creative Commons Attribution License） g) 项目资助说明及项目登记号：本研究部分受波兰国家科学中心（Narodowe Centrum Nauki）资助，项目编号为2017/26/A/ST9/00756（MAESTRO 9）。BC与MZ感谢OPUS-LAP/GA ČR-LA双边项目（2021/43/I/ST9/01352/OPUS 22 以及 GF23-04053L）的支持。