Analysis of Velocity Shifts in Broad Absorption Line (BAL) Quasars: A Catalog of 25 Quasars with 56 BAL Systems

{'原文': 'We began with the BAL catalog including 2005 quasars constructed by He et al. (2017) from the SDSS data set (SDSS DR12). Two authors of this paper independently visually inspected the spectra of these 2005 quasars to find the BALs that showing velocity shift phenomenon. Finally, we found CIV and/or SiIV BALs of 23 sources show velocity shifts. Thereinto, six sources have been reported in previous articles (Hall2007; Joshi2014, 2019; Grier2016; LL2019), while the remaining 17 quasars had never been reported before. In addition, in order to present an overall sample of BALs showing velocity shifts, we added two of the three sources in a systematic investigation of BAL acceleration that have been reported by G2016, J013656.31-004623.8 and J091425.72+504854.9, to our sample. These two sources were not included in He's(He et al. 2017) catalog because the signal-to-noise ratios of their spectra did not meet He's(He et al. 2017) sample selection criteria. Thus, the sample we used to search for BAL velocity shifts consists of 70 spectra of 25 quasars. Detail information of our BAL quasar sample are shown in Table 1.', '修正后的版本': 'We started with the BAL catalog containing 2005 quasars constructed by He et al. (2017) using the SDSS data set (SDSS DR12). Two authors of this paper independently inspected the spectra of these 2005 quasars visually to identify BALs exhibiting velocity shift phenomena. We ultimately identified 23 sources showing velocity shifts in CIV and/or SiIV BALs. Of these, six sources have been previously reported in the literature (Hall 2007; Joshi 2014, 2019; Grier 2016; LL 2019), while the remaining 17 quasars are novel findings. To ensure a comprehensive sample of BALs exhibiting velocity shifts, we incorporated two of the three sources reported by G2016 in a systematic investigation of BAL acceleration, specifically J013656.31-004623.8 and J091425.72+504854.9, into our sample. These two sources were excluded from He's (He et al. 2017) catalog because the signal-to-noise ratios of their spectra did not meet the sample selection criteria established by He (He et al. 2017). Consequently, our sample used for investigating BAL velocity shifts comprises 70 spectra of 25 quasars. Table 1 provides detailed information about our BAL quasar sample.', '中文详解': '我们从He等人(2017)利用SDSS数据集(SDSS DR12)构建的包含2005个类星体的BAL目录开始。本文的两位作者独立地对这些2005个类星体的光谱进行了目视检查，以识别出显示速度漂移现象的BAL。最终，我们确定了23个源，其CIV和/或SiIV BAL显示出速度漂移。其中，6个源之前已在文献中报道（Hall 2007; Joshi 2014, 2019; Grier 2016; LL 2019），而剩余的17个类星体是新发现。为了确保包含所有显示速度漂移的BAL的样本，我们将G2016在对BAL加速进行系统调查时报道的三个源中的两个，即J013656.31-004623.8和J091425.72+504854.9，纳入我们的样本。这两个源被排除在He（He等人2017）的目录之外，因为它们的光谱信噪比不符合He（He等人2017）制定的样本选择标准。因此，我们用于研究BAL速度漂移的样本包括25个类星体的70个光谱。表1提供了我们BAL类星体样本的详细信息。'}, '原文': 'As in past works by Lu & Lin and Lin & Lu(2018a, 2018b, 2018c, 2018d, 2019a, 2019b, 2019c,2019d, 2020a, 2020b, 2020c), for each spectra in our quasar sample, we chose several wavelength windows without strong emission and absorption lines as wavelength regions for fitting a power-law continuum. Then by iteratively fitting the continuum within these wavelength regions, we fit a power-law continuum for each spectra. By combining the power-law continuum and the Gaussian functions that used to fit the emission lines, we obtained a pseudo-continuum for each quasar spectra. We used these pseudo-continua to normalized the pristine spectra (Figure 1), and identified and measured BALs based on the pseudo-continuum normalized spectra. We have finally identified total 56 BAL systems, including 56 C iv BALs and 25 Si iv BALs. Therein, 35 absorption systems show velocity shift phenomenon, including 30 C iv BALs and five Si iv BALs. The method we used to measured the velocity shifts of BAL troughs was as that in Lu &Lin (2019a).', '修正后的版本': 'Similar to previous studies by Lu & Lin and Lin & Lu (2018a, 2018b, 2018c, 2018d, 2019a, 2019b, 2019c, 2019d, 2020a, 2020b, 2020c), for each spectrum in our quasar sample, we selected several wavelength windows devoid of strong emission and absorption lines as the wavelength regions for fitting a power-law continuum. Through iterative fitting of the continuum within these regions, we fitted a power-law continuum for each spectrum. By combining the power-law continuum with the Gaussian functions employed to fit the emission lines, we obtained a pseudo-continuum for each quasar spectrum. We used these pseudo-continua to normalize the pristine spectra (Figure 1) and identified and measured BALs based on the pseudo-continuum normalized spectra. We ultimately identified a total of 56 BAL systems, including 56 C iv BALs and 25 Si iv BALs. Notably, 35 absorption systems exhibit velocity shift phenomena, encompassing 30 C iv BALs and five Si iv BALs. Our method for measuring the velocity shifts of BAL troughs mirrored that used in Lu & Lin (2019a).', '中文详解': '与Lu和Lin以及Lin和Lu（2018a，2018b，2018c，2018d，2019a，2019b，2019c，2019d，2020a，2020b，2020c）的先前研究类似，对于我们类星体样本中的每个光谱，我们选择了一些没有强发射线和吸收线的波长窗口作为拟合幂律连续谱的波长区域。通过在这些区域内迭代拟合连续谱，我们为每个光谱拟合了一个幂律连续谱。通过将幂律连续谱与用于拟合发射线的高斯函数相结合，我们为每个类星体光谱获得了一个伪连续谱。我们使用这些伪连续谱对原始光谱进行标准化（图1），并基于伪连续谱标准化光谱识别和测量了BAL。我们最终确定了总共56个BAL系统，其中包括56个C iv BAL和25个Si iv BAL。值得注意的是，35个吸收系统表现出速度漂移现象，包括30个C iv BAL和5个Si iv BAL。我们用于测量BAL槽速度漂移的方法与Lu和Lin（2019a）中使用的方法相同。'}, '原文': 'We also quasars the equivalent widths (EWs) for these C IV and Si IV BALs in each epoch using the method in Lu & Lin (2018a; see their Equation (2)), and their fractional EW variations between each two-epoch spectra using the method in Lu et al. (2018; see their Equation (2)). We have finally identified 20 variable C iv and 11 variable Si iv BALs showing fractional EW variations (△EW/) up to a significance level of 3σ. The velocity shift, EW and △EW/ measurements for Civ and Si iv BALs are shown in Table 2.', '修正后的版本': 'We further calculated the equivalent widths (EWs) for these C IV and Si IV BALs in each epoch using the method described in Lu & Lin (2018a; see their Equation (2)) and their fractional EW variations between each two-epoch spectra using the method outlined in Lu et al. (2018; see their Equation (2)). We ultimately identified 20 variable C iv and 11 variable Si iv BALs exhibiting fractional EW variations (△EW/) up to a significance level of 3σ. Table 2 presents the measurements of velocity shift, EW, and △EW/ for Civ and Si iv BALs.', '中文详解': '我们还使用Lu和Lin（2018a；参见他们的方程（2））中描述的方法计算了每个时期这些C IV和Si IV BAL的等效宽度（EW），并使用Lu等人（2018；参见他们的方程（2））中概述的方法计算了每个两个时期光谱之间的分数EW变化。我们最终确定了20个变化的C iv和11个变化的Si iv BAL，显示出分数EW变化（△EW/）高达3σ的显着水平。表2显示了Civ和Si iv BAL的速度漂移，EW和△EW/的测量结果。'}, '原文': 'Throughout this paper, we do not differentiate between BALs and mini-BALs that have a absorption trough width between 500 and 2000 km s−1 (Hamann & Sabra 2004). This is because the absorption index between these two classes of absorption troughs shows a continuous distribution (e.g., Trump et al. 2006; Ganguly & Brotherton 2008; Gibson et al. 2009), and in some cases, mini-BALs can translate to BALs (e.g., Rodríguez Hidalgo et al. 2013).', '修正后的版本': 'Throughout this paper, we do not distinguish between BALs and mini-BALs, which have absorption trough widths ranging from 500 to 2000 km s−1 (Hamann & Sabra 2004). This approach is justified because the absorption index between these two classes of absorption troughs exhibits a continuous distribution (e.g., Trump et al. 2006; Ganguly & Brotherton 2008; Gibson et al. 2009), and in certain instances, mini-BALs can transition into BALs (e.g., Rodríguez Hidalgo et al. 2013).', '中文详解': '在本文中，我们不区分BAL和mini-BAL，它们的吸收槽宽度在500到2000 km s−1之间（Hamann和Sabra 2004）。这种方法是合理的，因为这两类吸收槽之间的吸收指数呈连续分布（例如，Trump等人2006；Ganguly和Brotherton 2008；Gibson等人2009），并且在某些情况下，mini-BAL可以转化为BAL（例如，Rodríguez Hidalgo等人2013）。