论文标题
高分辨率类星体光谱中的MGII吸收器。 I. voigt配置文件模型
MgII Absorbers in High Resolution Quasar Spectra. I. Voigt Profile Models
论文作者
论文摘要
我们介绍了VOIGT曲线（VP）模型，列密度，多普勒B参数，运动学以及422 MGII吸收剂的组件分布，在对249名员工和uves Quasar Spectra的调查中发现。样品的等效宽度范围为0.006 <w_r（2796）<6.23埃埃斯特群（A），红移范围为0.19 <z <2.55，平均值为<z> = 1.18。基于历史先例，我们将180个吸收剂分类为弱系统（W_R（2796）<0.3 A），将242分为强系统（W_R（2796）> = 0.3 A）。假设每个系统的重要组件数量最少，则VP拟合总共产生了2,989个组件，平均为弱和强MGII子样本的平均成分分别为2.7和10.3组件。完整样品的VP组件线密度为8.62 +/- 0.23云/a。 VP组件柱密度在12.4 <log [n（mGII）] <17.0 [ions cm^-2]上的分布很好地建模了-1.45 +/- 0.01的幂律斜率。中值多普勒B参数为4.5 +/- 3.5 km/s，6.0 +/- 4.5 km/s和5.7 +/- 4.4 km/s，对于弱，强和完整的样品。我们使用三组分复合材料高斯函数建模了我们完整样本的组件速度拆分（两点速度相关函数TPCF）的概率。我们由此产生的速度分散剂分别为25.4、68.7和207.1 km/s。这些数据为研究MGII吸收器运动学演化的宇宙演化提供了出色的数据库。
We present the Voigt profile (VP) models, column densities, Doppler b parameters, kinematics, and distribution of components for 422 MgII absorbers found in a survey of 249 HIRES and UVES quasar spectra. The equivalent width range of the sample is 0.006 < W_r(2796) < 6.23 angstroms (A) and the redshift range is 0.19 < z < 2.55, with a mean of <z> = 1.18. Based on historical precedent, we classified 180 absorbers as weak systems (W_r(2796) < 0.3 A) and 242 as strong systems (W_r(2796) >= 0.3 A). Assuming a minimum number of significant components per system, the VP fitting, yielded a total of 2,989 components, with an average of 2.7 and 10.3 components found for the weak and strong MgII subsamples, respectively. The VP component line density for the full sample is 8.62 +/- 0.23 clouds/A. The distribution of VP component column density over the range 12.4 < log[N(MgII)] < 17.0 [ions cm^-2] is well modeled with a power-law slope of -1.45 +/- 0.01. The median Doppler b parameters are 4.5 +/- 3.5 km/s, 6.0 +/- 4.5 km/s and 5.7 +/- 4.4 km/s for the weak, strong, and full samples. We modeled the probability of component velocity splitting (the two-point velocity correlation function, TPCF) of our full sample using a three-component composite Gaussian function. Our resulting velocity dispersions are 25.4, 68.7, and 207.1 km/s, respectively. These data provide an excellent database for studying the cosmic evolution of MgII absorber kinematic evolution.
