We combine in a self-consistent way the constraints from both gravitational lensing and stellar kinematics to perform a detailed investigation of the internal mass distribution, amount of dark matter, and dynamical structure of the 16 early-type lens galaxies from the SLACS Survey, at z = 0.08 - 0.33, for which both HST/ACS and NICMOS high-resolution imaging and VLT VIMOS IFU spectroscopy are available. Based on this data set, we analyze the inner regions of the galaxies, i.e. typically within one (3D) effective radius r_e, under the assumption of axial symmetry and by constructing dynamical models supported by two-integral stellar DFs. For all systems, the total mass density distribution is found to be well approximated by a simple power-law: this profile is on average slightly super-isothermal, with a logarithmic slope <gamma'> = 2.074^{+0.043}_{-0.041} (68% CL) and an intrinsic scatter 0.144^{+0.055}_{-0.014}, and is fairly round, with an average axial ratio <q> = 0.77+/-0.04. The lower limit for the dark matter fraction (fDM) inside r_e ranges, in individual systems, from nearly zero to almost a half, with a median value of 12%. By including stellar masses derived from SPS models with a Salpeter IMF, we obtain an average fDM = 31%. The fDM rises to 61% if, instead, a Chabrier IMF is assumed. For both IMFs, the dark matter fraction increases with the total mass of the galaxy (3-sigma correlation). Based on the intrinsic angular momentum parameter calculated from our models, we find that the galaxies can be divided into two dynamically distinct groups, which are shown to correspond to the usual classes of the slow and fast rotators. Overall, the SLACS systems are structurally and dynamically very similar to their nearby counterparts, indicating that the inner regions of early-type galaxies have undergone little, if any, evolution since redshift z ~ 0.35. (Abridged)
The global mass - to - light ratio of SLACS lenses
早期，-型星系（ETG）的暗物质含量是一个激烈争论的话题与对比的结果争论赞成或反对的有效半径内的显着的暗质量的存在和光度和质量的变化。为了解决这个问题，我们在这里调查的全球质量-光比$Υ(r) = M(r)/L(r)$的样本中观察到的21个镜头斯隆镜头ACS（SLACS）调查。我们遵循通常的方法，将星系建模为两个组成部分的系统，但我们使用的$Υ(r)$的现象学分析，我们中的一些人在Tortora et al.（2007）中提出，能够顺利地插入常数$M/L$模型和广泛的一类暗物质晕。由此产生的星系模型，然后拟合的爱因斯坦半径和速度色散的数据。我们的唯象模型结果是在很好的协议与数据表明存在大量的暗物质晕，以解释透镜和动力学性质的SLACS透镜。根据暗物质质量分数的值，我们认为暗晕可能在数据探测的内部区域起着重要的作用，但这一结论强烈依赖于所采用的恒星星族初始质量函数。最后，我们发现，在$R_{eff}$的暗物质质量分数尺度与总光度和恒星质量在这样一种方式，更明亮（因此更大质量）的星系有一个更大的暗物质的内容。
Line-of-sight shear in SLACS strong lenses II: validation tests with an extended sample
University of Cambridge（剑桥大学）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Laboratoire Univers et Particules de Montpellier, CNRS & Université de Montpellier（蒙彼利埃大学与法国国家科学研究中心宇宙与粒子物理实验室）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Independent University, Bangladesh（孟加拉独立大学）
COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses VIII. Deconvolution of high resolution near-IR images and simple mass models for 7 gravitationally lensed quasars
Line-of-sight shear in SLACS strong lenses I: shear and mass model parametrisations
Institute of Astronomy, University of Cambridge（剑桥大学天文学研究所）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Clare Hall（克莱尔学院）；Laboratoire Univers et Particules de Montpellier, CNRS & Université de Montpellier（蒙彼利埃大学与法国国家科学研究中心宇宙与粒子物理实验室）；Department of Astronomy & Astrophysics, University of Chicago（芝加哥大学天文与天体物理系）；Kavli Institute for Cosmological Physics, University of Chicago（芝加哥大学卡弗里宇宙物理学研究所）；Center for Astronomy, Space Science and Astrophysics, Independent University, Bangladesh（孟加拉独立大学天文、空间科学与天体物理中心）
