Studying Galaxies, Galaxy Clusters, and Cosmology with Weak Gravitational Lensing Magnification

弱引力透镜(WL)被认为是研究暗能量(DE)的本质、检验广义相对论(GR)以及理解可见光和暗物质(DM)结构之间关系的最强大的技术之一。虽然这一领域的大多数研究人员在这些研究中使用了WL的剪切效应，但我已经开始将放大效应作为一种竞争性工具，它补充了剪切，并允许进行一些新的、独特的测量，这是剪切不可能实现的。这里提出的艾美诺特小组将进一步开发和应用这些方法，以产生第一个与天体物理相关的此类测量结果。我们将从CFHTLS和KILDS数据中测量红移高达z~1.4的星系的放大倍数。通过这种方式，我们将约束Dm-Hale质量，并将它们与恒星质量、光谱类型等联系起来。我们还将使用星等漂移效应测量这些星系的尘埃轮廓，以几个MPC为单位。此外，我们对来自SPARCS和KIDES的高红移星团的质量测量将对理解星系团的形成和测量星系团的质量函数做出不可或缺的贡献，这些红移是其他方法难以获得的。最终，通过将星系的尘埃和Dm晕测量与几个红移切片上的星团测量相结合，我们将测量放大层析成像，从而测试GR并限制DE的性质。

Weak gravitational lensing (WL) has been recognised as one of the most powerful techniques to study the nature of dark energy (DE), to test general relativity (GR), and to understand the relationship between visible and dark matter (DM) structures. While most researchers in this field use the shear effect of WL for these studies I have begun to establish the magnification effect as a competitive tool, which complements the shear and allows some new, unique measurements that are not possible with the shear. The Emmy Noether group proposed here will further develop and apply these methods to yield the first astrophysically relevant measurements of this kind. We will measure the magnification induced by galaxies with redshifts up to z ~ 1.4 from CFHTLS and KiDS data. In this way we will constrain DM-halo masses and relate them to stellar masses, spectral types, etc. We will also measure the dust profiles of these galaxies out to several Mpc using the magnitude-shift effect. Furthermore, our mass measurements of high-redshift clusters from SpARCS and KiDS will be an indispensable contribution to understanding cluster formation and measuring the galaxy cluster mass function, at redshifts hard to access by other methods. Eventually, by combining the dust- and DM-halo measurements of galaxies with clustering measurements in several redshift slices we will measure magnification tomography and thereby test GR and constrain the nature of DE.