Gravitational Lensing: Strong, Weak and Micro

Transcription

1 P. Schneider C. Kochanek J. Wambsganss Gravitational Lensing: Strong, Weak and Micro Saas-Fee Advanced Course 33 Swiss Society for Astrophysics and Astronomy Edited by G. Meylan, P. Jetzer and P. North With 196 Illustrations, 36 in Color ^y Springer

2 Contents Part 1: Introduction to Gravitational Lensing and Cosmology P. Schneider 1 1 Introduction History of Gravitational Light Deflection Discoveries What is Lensing Good for? 14 2 Gravitational Lens Theory The Deflection Angle The Lens Equation Magnification and Distortion Critical Curves and Caustics, and General Properties of Lenses The Mass-Sheet Degeneracy 29 3 Simple Lens Models Axially Symmetric Lenses The Point-Mass Lens \ The Singular Isothermal Sphere Non-Symmetric Lenses 38 4 The Cosmological Standard Model I: The Homogeneous Universe The Cosmic Expansion Distances and Volumes Gravitational Lensing in Cosmology 52 5 Basics of Lensing Statistics Cross-Sections Lensing Probabilities; Optical Depth Magnification Bias 58 6 The Cosmological Standard Model II: The Inhomogeneous Universe Structure Formation Halo Abundance and Profile 71

3 X Contents 6.3 The Concordance Model Challenges 81 7 Final Remarks 83 References 84 Part 2: Strong Gravitational Lensing C. S. Kochanek 91 1 Introduction 91 2 An Introduction to the Data 92 3 Basic Principles Some Nomenclature Circular Lenses Non-Circular Lenses The Mass Distributions of Galaxies Common Models for the Monopole The Effective Single Screen Lens Constraining the Monopole The Angular Structure of Lenses Constraining Angular Structure Model Fitting and the Mass Distribution of Lenses Non-Parametric Models..' Statistical Constraints on Mass Distributions Stellar Dynamics and Lensing Time Delays A. General Theory of Time Delays Time Delay Lenses in Groups or Clusters Observing Time Delays and Time.Delay Lenses..., Results: The Hubble Constant and Dark Matter." The Future of Time Delay Measurements Gravitational Lens Statistics The Mechanics of Surveys : The Lens Population Cross Sections '....' Optical Depth Spiral Galaxy Lenses..; Magnification Bias Cosmology With Lens Statistics The Current State What Happened to the Cluster Lenses? The Effects of Halo Structure and the Power Spectrum Binary Quasars...:.. ' The Role of Substructure Low Mass Dark Halos '...:..'.;: The Optical Properties of Lens Galaxies The Interstellar Medium of Lens Galaxies 238

4 Contents XI 10 Extended Sources and Quasar Host Galaxies An Analytic Model for Einstein Rings Numerical Models of Extended Lensed Sources Lensed Quasar Host Galaxies Does Strong Lensing Have a Future?..."." 255 References 256 Part 3: Weak Gravitational Lensing P. Schneider Introduction The Principles of Weak Gravitational Lensing Distortion of Faint Galaxy Images Measurements of Shapes and Shear Tangential and Cross Component of Shear Magnification Effects Observational Issues and Challenges Strategy Data Reduction: Individual Frames Data Reduction: Coaddition Image Analysis Shape Measurements Clusters of Galaxies: Introduction, and Strong Lensing Introduction General Properties of Clusters The Mass of Galaxy Clusters Luminous Arcs and Multiple Images Results from Strong Lensing in Clusters Mass Reconstructions from Weak Lensing The Kaiser-Squires Inversion Improvements and Generalizations Inverse Methods Parameterized Mass Models Problems of Weak Lensing Cluster Mass Reconstruction and Mass Determination Results Aperture Mass and Other Aperture Measures Mass Detection of Clusters Cosmic Shear - Lensing by the LSS : Light Propagation in an Inhomogeneous Universe Cosmic Shear: The Principle Second-Order Cosmic Shear Measures Cosmic Shear and Cosmology E-Modes, B-Modes Predictions; Ray-Tracing Simulations 377

5 XII Contents 7 Large-Scale Structure Lensing: Results Early Detections of Cosmic Shear Integrity of the Results Recent Cosmic Shear Surveys Detection of B-Modes 392' 7.5 Cosmological Constraints D Lensing Discussion The Mass of, and Associated with Galaxies Introduction Galaxy-Galaxy Lensing Galaxy Biasing: Shear Method Galaxy Biasing: Magnification Method Additional Issues in Cosmic Shear Higher-Order Statistics Influence of LSS Lensing on Lensing by Clusters and Galaxies Concluding Remarks 439 References 442 Part 4: Gravitational Microlensing J. Wambsganss Lensing of Single Stars by Single Stars Brief History Theoretical Background How Good is the Point Lens - Point Source Approximation? Statistical Ensembles Binary Lenses Theory and Basics of Binary Lensing First Microlensing Lightcurve of a Binary Lens: OGLE-7...\ Binary Lens MACHO 1998-SMC-l Binary Lens MACHO 1999-BLG Binary Lens EROS BLG Microlensing and Dark Matter: Ideas, Surveys and Results Why We Need Dark Matter: Flat Rotation Curves (1970s), How to Search for Compact Dark Matter (as of 1986) Just Do It: MACHO, EROS, OGLE et al. (as of 1989) "Pixel"-Lensing: Advantage Andromeda! Current Interpretation of Microlensing Surveys with Respect to Halo Dark Matter (as of 2004) Microlensing toward the Galactic Bulge Microlensing Surveys in Search of Extrasolar Planets How Does the Microlensing Search for Extrasolar Planet Work? The Method 486

6 Contents XIII 4.2 Why Search for Extrasolar Planets with Microlensing? - Advantages and Disadvantages Who is Searching? The Teams: OGLE, MOA, PLANET, MicroFUN What is the Status of Microlensing Planet Searches so far? The Results When will Planets be Detected with Microlensing? The Prospects Note Added in April 2004 (About One Year after the 33rd Saas Fee Advanced Course) Summary Higher Order Effects in Microlensing: Astrometric Microlensing Quasar Microlensing Microlensing Mass, Length and Time Scales Early and Recent Theoretical Work on Quasar Microlensing Observational Evidence for Quasar Microlensing Quasar Microlensing: Now and Forever? 534 References Inde;c 541