Gravitational Lensing

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Deflection angle Introduction to Gravitational Lensing Applications Mass mapping by Shearing effect shearing • The orientation of intrinsic ellipticities of galaxies should be almost entirely random • Observing shearing of the images images, we can get the mass distribution shear convergence θ = Angular position Potential mapped on the coordinate of line of sight g
Deflection angle Introduction to Gravitational Lensing Applications Evidence of Dark Matter Adopted from: J. Tyson, G. Kochanski and I. Dell’Antonio, Ap. J. Lett. 498 107 (1998) • Combine weak and strong lensing analysis analysis, we can map the mass distribution of a cluster. Galaxy cluster CL0024+1654 is an example. • Spikes are due to the visible galaxy • A smooth background mass density is observed in the region without any luminous matter
Page 1 and 2: Nelson Leung Kwok Hui Kin
Page 3 and 4: • In 1919, 1919 this effect was c
Page 5 and 6: Deflection angle Introduction to Gr
Page 7 and 8: D LS D L Deflection angle Introduct
Page 9 and 10: Einstein Ring Applications Deflecti
Page 11 and 12: Types of Lensing Applications Defle
Page 15 and 16: How cosmologists g and astrophysici
Page 25: Deflection angle Introduction to Gr
Page 29 and 30: Conclusion In recent years, gravita
Page 31: References • D.walsh, et.al. ‘0

Gravitational Lensing

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