Gravitational Lensing
Gravitational Lensing
Gravitational Lensing
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Deflection angle Introduction to <strong>Gravitational</strong> <strong>Lensing</strong> Applications<br />
Mass Profile of Galaxy Clusters<br />
Reconstruction of mass distribution<br />
• Mass mapping by GL is valuable because does not<br />
depend on dynamic state of the cluster/galaxy<br />
(h (the tradition method h for f searching h mass<br />
distribution is by their dynamic state)<br />
• Using strong and Weak <strong>Lensing</strong> to map the mass<br />
distribution of the Lens<br />
• Multiple images of Strong <strong>Lensing</strong> enable us to<br />
construct the lens lens’ mass using the lens equation<br />
with numerical calculations<br />
• Weak Lens’ shearing effect is the other parameter<br />
for mass mapping<br />
• In real situations, parametric models of the<br />
source and the lens are complicated We<br />
construct mass model to match observed images<br />
and find best‐fit parameters<br />
Adopted d dffrom: Annu. Rev. Astron. Astrophys. h 1999. 37: 127‐189<br />
source and the lens are complicated. We
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