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Strong Lensing by Galaxies
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Strong gravitational lensing at the galaxy scale is a valuable tool for various applications in astrophysics and cosmology. The primary uses of galaxy-scale lensing are to study elliptical galaxies' mass structure and evolution, constrain the stellar initial mass function, and measure cosmological parameters. Since the discovery of the first galaxy-scale lens in the 1980s, this field has made significant advancements in data quality and modeling techniques. In this review, we describe the most common methods for modeling lensing observables, especially imaging data, as they are the most accessible and informative source of lensing observables. We then summarize the primary findings from the literature on the astrophysical and cosmological applications of galaxy-scale lenses. We also discuss the current limitations of the data and methodologies and provide an outlook on the expected improvements in both areas in the near future.
Forward citations
Cited by 2 Pith papers
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Line-of-sight shear in SLACS strong lenses II: validation tests with an extended sample
Line-of-sight shear in 45 SLACS lenses is often larger than N-body expectations (mean |γ_LOS| ≈ 0.085–0.11), and adding mass octupoles or checking image properties does not remove the excess.
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