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Automatic Detection of Dark Matter via Weak Gravitational Lensing

Dark Matter is an elusive form of matter that makes up approximately 25% of the known universe. Since it does not absorb or reflect light, it can never be detected via direct observation with a telescope. Instead, its existence must be inferred from the effect of its gravitational field on the background stars / galaxies. If a source of Dark Matter lies between an observer on Earth and a field of background stars, the Dark Matter’s gravitational field will distort the light from the background stars to change the shape and distribution of the stars that the observer sees from their true distribution. This effect is called ”gravitational lensing” and it can be split into two regimes: weak and strong. The effects of strong lensing are somewhat obvious because the distortions produced are very pronounced, i.e. affected galaxies will appear to be bent into long arcs, but this regime is a relatively rare occurrence. Weak lensing, however, produces distortions that are difficult to separate from the background ”noise” of the universe (i.e. the size / ellipticity distributions of galaxies) and measurement error (i.e. thermal distortions in telescope mirrors, effects of atmosphere, etc.). This is the predominant regime for observations of the universe and automatic detection of weak lensing effects is a relatively new field of study.