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When my professor first started running his probabilities and modeling, he was often skewed to the bottom right of his plot map. He worked for many months trying to account for it, and last time I talked with him, he had chosen to simply adjust and center the image. I don't know if he ever found a programming error, or an inconsistency in Einstein's formula, or if there was possibly another source or reason that the computer model was skewed in relation to what we see in real-life observations.
Would your dark matter theory, or a second gravitational source that is invisible account for everything falling into place, yet skewed at the same time?
In addition to macrolensing by the galaxy, stars in the lensing galaxy act as secondary lenses to produce an additional magnification. This secondary magnification is based on the same principle as macrolensing, but on a smaller scale, and since stars are much smaller than galaxies, is known as “microlensing”. Because the stars are moving in the lensing galaxy, the microlensing magnification also changes with time. From Earth, the brightness of the quasar images (four in the case of the Einstein Cross) flickers around a mean value, due to microlensing. The size of the area magnified by the moving stars is a few light-days, i.e., comparable in size to the quasar accretion disc.
The microlensing affects various emission regions of the disc in different ways, with smaller regions being more magnified. Because differently sized regions have different colors (or temperatures), the net effect of the microlensing is to produce color variations in the quasar images, in addition to the brightness variations. By observing these variations in detail for several years, astronomers can measure how matter and energy are distributed about the supermassive black hole that lurks inside the quasar. Astronomers observed the Einstein Cross three times a month over a period of three years using ESO’s Very Large Telescope (VLT), monitoring all the brightness and color changes of the four images.