The parallactic refraction between the stars and the satellite is small and well determinate, except for the irregular stellar movements known as erratics.
Using this method, isopachic fractional fringe orders can be measured with compensator, and the parallax and drift of fringe pattern can be eliminated.
They use a distance called the parsec (a contraction of parallax and second), based on a universal measure called the stellar parallax and equivalent to 3.26 light-years.
Scientists hail Gaia's mapping work as crucial to the parallax method, which compares the difference in the direction a star appears to be traveling depending on where on earth it is viewed.
So if you know how far away the nearer one is by measuring its parallax, you just have to compare its brightness to one farther away to get its distance.
By timing the transit from two widely-separated locations, teams of astronomers could calculate the parallax angle—the apparent difference in position of an astronomical body due to a difference in the observer's position.