Summarize the links in the distance chain that allow us to estimate distances to

We can determine the distance to solar system objects through radar ranging. This gives us an accurate distance to the Sun so that we can use stellar parallax to measure the distances to the nearest stars. The Hyades is an open cluster whose stars are near enough to us that their distances can be measured with stellar parallax. This gives us a cluster of stars that we can plot on an H-R diagram to determine the luminosity of the main sequence. For more distant clusters, we can compare their main sequence to this fit and measure their distance by the method of main-sequence fitting. The distances to Cepheid variables in clusters can be determined from main-sequence fitting. Since there is a period-luminosity relationship for Cepheids, we can measure the distances to other Cepheids by just measuring the time period between peaks of brightness. Cepheids are bright enough to be observed in galaxies other than the Milky Way. Therefore, they serve as a bridge between us and standard candles in other galaxies. Once we determine the distance to another galaxy for which we have observed a white-dwarf supernova, we then can calibrate the average luminosity of white-dwarf supernovae, as well as use other methods, such as the Tully-Fisher relation. White-dwarf supernovae and the Tully-Fisher relation get us far enough away from the Milky Way that we then can calibrate Hubble's law by determining the Hubble constant. Once we know the Hubble constant, we will be able to determine a galaxy's distance from its redshift.