To know the expansion curve is to know a lot about cosmic expansion, e.g., the age of the universe and the distance to galaxies with a measured redshift.
The expansion curve is normally drawn for the cosmic expansion factor a(t) against cosmic time. The expansion factor is just a measure of by how much smaller (in terms of ratio) the cosmos was at some time in the past. It is very simply related to the redshift factor (z), as is clear from the right- and left-hand axes of the graph, i.e: 1 + z = 1/a(t). The redshift factor z is the change in wavelength, expressed as a fraction of the original wavelength emitted.
Curve (i) is a plot for the perfectly parabolic expansion of the Einstein-de Sitter model, where matter density exactly equals the critical density for a 'flat' cosmos. Curve (ii) is for the present Lambda-Cold-Dark-Matter model, where normal plus dark matter together makes out about 25% of the critical density and the rest is vacuum energy (Einstein's cosmological constant). Both curves were plotted for a Hubble constant H0 ≈ 72 km/s/Mpc.
The two black bullets, where the z=1 line cuts the two curves respectively, represent a galaxy that is observed at redshift z=1. The markers now(i) and now(ii) represent the age of the universe according to the respective models (about 10 and 14 billion years respectively). The two arrows s1 and s2 are the look-back distances of the galaxy according to the two models, roughly 6 and 8 billion light-years. This, according to the model employed, is the distance that light has traveled since being emitted. It is not the 'real distance' of the galaxy, which has changed over time due to the cosmic expansion.
In order to determine the shape of the expansion curve, cosmologists measure the redshift of a large number of galaxies, near and far. This alone is however not good enough - they also need the look-back distance (or time), which is easier said than measured. The distance to many stars in our own galaxy can be measured by means of parallax over the course of a year, as Earth moves around the Sun. Other galaxies pose a problem though - at their distances the parallax is just too small to be of any use. This is where proper motion, Cepheid variable stars and supernovae come in.
The way these standard methods are being utilized to build a 'distance ladder' is quite intriguing, but a bit too lengthy to describe here. At the risk of infuriating loyal readers, I'll have to refer you to a .pdf or a .doc (about 9 pages in length) on my website, containing a non-technical description of each method.
Jorrie
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