Cosmology at intermediate redshifts with X-ray observations
Cosmological models aim at explaining how the Universe at z~1500 we see in CMB observations evolves to our local z~0 lumpy Universe. Most of the X-ray background originates at redshifts z~2 and therefore can in principle be used to measure the structure of the Universe at these intermediate redshifts. This happens to be an exciting epoch in the evolution of the Universe, because it is when the largest structures we see today begin to collapse. X-ray background fluctuation studies can map the structure of the Universe at intermediate redshifts. I will discuss measurements on different scales which can provide a general picture of the power spectrum of density fluctuations at comoving wavevector from 0.01 to 10 h/Mpc.
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