Large-scale structure formation in the universe is the final pillar in the Hot Big Bang Standard Model. We want to know how galaxy clusters formed, how dark matter came to be where it is. Also, we learn why galaxy clusters have so much hot gas, and how the absorption features in distant quasars came to be. We also see how the dark matter distribution can be mapped by its effect on galaxy's light and on the shape of clusters too. We also see how the Cosmic Microwave Background plays a central role in it all. This is part of my complete intro Astronomy class that I taught at Willam Paterson University and CUNY Hunter. Some simulations were performed at the National Center for Supercomputer Applications by Andrey Kravtsov (The University of Chicago) and Anatoly Klypin (New Mexico State University). Visualizations by Andrey Kravtsov. The Millennium Simulation Project Volume rendering of a simulation from the EAGLE project Rob Crain & Jim Geach Planck simulations of CMB transit Supplement the videos with OpenStax Astronomy 29: The Big Bang Large-scale structure The Laniakea Supercluster NASA's Hubble, Chandra Find Clues that May Help Identify Dark Matter Dark Matter Lyman-alpha forest Evolution of HI: 3C273 spectrum from HST/FOC z=0; z=3.6 QSO HIRES/Keck spectrum from M.