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Why do we believe the Dark Matter in the Universe to be cold? What does it mean for Dark Matter to be cold? And how does this affect the evolution of structure formation in the Universe? This video answers these along with many other important questions regarding CDM in the standard model of Cosmology.
We will begin by examining the evidence for dark matter, which comes from the missing mass within galaxies. Observations of the velocity distribution of stars within galaxies show they have a flat rotation curve, instead of decreasing with radial distance from the galactic centre, as would be the case using Newtonian mechanics and the observed stellar mass distribution. The gravitational interaction between galaxies and clusters, as well as gravitational lensing of starlight provide a way to constrain the total gravitating mass of a galaxy. When compared to the mass from stars alone shows that a large majority of the mass is unseen. A spherical distribution of unseen mass around galaxies is capable of explaining the flat rotation curve and the total gravity from galaxies.
These dark matter halos form from the early Universe right after inflation occurs from the Quantum Foam left over from the Big Bang. The Heisenberg uncertainty principle leads to small density fluctuations across spacetime which manifest as slight over densities in dark matter. These are then capable of growing via self gravity, sowing the seeds of where galaxies are as we see them today. However, the temperature of dark matter in the universe has a massive effect on this structure formation.
Hot dark matter particles move with a higher average kinetic energy, which can cause the over densities to spread out and smooth out over time - an effect known as Free Streaming. Conversely, cold dark matter is not as affected by free streaming as smaller initial density perturbations can survive the smoothing effect and actually grow due to self gravity. In essence this means that the temperature of the dark matter in the Universe controls the minimum mass or size of structure which can form and we can observe today. With hotter dark matter erasing the smallest perturbations over time, leaving only the largest structures to survive the free streaming.
Observations, such as from the Sloan Digital Sky Survey (SDSS) catalogue galaxies in the night sky allowing us to deduce the clustering and size of structures in the Universe. Other observational evidence which originates from the initial density perturbations left after inflation such as the Cosmic Microwave Background (CMB) can also be used to justify this. With the conclusion that our Universe must contain cold dark matter for such structures to form. Cosmological hydrodynamical supercomputer simulations are used to further justify this by simulating universes with different dark matter temperatures, also predicting cold dark matter responsible compared to the sizes of galaxies in our universe.
This video was sponsored by Brilliant.
0:00 - LambdaCDM Model in Cosmology and Astrophysics
0:32 - Evidence for Dark Matter (Galactic Rotation Curves)
2:10 - Dark Matter Halos
2:28 - Quantum Foam, Inflation and Theoretical Physics in the Early Universe
3:16 - Growth of Cosmic Structures via Mergers and Self Gravity
4:04 - Effect of Temperature on Dark Matter and the Universe
4:47 - Free Streaming of Hot Dark Matter Particles
5:35 - Effect on Structure Size and Comparison to Observations