Using Large-Scale Structure and CMB Observations to Probe the Properties of Dark Energy

          @misc{ scivideos_PIRSA:09050000,
            doi = {10.48660/09050000},
            url = {https://pirsa.org/09050000},
            author = {Spergel, David},
            keywords = {Cosmology},
            language = {en},
            title = {Using Large-Scale Structure and CMB Observations to Probe the Properties of Dark Energy},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2009},
            month = {may},
            note = {PIRSA:09050000 see, \url{https://scivideos.org/pirsa/09050000}}
          }
          

Abstract

Cosmologists are struggling to understand why the expansion rate of our universe is now accelerating. There are two sets of explanations for this remarkable observation: dark energy fills space or general relativity fails on cosmological scales. If dark energy is the solution to the cosmic acceleration problem, then the logarithmic growth rate of structure $dlnG/dlna = \Omega^\gamma$, where $\Omega$ is the matter density independent of scale in a dark matter plus dark energy model. By combining measurements of the amplitude of redshift space, $\beta = (1/b) dlnG/dlna$ with measurements of galaxy bias, $b$, from cross-correlations with CMB lensing, redshift surveys will be able to determine the logarithmic growth rate as a function of scale and redshift. I will discuss the role of upcoming surveys in improving our ability to understand the origin of cosmic acceleration.