PIRSA:13120054

Supersymmetry, Non-thermal Dark Matter and Precision Cosmology

Watson, S. (2013). Supersymmetry, Non-thermal Dark Matter and Precision Cosmology. Perimeter Institute. https://pirsa.org/13120054

Watson, Scott. Supersymmetry, Non-thermal Dark Matter and Precision Cosmology. Perimeter Institute, Dec. 05, 2013, https://pirsa.org/13120054 

          @misc{ pirsa_PIRSA:13120054,
            doi = {10.48660/13120054},
            url = {https://pirsa.org/13120054},
            author = {Watson, Scott},
            keywords = {Cosmology},
            language = {en},
            title = {Supersymmetry, Non-thermal Dark Matter and Precision Cosmology},
            publisher = {Perimeter Institute},
            year = {2013},
            month = {dec},
            note = {PIRSA:13120054 see, \url{https://pirsa.org}}
          }

Scott Watson Syracuse University

Talk number PIRSA:13120054
DOI 10.48660/13120054
Collection
Talk Type Scientific Series
Subject

Abstract

Within the Minimal Supersymmetric Standard Model (MSSM), LHC bounds suggest that scalar superpartner masses are far above the electroweak scale. Given a high superpartner mass, nonthermal dark matter is a viable alternative to WIMP dark matter generated via freezeout. In the presence of moduli fields nonthermal dark matter production is associated with a long matter dominated phase, modifying the spectral index and primordial tensor amplitude relative to those in a thermalized primordial universe. Nonthermal dark matter can have a higher self-interaction cross-section than its thermal counterpart, enhancing astrophysical bounds on its annihilation signals. I will review recent progress in this program, and discuss how we can constrain the contributions to the neutralino mass from the bino, wino and higgsino using existing astrophysical bounds and direct detection experiments for models with nonthermal neutralino dark matter. Using these constraints we will then see how expected changes to inflationary observables result from the nonthermal phase.