PIRSA:15030106

Video URL

https://pirsa.org/15030106

Looking for non-dark matter: Sunyaev-Zeldovich-gravitational-lensing cross correlations

Murray, N. (2015). Looking for non-dark matter: Sunyaev-Zeldovich-gravitational-lensing cross correlations. Perimeter Institute for Theoretical Physics. https://pirsa.org/15030106

Murray, Norman. Looking for non-dark matter: Sunyaev-Zeldovich-gravitational-lensing cross correlations. Perimeter Institute for Theoretical Physics, Mar. 10, 2015, https://pirsa.org/15030106 

          @misc{ scivideos_PIRSA:15030106,
            doi = {10.48660/15030106},
            url = {https://pirsa.org/15030106},
            author = {Murray, Norman},
            keywords = {Cosmology},
            language = {en},
            title = {Looking for non-dark matter: Sunyaev-Zeldovich-gravitational-lensing cross correlations},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2015},
            month = {mar},
            note = {PIRSA:15030106 see, \url{https://scivideos.org/index.php/pirsa/15030106}}
          }

Norman Murray Canadian Institute for Theoretical Astrophysics (CITA)

Talk numberPIRSA:15030106
DOI10.48660/15030106
Source RepositoryPIRSA
Collection
Talk Type Scientific Series
Subject

Abstract

Visible matter consists mostly of hydrogen and helium, only a small fraction
of which is in stars. Until recently, the bulk of the gas in the local
universe was in fact not seen. In the largest structures, massive galaxy
clusters, the gas is seen via its x-ray emission, but in the much more
numerous groups and isolated galaxies, it has not been possible to detect
it. I will describe how, in the last year or so, the situation has changed,
with the detection of a cross-correlation between the thermal SZ effect and
lensing maps, and through the stacking of SZ images at the locations of
galaxies. These and similar techniques will tell us about the physics by
which stars and massive black holes heat and move gas in and around the
halos of galaxies and cluster, and will allow for tighter constraints on the
value of the primordial power spectrum (sigma_8).