PIRSA:15080002

Video URL

https://pirsa.org/15080002

Probing Dark Energy with the Canadian Hydrogen Intensity Mapping Experiment (CHIME)

Shaw, R. (2015). Probing Dark Energy with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). Perimeter Institute for Theoretical Physics. https://pirsa.org/15080002

Shaw, Richard. Probing Dark Energy with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). Perimeter Institute for Theoretical Physics, Aug. 12, 2015, https://pirsa.org/15080002 

          @misc{ scivideos_PIRSA:15080002,
            doi = {10.48660/15080002},
            url = {https://pirsa.org/15080002},
            author = {Shaw, Richard},
            keywords = {Cosmology, Other Physics},
            language = {en},
            title = {Probing Dark Energy with the Canadian Hydrogen Intensity Mapping Experiment (CHIME)},
            publisher = {Perimeter Institute for Theoretical Physics},
            year = {2015},
            month = {aug},
            note = {PIRSA:15080002 see, \url{https://scivideos.org/pirsa/15080002}}
          }

Richard Shaw University of British Columbia

Talk numberPIRSA:15080002
DOI10.48660/15080002
Source RepositoryPIRSA
Collection
Talk Type Conference
Subject

Abstract

CHIME will use the 21cm emission line of neutral hydrogen to map large-scale structure between redshifts of 0.8 and 2.5. By measuring BAO we will place constraints on the dark energy equation of state as it begins to dominate the expansion of the Universe, particularly at redshifts poorly probed by current BAO surveys. In this talk I will introduce CHIME, a transit radio interferometer designed specifically for this purpose. I will discuss its goals and describe the powerful new analysis techniques we have developed to confront the many challenges of such observations, in particular removal of astrophysical foregrounds which are six orders of magnitude larger than the 21cm signal. A smaller 40m x 37m pathfinder telescope is currently operating at the DRAO in Penticton, BC, and the construction of the full-sized 80m x 100m instrument commenced in early 2015. I will report on current progress, and the lessons already learned.