Seeing Dark Energy 10 Years Later

Details Seeing Dark Energy 10 Years Later Seeing Dark Energy 10 Years Later

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1166...73r&link_type=abstract

SOURCES AND DETECTION OF DARK MATTER AND DARK ENERGY IN THE UNIVERSE: Proceedings of the 8th UCLA Symposium. AIP Conference Pro

Mathematics

Logic

2

Dark Energy, Supernovae, Cosmology

Scientific paper

After Hubble's discovery of cosmic expansion, cosmologists expected that the mass and fate of the Universe would be revealed by its deceleration. In the 1990's two teams took up the challenge to measure the cosmic deceleration using yardsticks built from exploding stars called supernovae. I was a member of the High-z Team. In the fall of 1997 I was leading the reduction and analysis of our supernova data. After calibrating the relation between flux and redshift for nearby and distant supernovae, I used our data to calculate the normalized mass of the Universe, Ωm, required to cause the deceleration exhibited by the supernovae. The answer was (significantly) negative! This was my first indication that the expansion is accelerating. I then added Einstein's cosmological constant (a dark energy) to the mix. I found a nonvanishing cosmological constant at the 99.8% confidence level. In February 1998, Alex Filippenko and I presented these findings on behalf of the High-z Team (Alex spoke). We published our conclusions a few months later in Riess et al. 1998. Understanding the nature of the dark energy poses an enormous challenge for physics and astronomy alike.

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