Physical Evidence for Dark Energy

A. J. Connolly (UPitt); A. S. Szalay (JHU); A. Stebbins (FNAL); C. J. Miller (CMU); D. J. Eisenstein (Steward); D. Johnston (CfCP); E. S. Sheldon (CfCP); et al. (SDSS Collaboration); I. Csabai (Eotvos); I. Szapudi (Hawaii)

Physical Evidence for Dark Energy

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arxiv astro-ph/0307335 v2 pith:JCIQ7H52 submitted 2003-07-18 astro-ph hep-ex

R. Scranton , A. J. Connolly (UPitt) , R. C. Nichol (CMU) , A. Stebbins (FNAL) , I. Szapudi (Hawaii) , D. J. Eisenstein (Steward) , N. Afshordi (Princeton) , T. Budavari (JHU)

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I. Csabai (Eotvos) J. A. Frieman (FNAL) J. E. Gunn (Princeton) D. Johnston (CfCP) Y. Loh R. H. Lupton (Princeton) C. J. Miller (CMU) E. S. Sheldon (CfCP) R. S. Sheth (UPitt) A. S. Szalay (JHU) M. Tegmark Y. Xu (UPenn) et al. (SDSS collaboration)

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We present measurements of the angular cross-correlation between luminous red galaxies from the Sloan Digital Sky Survey and the cosmic microwave background temperature maps from the Wilkinson Microwave Anisotropy Probe. We find a statistically significant achromatic positive correlation between these two data sets, which is consistent with the expected signal from the late Integrated Sachs-Wolfe (ISW) effect. We do not detect any anti-correlation on small angular scales as would be produced from a large Sunyaev-Zel'dovich (SZ) effect, although we do see evidence for some SZ effect for our highest redshift samples. Assuming a flat universe, our preliminary detection of the ISW effect provides independent physical evidence for the existence of dark energy.

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