Measuring Dark Energy Clustering with CMB-Galaxy Correlations

Details Measuring Dark Energy Clustering with CMB-Galaxy Correlations Measuring Dark Energy Clustering with CMB-Galaxy Correlations

2004-08-24

arxiv.org/abs/astro-ph/0408456v2

Phys.Rev.D70:123002,2004

Astronomy and Astrophysics

Astrophysics

8 pages, 9 figures changes reflect PRD published version

Scientific paper

10.1103/PhysRevD.70.123002

The integrated Sachs-Wolfe (ISW) effect in the cosmic microwave background (CMB) as measured through its correlation with galaxies provides a unique opportunity to study the dynamics of the dark energy through its large scale clustering properties. Ultimately, a deep all-sky galaxy survey out to z~2 can make a 10sigma or ~10% measurement of the correlation and limit ~3% changes in the gravitational potential or total density fluctuation due to dark energy clustering on the Gpc scale. A canonical single scalar field or quintessence model predicts that these clustering effects will appear on the horizon scale with a strength that reflects the evolution of the dark energy density. In terms of a constant equation of state, this would allow tests of the quintessence prediction for models where |1+w| > 0.05.

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