The WiggleZ Dark Energy Survey - Berkeley Cosmology Group

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Other analyses in progress ... • Cosmo-MC module for P(k) and data release • Limits on modified gravity theories • Higher-order clustering (non-Gaussianity , skewness) • BAO reconstruction and 2D fitting for DA(z) / H(z) • Clusters and voids • Cosmic topology (genus) • Turnover in power spectrum (early-universe physics)
Summary of results from <strong>WiggleZ</strong> • Baryon acoustic peak detected at ~3-sigma significance and measures cosmic distances to z=0.8 • <strong>WiggleZ</strong> gives most accurate growth measurement, extending previous work to higher redshift • Alcock-Paczynski effect allows direct reconstruction of H(z) at high redshift • G.R. + Lambda models remain a good fit • If dark energy behaves as Lambda, what is its physics?
Page 1 and 2: The WiggleZ Dark Energy Survey •
Page 3 and 4: The WiggleZ Survey (observational)
Page 5 and 6: Survey comparison
Page 7 and 8: Survey design • Follow up UV-sele
Page 9 and 10: Survey design
Page 11 and 12: Target Galaxy selection targets (Cr
Page 13 and 14: The baryon acoustic peak in WiggleZ
Page 15 and 16: BAO Hubble diagram arXiv:1108.2635
Page 17 and 18: The Comparison dark energy of BAO p
Page 19 and 20: Cosmological parameter fits arXiv:1
Page 21 and 22: Cosmological parameter fits Spatial
Page 23 and 24: Redshift-space distortions 4 • Do
Page 25 and 26: Redshift-space distortions in Wiggl
Page 27 and 28: Growth rate measurements from Wiggl
Page 29 and 30: Density and velocity power spectra
Page 31 and 32: Alcock-Paczynski measurement in Wig
Page 33 and 34: Alcock-Paczynski measurement in Wig
Page 35 and 36: Non-parametric expansion history ar
Page 37 and 38: Non-parametric expansion history ar
Page 39: Transition to cosmic homogeneity Sc

The WiggleZ Dark Energy Survey - Berkeley Cosmology Group

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