The WiggleZ Dark Energy Survey - Berkeley Cosmology Group

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Stacking the BAO measurements! 5-sigma detection significance arXiv:1108.2635
Redshift-space distortions 4 • Does a cosmological model produce self-consistent cosmic growth and expansion histories? coherent flows virialized motions 4. RESULTS: I. 2MRS VELOCITY FIELD AND COMPARISON WITH MEASURED DISTANCES In a reconstruction of the velocity field using MAK based on priors, we fix Ωm = 0.258 as indicated by WMAP5 results and set the bias parameter (Kaiser & Lahav 1989) to 1 using 2dF and SDSS/WMAP results (Dunkley et al. 2008; Tegmark et al. 2004; Cole et al. 2005). The velocity of each galaxy in 2MRS is reconstructed using these parameters. The first approach is to measure the 3,000 km s −1 bulk flow in both cases as it is done in Section 4.1. In a parallel approach, discussed in Section 4.2, we leave Ωm free and then constrain its value by maximizing the correlation between the reconstructed and observed peculiar velocities. The 2MRS velocities are reconstructed using a uniform grid of size 130 3 sampling a cubic volume of 260 3 h −3 Mpc 3 as shown in Fig. 2. The motion of the Local Group is obtained using an interpolation based on the adaptive weighting of the peculiar velocities of the objects that lie within 4-5h −1 Mpc from us (method detailed in Appendix C). We have checked that increasing the reconstruction resolution does not significantly change the reconstructed velocities. −1
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: Cosmological parameter fits Spatial
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 and 40: Transition to cosmic homogeneity Sc
Page 41: Summary of results from WiggleZ •

The WiggleZ Dark Energy Survey - Berkeley Cosmology Group

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