Ofer Lahav

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Correlation Function per Type dP / n [1+ξ(r)] dV ξ(r) = (r/r 0 ) -γ Why a power law? different slopes for blue and red explained by different halo Occupation numbers
Probing Dark Energy • Probe dark energy through the history of the expansion rate: H 2 (z) = H 2 0 [Ω M (1+z) 3 + Ω DE (1+z) 3 (1+w) ] (flat Universe) matter dark energy (constant w) P = w ρ • Comoving distance r(z) = ∫ dz/H(z) • Standard Candles d L(z) = (1+z) r(z) • Standard Rulers d A(z) = (1+z) −1 r(z) • Standard Population (volume) dV/dzdΩ = r 2 (z)/H(z) • The rate of growth of structure also determined by H(z) and by any modifications of gravity on large scales
Page 1 and 2: Large Scale Structure at Low Redshi
Page 3 and 4: LSS at low z • 2MRS/6dF The LG di
Page 6 and 7: 2MASS Galactic chart F
Page 8 and 9: 2MASS and follow-ups • 2MASS: 1.5
Page 10 and 11: Dipole - weighting schemes by Numbe
Page 12 and 13: Kocevski, Mullis & Ebeling, astro-p
Page 14 and 15: The expected rms bulk motion h V 2
Page 16 and 17: The revival of peculiar velocities
Page 18 and 19: 7 Abell clusters 77 groups (>8) 20
Page 20 and 21: From 2dF+CMB (6 parameter fit): Col
Page 22 and 23: Brief History of ‘Hot Dark Matter
Page 24 and 25: Data 2dFGRS Neutrino mass from Cosm
Page 26 and 27: The halo model - the ‘new biasing
Page 30 and 31: Imaging CFHTLS Supernovae SDSS Spec
Page 32 and 33: Input: magnitudes ANNz Collister &
Page 34 and 35: DES + VISTA griz+YJHKs filters 10σ
Page 36: Conclusions - in the Trio’s own w

Ofer Lahav

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