Galaxies_BigBang_Dark Matter
Acceleration of Universe Background level Evolution of expansion: H(a), w(a) degeneracy: DE & MG Perturbation level Evolution of inhomogeneity:
15 The Big Bang Where do we come from, where are we going?
18 The Big Bang Where do we come from, where are we going?
Coma Cluster Treasury Survey
Chapter 16: Other Galaxies
Jennifer Lotz Hubble Science Briefing Jan. 16, 2014
Large-scale Structure: Theory & Observations
Coma Cluster Treasury Survey Alister W. Graham (Swinburne), Helmut Jerjen (ANU), Terry J. Bridges (AAO & Aust. Gemini Office) and David Carter (P.I.),
Observational Probes of Dark Energy Timothy McKay University of Michigan Department of Physics Observational cosmology: parameters (H 0, 0 ) => evolution.
Large-scale Structure: Theory & Observations Josh Frieman Structure Formation & Evolution, Santiago, October 2002.
Jennifer Lotz Hubble Science Briefing Jan. 16, 2014 Exploring the Depths of the Universe.
