AR_final file_2018-19

Figure 2: Comparison of clustering and abundance computed using HOD fitting functions with measurements. (Left panel) Projected correlation function for different magnitude thresholds. Solid circles with error bars show measurements from Zehavi, et al. 2011 . Solid curves show the correlation function computed using fitting form of the HOD parameters combined with the simulation-based theoretical model of halo clustering. (For clarity, 0 . 25dex staggering has been introduced in the measurements and models for all thresholds other than M r < − 20 . 5.) (Right panel) Cumulative luminosity function as a function of magnitude. Black solid line shows the curve obtained from the theoretical model and red circles show the measurements from Zehavi, et al. 2011 . Om(z) 0.15 0.2 0.25 0.3 0.35 0.4 z 0.2 0.4 0.6 0.8 1 1.2 Figure 3: Shows the Om ( z ) plot (best fit and median with 1 − σ and 2 − σ confidence regions) for the present estimated values of the coefficients of the Taylor expansion of the Hubble parameter. ( 59 )