2019/08/28 by Xiaolin Luo, Ziyong Wu, Xiao-Dong Li +3 · 1 citation
Physics and Astronomy · #astro-ph.CO
paper · pdf · doi:10.3847/1538-4357/ab50b5
7 pages, 7 figures
arxiv created 2019/08/28 · arxiv updated 2020/01/08
The tomographic Alcock-Paczynski (AP) method utilizes the redshift evolution of the AP distortion to place constraints on cosmological parameters. It has proved to be a robust method that can separate the AP signature from the redshift space distortion (RSD) effect, and deliver powerful cosmological constraints using the \lesssim 40h-1 \rm Mpc clustering region. In previous works, the tomographic AP method was performed via the anisotropic 2-point correlation function statistic. In this work we consider the feasibility of conducting the analysis in the Fourier domain and examine the pros and cons of this approach. We use the integrated galaxy power spectrum (PS) as a function of direction, PΔk(μ), to quantify the magnitude of anisotropy in the large-scale structure clustering, and use its redshift variation to do the AP test. The method is tested on the large, high resolution Big-MultiDark Planck (BigMD) simulation at redshifts z=0-1, using the underlying true cosmology Ωm=0.3071, w=-1. Testing the redshift evolution of PΔk(μ) in the true cosmology and cosmologies deviating from the truth with δΩm=0.1, δw=0.3, we find that the redshift evolution of the AP distortion overwhelms the effects created by the RSD by a factor of ∼1.7-3.6. We test the method in the range of k∈(0.2,1.8) h \rm Mpc-1, and find that it works well throughout the entire regime. We tune the halo mass within the range 2× 1013 to 1014 M\odot, and find that the change of halo bias results in \lesssim 5 % change in PΔk(μ), which is less significant compared with the cosmological effect. Our work shows that it is feasible to conduct the tomographic AP analysis in the Fourier space.