| 作者: |
Li, Xiao-Dong; Miao, Haitao; Wang, Xin; Zhang, Xue; Fang, Feng; Luo, Xiaolin; Huang, Qing-Guo; Li, Miao |
| 摘要: |
The tomographic Alcock-Paczynski (AP) test is a robust large-scale structure (LSS) measurement that receives little contamination from the redshift space distortion. It has placed tight cosmological constraints by using small and intermediate clustering scales of the LSS data. However, previous works have neglected the cross-correlation among different redshift bins, which could cause the statistical uncertainty being underestimated by similar to 20%. In this work, we further improve this method by including this multi-redshift's full correlation. We apply it to the SDSS DR12 galaxies sample and find out that, for Lambda CDM, the combination of AP with the Planck+BAO data set slightly reduces (within 1 sigma) Omega(m) to 0.304 +/- 0.007 (68.3% CL). This then leads to a larger H-0 and also mildly affects Omega(b) h(2) and n(s) as well as the derived parameters z(*), r(*), and z(re) but not tau, A(s), and sigma(8). For the flat wCDM model, our measurement gives Omega(m) = 0.301 +/- 0.010 and w = -1.090 +/- 0.047, where the additional AP measurement reduces the error budget by similar to 25%. When including more parameters into the analysis, the AP method also improves the constraints on Omega(k), Sigma(m)mu, and N-eff by 20%-30%. Early universe parameters such as dn(s)/d ln k and r, however, are unaffected. Assuming the dark energy equation of state w = w(0) +w(a) z/1+z , the Planck+BAO+SNe Ia+H-0+AP data sets prefer a dynamical dark energy at approximate to 1.5 sigma CL. Finally, we forecast the cosmological constraints expected from the DESI galaxy survey and find that combining AP with the CMB+BAO method would improve the w(0)-w(a) constraint by a factor of similar to 10. |
