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The tomographic AP method is so far the best method in separating theAlcock-Paczynski (AP) signal from the redshift space distortion (RSD) effectsand deriving powerful constraints on cosmological parameters using the$\lesssim40h^{-1}\ \rm Mpc$ clustering region. To guarantee that the method canbe easily applied to the future large scale structure (LSS) surveys, we studythe possibility of estimating the systematics of the method using fastsimulation method. The major contribution of the systematics comes from thenon-zero redshift evolution of the RSD effects, which is quantified by$\hat\xi_{\Delta s}(\mu,z)$ in our analysis, and estimated using theBigMultidark exact N-body simulation and approximate COLA simulation samples.We find about 5\%/10\% evolution when comparing the $\hat\xi_{\Delta s}(\mu,z)$measured as $z=0.5$/$z=1$ to the measurements at $z=0$. We checked theinaccuracy in the 2pCFs computed using COLA, and find it 5-10 times smallerthan the intrinsic systematics of the tomographic AP method, indicating thatusing COLA to estimate the systematics is good enough. Finally, we test theeffect of halo bias, and find $\lesssim$1.5\% change in $\hat\xi_{\Delta s}$when varying the halo mass within the range of $2\times 10^{12}$ to $10^{14}$$M_{\odot}$. We will perform more studies to achieve an accurate and efficientestimation of the systematics in redshift range of $z=0-1.5$.

astrophysical journal/the astrophysical journal

Cosmological constraints from the redshift dependence of the  Alcock-Paczynski effect: Possibility of estimateing the non-linear  systematics using fast simulations