Alcock-Paczynski Test with the Evolution of Redshift-Space Galaxy Clustering Anisotropy. (arXiv:1904.05503v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Park_H/0/1/0/all/0/1">Hyunbae Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Park_C/0/1/0/all/0/1">Changbom Park</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sabiu_C/0/1/0/all/0/1">Cristiano G. Sabiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_X/0/1/0/all/0/1">Xiao-dong Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hong_S/0/1/0/all/0/1">Sungwook E. Hong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kim_J/0/1/0/all/0/1">Juhan Kim</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tonegawa_M/0/1/0/all/0/1">Motonari Tonegawa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zheng_Y/0/1/0/all/0/1">Yi Zheng</a>
We develop an improved Alcock-Paczynski (AP) test method that uses the
redshift-space two-point correlation function (2pCF) of galaxies. Cosmological
constraints can be obtained by examining the redshift dependence of the
normalized 2pCF, which should not change apart from the expected small
non-linear evolution. An incorrect choice of cosmology used to convert redshift
to comoving distance will manifest itself as redshift-dependent 2pCF. Our
method decomposes the redshift difference of the two-dimensional correlation
function into the Legendre polynomials whose amplitudes are modeled by radial
fitting functions. Our likelihood analysis with this 2-D fitting scheme
tightens the constraints on $Omega_m$ and ${w}$ by $sim 40%$ compared to the
method of Li et al. (2016, 2017, 2018) that uses one dimensional angular
dependence only. We also find that the correction for the non-linear evolution
in the 2pCF has a non-negligible cosmology dependence, which has been neglected
in previous similar studies by Li et al.. With an accurate accounting for the
non-linear systematics and use of full two-dimensional shape information of the
2pCF down to scales as small as $5~h^{-1}{rm Mpc}$ it is expected that the AP
test with redshift-space galaxy clustering anisotropy can be a powerful method
to constraining the expansion history of the universe.
We develop an improved Alcock-Paczynski (AP) test method that uses the
redshift-space two-point correlation function (2pCF) of galaxies. Cosmological
constraints can be obtained by examining the redshift dependence of the
normalized 2pCF, which should not change apart from the expected small
non-linear evolution. An incorrect choice of cosmology used to convert redshift
to comoving distance will manifest itself as redshift-dependent 2pCF. Our
method decomposes the redshift difference of the two-dimensional correlation
function into the Legendre polynomials whose amplitudes are modeled by radial
fitting functions. Our likelihood analysis with this 2-D fitting scheme
tightens the constraints on $Omega_m$ and ${w}$ by $sim 40%$ compared to the
method of Li et al. (2016, 2017, 2018) that uses one dimensional angular
dependence only. We also find that the correction for the non-linear evolution
in the 2pCF has a non-negligible cosmology dependence, which has been neglected
in previous similar studies by Li et al.. With an accurate accounting for the
non-linear systematics and use of full two-dimensional shape information of the
2pCF down to scales as small as $5~h^{-1}{rm Mpc}$ it is expected that the AP
test with redshift-space galaxy clustering anisotropy can be a powerful method
to constraining the expansion history of the universe.
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