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With the advent of very large volume, wide‐angle photometric redshift surveys like e.g. Panoramic Survey Telescope and Rapid Response System, Dark Energy Survey or Physics of the Accelerating Universe, which aim at using the spatial distribution of galaxies as a means to constrain the equation of state parameter of dark energy,  w  DE , it has become extremely important to understand the influence of redshift inaccuracies on the measurement. We have developed a new model for the anisotropic two‐point large‐scale ( r ≳64   h  −1  Mpc) correlation function    ξ  (   r  p   ,  π  )   , in which non‐linear structure growth and non‐linear coherent infall velocities are taken into account, and photometric redshift errors can easily be incorporated. In order to test its validity and investigate the effects of photometric redshifts, we compare our model with the correlation function computed from a suite of 50 large‐volume, moderate‐resolution numerical  N ‐body simulation boxes, where we can not only perform the analysis in real and redshift space, but also simulate the influence of a Gaussian redshift error distribution with an absolute rms of σ  z   = 0.015, 0.03, 0.06 and 0.12, respectively. We conclude that for the given volume ( V  box  =2.4  h  −3  Gpc 3 ) and number density (    n  ¯   ≈  1.25  ×   10   −  4) of objects the full shape of    ξ  (   r  p   ,  π  )    is modelled accurately enough to use it to derive unbiased constraints on the equation of state parameter of dark energy  w  DE  and the linear bias  b , even in the presence of redshift errors of the order of σ  z   = 0.06.

A model of the anisotropic correlation function ξ ( r p , π) in redshift space including redshift errors