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Galaxy clustering data provide a powerful probe of dark energy. We examine how the constraints on the scaled expansion history of the Universe,  x  h ( z ) = H ( z ) s  (with  s  denoting the sound horizon at the drag epoch), and the scaled angular diameter distance,  x  d ( z ) = D  A ( z )/ s , depend on the methods used to analyse the galaxy clustering data. We find that using the observed galaxy power spectrum,   P  obs  g (  k  ) ,  x  h ( z ) and  x  d ( z ) are measured more accurately and are significantly less correlated with each other, compared to using only the information from the baryon acoustic oscillations (BAO) in   P  obs  g (  k  ) . Using the { x  h ( z ),  x  d ( z )} from   P  obs  g (  k  )  gives a Dark Energy Task Force (DETF) dark energy figure of merit (FoM) approximately a factor of 2 larger than using the { x  h ( z ),  x  d ( z )} from BAO only; this provides a robust conservative method to go beyond BAO only in extracting dark energy information from galaxy clustering data.  We find that a Stage IV galaxy redshift survey, with 0.7 &lt;  z  &lt; 2 over 15 000 (deg) 2 , can measure  with high precision [where  f  g ( z ) and  G ( z ) are the linear growth rate and factor of large‐scale structure, respectively, and  is the dimensionless normalization of   P  obs  g (  k  ) ], when redshift‐space distortion information is included. The measurement of  provides a powerful test of gravity, and significantly boosts the dark energy FoM when general relativity is assumed.

Robust constraints on dark energy and gravity from galaxy clustering data