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We apply a new model for the spherically averaged correlation function at large pair separations to the measurement of the clustering of luminous red galaxies (LRGs) made from the Sloan Digital Sky Survey by Cabre &amp; Gaztañaga. Our model takes into account the form of the baryonic acoustic oscillation peak and the large‐scale shape of the correlation function. We perform a Monte Carlo Markov chain analysis for different combinations of data sets and for different parameter sets. When used in combination with a compilation of the latest cosmic microwave background (CMB) measurements, the LRG clustering and the latest supernovae results give constraints on cosmological parameters which are comparable and in remarkably good agreement, resolving the tension reported in some studies. The best‐fitting model in the context of a flat, Λ cold dark matter cosmology is specified by  Ω m = 0.261 ± 0.013, Ω b = 0.044 ± 0.001,  n  s = 0.96 ± 0.01,  H  0 = 71.6 ± 1.2 km s −1  Mpc −1   and  σ 8 = 0.80 ± 0.02 . If we allow the time‐independent dark energy equation of state parameter to vary, we find results consistent with a cosmological constant at the 5 per cent level using all data sets:   w  DE =−0.97 ± 0.05 . The large‐scale structure measurements by themselves can constrain the dark energy equation‐of‐state parameter to   w  DE =−1.05 +0.16  −0.15  , independently of CMB or supernovae data. We do not find convincing evidence for an evolving equation of state. We provide a set of ‘extended distance priors’ that contain the most relevant information from the CMB power spectrum and the shape of the LRG correlation function which can be used to constrain dark energy models and spatial curvature. Our model should provide an accurate description of the clustering even in much larger, forthcoming surveys, such as those planned with NASA's JDEM or ESA's Euclid mission.

Cosmological parameter constraints from SDSS luminous red galaxies: a new treatment of large‐scale clustering