Cosmological constraints from baryon acoustic oscillations and clustering of large-scale structure

We constrain cosmological parameters using combined measurements of the baryon acoustic oscillation (BAO) feature in the correlation function of galaxies and Ly alpha absorbers that together cover 0.1 < z < 2.4. The BAO position measurements alone - without fixing the absolute sound horizon 'standard ruler' length with cosmic microwave background (CMB) data - constrain (m) = 0.303 +/- 0.040 (68 per cent confidence) for a flat Lambda cold dark matter (Lambda CDM) model, and w = - 1.06(-0.32)(+0.330), Omega(m) = 0.292(-0.040)(+0.045) for a flat wCDM model. Adding other large-scale structure (LSS) clustering constraints - correlation function shape, the Alcock-Paczynski test and growth rate information - to the BAO considerably tightens constraints ((m) = 0.290 +/- 0.019, H-0 = 67.5 +/- 2.8 km s(-1) Mpc(-1), Sigma(8) = 0.80 +/- 0.05 for Lambda CDM, and w = -1.14 +/- 0.19 for wCDM). The LSS data mildly prefer a lower value of H-0, and a higher value of (m), than local distance ladder and Type IA supernovae (SNe) measurements, respectively. While tension in the combined CMB, SNe and distance ladder data appear to be relieved by allowing w < -1, this freedom introduces tension with the LSS Sigma(8) constraint from the growth rate of matter fluctuations. The combined constraint on w from CMB, BAO and LSS clustering for a flat wCDM model is w = -1.03 +/- 0.06.