We present a method for calculating large numbers of power spectra C _ { \ell } and P ( k ) that accelerates CMBfast by a factor around 10 ^ { 3 } without appreciable loss of accuracy , then apply it to constrain 11 cosmological parameters from current Cosmic Microwave Background ( CMB ) and Large Scale Structure ( LSS ) data .
While the CMB alone still suffers from several degeneracies , allowing , e.g . , closed models with strong tilt and tensor contributions , the shape of the real space power spectrum of galaxies from the IRAS Point Source Catalogue Redshift ( PSCz ) survey breaks these degeneracies and helps place strong constraints on most parameters .
At 95 % confidence , the combined CMB and LSS data imply a baryon density 0.020 < \omega _ { b } < 0.037 , dark matter density 0.10 < \omega _ { dm } < 0.32 with a neutrino fraction f _ { \nu } < 38 \% , vacuum density \Omega _ { \Lambda } < 0.76 , curvature -0.19 < \Omega _ { k } < 0.10 , scalar tilt 0.86 < n _ { s } < 1.16 , and reionization optical depth \tau < 0.44 .
These joint constraints are quite robust , changing little when we impose priors on the Hubble parameter , tilt , flatness , gravity waves or reionization .
Adding nucleosynthesis and neutrino priors on the other hand tightens constraints considerably , requiring \Omega _ { \Lambda } > 0.49 and a red-tilt , n _ { s } < 1 .

The analysis allows a number of consistency tests to be made , all of which pass .
At the 95 % level , the flat scalar “ concordance model ” with \Omega _ { \Lambda } = 0.62 , \omega _ { dm } = 0.13 , \omega _ { b } = 0.02 , f _ { \nu } \sim 0 , n _ { s } = 0.9 , \tau = 0.1 , h = 0.63 is consistent with the CMB and LSS data considered here , with big bang nucleosynthesis , cluster baryon fractions and cluster abundance .
The inferred PSCz bias b \sim 1.2 agrees with the value estimated independently from redshift space distortions .
The inferred cosmological constant value agrees with the one derived independently from SN 1a studies .
Cosmology seems to be on the right track !