We develop a new methodology called double-probe analysis with the aim of minimizing informative priors in the estimation of cosmological parameters .
Using our new methodology , we extract the dark-energy-model-independent cosmological constraints from the joint data sets of Baryon Oscillation Spectroscopic Survey ( BOSS ) galaxy sample and Planck cosmic microwave background ( CMB ) measurement .
We measure the mean values and covariance matrix of \ { R , l _ { a } , \Omega _ { b } h ^ { 2 } , n _ { s } , log ( A _ { s } ) , \Omega _ { k } , H ( z ) , D _ { A } ( z ) , f ( z ) \sigma _ { 8 } ( z ) \ } , which give an efficient summary of Planck data and 2-point statistics from BOSS galaxy sample .
The CMB shift parameters are R = \sqrt { \Omega _ { m } H _ { 0 } ^ { 2 } } r ( z _ { * } ) , and l _ { a } = \pi r ( z _ { * } ) / r _ { s } ( z _ { * } ) , where z _ { * } is the redshift at the last scattering surface , and r ( z _ { * } ) and r _ { s } ( z _ { * } ) denote our comoving distance to z _ { * } and sound horizon at z _ { * } respectively ; \Omega _ { b } is the baryon fraction at z = 0 .
The advantage of this method is that we do not need to put informative priors on the cosmological parameters that galaxy clustering is not able to constrain well , i.e . \Omega _ { b } h ^ { 2 } and n _ { s } .

Using our double-probe results , we obtain \Omega _ { m } = 0.304 \pm 0.009 , H _ { 0 } = 68.2 \pm 0.7 , and \sigma _ { 8 } = 0.806 \pm 0.014 assuming \Lambda CDM ; \Omega _ { k } = 0.002 \pm 0.003 assuming oCDM ; w = -1.04 \pm 0.06 assuming w CDM ; \Omega _ { k } = 0.002 \pm 0.003 and w = -1.00 \pm 0.07 assuming o w CDM ; and w _ { 0 } = -0.84 \pm 0.22 and w _ { a } = -0.66 \pm 0.68 assuming w _ { 0 } w _ { a } CDM .
The results show no tension with the flat \Lambda CDM cosmological paradigm .
By comparing with the full-likelihood analyses with fixed dark energy models , we demonstrate that the double-probe method provides robust cosmological parameter constraints which can be conveniently used to study dark energy models .

We extend our study to measure the sum of neutrino mass using different methodologies including double probe analysis ( introduced in this study ) , the full-likelihood analysis , and single probe analysis .
From the double probe analysis , we obtain \Sigma m _ { \nu } < 0.10 / 0.22 ( 68 % /95 % ) assuming \Lambda CDM and \Sigma m _ { \nu } < 0.26 / 0.52 ( 68 % /95 % ) assuming w CDM .
This paper is part of a set that analyses the final galaxy clustering dataset from BOSS .