We analyze the 2D correlation function of the SDSS-III Baryon Oscillation Spectroscopic Survey ( BOSS ) CMASS sample of massive galaxies of the ninth data release to measure cosmic expansion H and the angular diameter distance D _ { A } at a mean redshift of \langle { z } \rangle = 0.57 . We apply , for the first time , a new correlation function technique called clustering wedges \xi _ { \Delta \mu } ( s ) . Using a physically motivated model , the anisotropic baryonic acoustic feature in the galaxy sample is detected at a significance level of 4.7 \sigma compared to a featureless model . The baryonic acoustic feature is used to obtain model independent constraints cz / H / r _ { \mathrm { s } } = 12.28 \pm 0.82 ( 6.7 \% accuracy ) and D _ { A } / r _ { \mathrm { s } } = 9.05 \pm 0.27 ( 3.0 \% ) with a correlation coefficient of -0.5 , where r _ { s } is the sound horizon scale at the end of the baryonic drag era . We conduct thorough tests on the data and 600 simulated realizations , finding robustness of the results regardless of the details of the analysis method . Combining with r _ { s } constraints from the Cosmic Microwave Background we obtain H ( 0.57 ) = 90.8 \pm 6.2 kms ^ { -1 } Mpc ^ { -1 } and D _ { A } ( 0.57 ) = 1386 \pm 45 Mpc . We use simulations to forecast results of the final BOSS CMASS data set . We apply the reconstruction technique on the simulations demonstrating that the sharpening of the anisotropic baryonic acoustic feature should improve the detection as well as tighten constraints of H and D _ { A } by \sim 30 \% on average .