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Abstract

We present angular diameter measurements obtained by measuring the position of baryon acoustic oscillations (BAO) in an optimized sample of galaxies from the first three years of Dark Energy Survey data (DES Y3). The sample consists of 7 million galaxies distributed over a footprint of 4100  deg² with 0.6<z _photo <1.1 and a typical redshift uncertainty of 0.03(1+z). The sample selection is the same as in the BAO measurement with the first year of DES data, but the analysis presented here uses three times the area, extends to higher redshift, and makes a number of improvements, including a fully analytical BAO template, the use of covariances from both theory and simulations, and an extensive preunblinding protocol. We used two different statistics; angular correlation function and power spectrum, and validate our pipeline with an ensemble of over 1500 realistic simulations. Both statistics yield compatible results. We combine the likelihoods derived from angular correlations and spherical harmonics to constrain the ratio of comoving angular diameter distance D_M at the effective redshift of our sample to the sound horizon scale at the drag epoch. We obtain D_M(z_eff=0.835)/r_d=18.92±0.51, which is consistent with, but smaller than, the Planck prediction assuming flat ΛCDM, at the level of 2.3σ. The analysis was performed blind and is robust to changes in a number of analysis choices. It represents the most precise BAO distance measurement from imaging data to date, and is competitive with the latest transverse ones from spectroscopic samples at z>0.75. When combined with DES 3x2pt+SNIa, they lead to improvements in H₀ and Ω_m constraints by ∼20%.