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The Baryon Acoustic Oscillations (BAO) are one of the most used probes tounderstand the accelerated expansion of the Universe. Traditional methods relyon fiducial model information within their statistical analysis, which may be aproblem when constraining different families of models. The aim of this work isto provide a method that constrains $\theta_{BAO}$ through a model-independentand compare parameter estimation of the angular correlation function polynomialapproach, using the covariance matrix from the galaxy sample from thin redshiftbins, with the usual mock sample covariance matrix. We proposed a differentapproach to finding the BAO angular feature revisiting previous work in theliterature, we take the bias between the correlation function between the binsand the whole sample. We used widths of $\delta z = 0.002$ separation for allsamples as the basis for a sample covariance matrix weighted by the statisticalimportance of the redshift bin. We propose a different weighting scheme basedonly on random pair counting. We also propose an alternate shift parameterbased only on the data. Each sample belongs to the Sloan Digital Sky SurveyLuminous Red Galaxies (LRG): BOSS1, BOSS2, and eBOSS, with effective redshift$z_{eff}$: 0.35, 0.51, 0.71, respectively, and different numbers of bins with50, 100, and 200 respectively. In addition, we correct the angular separationfrom the polynomial fit ($\theta_{fit}$) that encodes the BAO feature with abias function obtained by comparing each bin correlation function with thecorrelation function of the whole set. We also tested the same correctionchoosing the bin at $z_{eff}$ and found that for eBOSS $\theta_{BAO}$ is in $1\sigma$ agreement with the Planck 18 model. BOSS1 and BOSS2 $\theta_{BAO}$agreed in $1\sigma$ with the Pantheon+ & S$H_0$ES Flat$\Lambda$CDM model, intension with Planck 18.

Angular Correlation Function from sample covariance with BOSS and eBOSS LRG