📝 SummarXiv

Abstract

We employ a model-independent approach in both the correlation function estimation and the angular BAO feature estimation by computing the angular two-point correlation function. First, we conducted a series of tests to the available DESI tracers to check their representativeness to angular clustering; the result was that, considering the completeness of the first data release across the footprint, we could only make use of the BGS sample for the effective redshifts 0.21 (BGS1) and 0.25 (BGS2). For a reliable analysis in such low redshift, we consider Lagrangian Perturbation Theory at first order on our mocks, which approximately reproduces the expected non-linearities, and generate the corresponding random catalogues. We use a purely statistical method to correct the projection effects and find that our results show reasonable agreement with the $\theta_{\rm BAO}$ expected by the CPL parameters obtained by DESI DR1, being BGS1 $11.78 \pm 1.12$ degrees and BGS2 $11.81 \pm 1.20$ degrees. This means a tension at the $1.5\sigma$ ($2.6\sigma$) level for BGS1 (BGS2) CPL parametrization, while a $2\sigma$ ($3.3\sigma$) discrepancy within the predicted by $\Lambda$CDM. We conclude that, with the current sample available, the use of an angular correlation function serving as the BAO probe, although prefers the CPL parametrization, does not provide conclusive results regarding the best cosmological model.