Dark Energy Survey Year 3 Results: Measurement of the Baryon Acoustic Oscillations with Three-dimensional Clustering
Creators: name: Chan, K. C.
name: Avila, S.
name: Rosell, A. Carnero
name: Ferrero, I.
name: Elvin-Poole, J.
name: Sanchez, E.
name: Camacho, H.
name: Porredon, A.
name: Crocce, M.
name: Abbott, T. M. C.
name: Aguena, M.
name: Allam, S.
name: Andrade-Oliveira, F.
name: Bertin, E.
name: Bocquet, S.
name: Brooks, D.
name: Burke, D. L.
name: Kind, M. Carrasco
name: Carretero, J.
name: Castander, F. J.
name: Cawthon, R.
name: Conselice, C.
name: Costanzi, M.
name: Pereira, M. E. S.
name: De Vicente, J.
name: Desai, S.
name: Diehl, H. T.
name: Doel, P.
name: Everett, S.
name: Flaugher, B.
name: Fosalba, P.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Gerdes, D. W.
name: Giannantonio, T.
name: Gruen, D.
name: Gruendl, R. A.
name: Gutierrez, G.
name: Hinton, S. R.
name: Hollowood, D. L.
name: Honscheid, K.
name: Huterer, D.
name: James, D. J.
name: Kuehn, K.
name: Lahav, O.
name: Lidman, C.
name: Lima, M.
name: Marshall, J. L.
name: Mena-Fernández, J.
name: Menanteau, F.
name: Miquel, R.
name: Palmese, A.
name: Paz-Chinchón, F.
name: Pieres, A.
name: Malagón, A. A. Plazas
name: Raveri, M.
name: Rodriguez-Monroy, M.
name: Roodman, A.
name: Ross, A. J.
name: Scarpine, V.
name: Sevilla-Noarbe, I.
name: Smith, M.
name: Suchyta, E.
name: Swanson, M. E. C.
name: Tarle, G.
name: Thomas, D.
name: Tucker, D. L.
name: Vincenzi, M.
name: Weaverdyck, N.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The three-dimensional correlation function offers an effective way to summarize the correlation of the large-scale structure even for imaging galaxy surveys. We have applied the projected three-dimensional correlation function, $ξ_{\rm p}$ to measure the Baryonic Acoustic Oscillations (BAO) scale on the first-three years Dark Energy Survey data. The sample consists of about 7 million galaxies in the redshift range $ 0.6 &lt; z_{\rm p } &lt; 1.1 $ over a footprint of $4108 \, \mathrm{deg}^2 $. Our theory modeling includes the impact of realistic true redshift distributions beyond Gaussian photo-$z$ approximation. To increase the signal-to-noise of the measurements, a Gaussian stacking window function is adopted in place of the commonly used top-hat. Using the full sample, $ D_{\rm M}(z_{\rm eff} ) / r_{\rm s} $, the ratio between the comoving angular diameter distance and the sound horizon, is constrained to be $ 19.00 \pm 0.67 $ (top-hat) and $ 19.15 \pm 0.58 $ (Gaussian) at $z_{\rm eff} = 0.835$. The constraint is weaker than the angular correlation $w$ constraint ($18.84 \pm 0.50$) because the BAO signals are heterogeneous across redshift. When a homogeneous BAO-signal sub-sample in the range $ 0.7 &lt; z_{\rm p } &lt; 1.0 $ ($z_{\rm eff} = 0.845$) is considered, $ξ_{\rm p} $ yields $ 19.80 \pm 0.67 $ (top-hat) and $ 19.84 \pm 0.53 $ (Gaussian). The latter is mildly stronger than the $w$ constraint ($19.86 \pm 0.55 $). We find that the $ξ_{\rm p} $ results are more sensitive to photo-$z$ errors than $w$ because $ξ_{\rm p}$ keeps the three-dimensional clustering information causing it to be more prone to photo-$z$ noise. The Gaussian window gives more robust results than the top-hat as the former is designed to suppress the low signal modes. $ξ_{\rm p}$ and the angular statistics such as $w$ have their own pros and cons, and they serve an important crosscheck with each other.
description: 20 pages, 12 figures, minor changes to match published version