학술논문
Dark Energy Survey Year 3 Results: Measurement of the Baryon Acoustic Oscillations with Three-dimensional Clustering
Document Type
Working Paper
Author
Chan, K. C.; Avila, S.; Rosell, A. Carnero; Ferrero, I.; Elvin-Poole, J.; Sanchez, E.; Camacho, H.; Porredon, A.; Crocce, M.; Abbott, T. M. C.; Aguena, M.; Allam, S.; Andrade-Oliveira, F.; Bertin, E.; Bocquet, S.; Brooks, D.; Burke, D. L.; Kind, M. Carrasco; Carretero, J.; Castander, F. J.; Cawthon, R.; Conselice, C.; Costanzi, M.; Pereira, M. E. S.; De Vicente, J.; Desai, S.; Diehl, H. T.; Doel, P.; Everett, S.; Flaugher, B.; Fosalba, P.; García-Bellido, J.; Gaztanaga, E.; Gerdes, D. W.; Giannantonio, T.; Gruen, D.; Gruendl, R. A.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.; Honscheid, K.; Huterer, D.; James, D. J.; Kuehn, K.; Lahav, O.; Lidman, C.; Lima, M.; Marshall, J. L.; Mena-Fernández, J.; Menanteau, F.; Miquel, R.; Palmese, A.; Paz-Chinchón, F.; Pieres, A.; Malagón, A. A. Plazas; Raveri, M.; Rodriguez-Monroy, M.; Roodman, A.; Ross, A. J.; Scarpine, V.; Sevilla-Noarbe, I.; Smith, M.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; Tucker, D. L.; Vincenzi, M.; Weaverdyck, N.
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Subject
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Abstract
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, $\xi_{\rm p}$ 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 < z_{\rm p } < 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 < z_{\rm p } < 1.0 $ ($z_{\rm eff} = 0.845$) is considered, $\xi_{\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 $\xi_{\rm p} $ results are more sensitive to photo-$z$ errors than $w$ because $\xi_{\rm p}$ 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. $\xi_{\rm p}$ and the angular statistics such as $w$ have their own pros and cons, and they serve an important crosscheck with each other.
Comment: 20 pages, 12 figures, minor changes to match published version
Comment: 20 pages, 12 figures, minor changes to match published version