Dark Energy Survey Year 3 results: Measurement of the baryon acoustic oscillations with three-dimensional clustering

Chan, K. C.; Avila, S.; Carnero Rosell, A.; 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.; Garcia-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-Fernandez, J.; Menanteau, F.; Miquel, R.; Palmese, A.; Paz-Chinchon, F.; Pieres, A.; Malagon, 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. und Weaverdyck, N. (2022): Dark Energy Survey Year 3 results: Measurement of the baryon acoustic oscillations with three-dimensional clustering. In: Physical Review D, Bd. 106, Nr. 12, 123502

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 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 < zp < 1.1 over a footprint of 4108 deg2. Our theory modeling includes the impact of realistic true redshift distributions beyond Gaussian photo -z approximation. xi p is obtained by projecting the three-dimensional correlation to the transverse direction. To increase the signal-to-noise of the measurements, we have considered a Gaussian stacking window function in place of the commonly used top-hat. xi p is sensitive to DM(zeff)/rs, the ratio between the comoving angular diameter distance and the sound horizon. Using the full sample, DM(zeff)/rs is constrained to be 19.00 +/- 0.67 (top-hat) and 19.15 +/- 0.58 (Gaussian) at zeff = 0.835. The constraint is weaker than the angular correlation w constraint (18.84 +/- 0.50), and we trace this to the fact that the BAO signals are heterogeneous across redshift. While ep responds to the heterogeneous signals by enlarging the error bar, w can still give a tight bound on DM=rs in this case. When a homogeneous BAO-signal subsample in the range 0.7 < zp < 1.0 (zeff = 0.845) is considered, ep yields 19.80 +/- 0.67 (top-hat) and 19.84 +/- 0.53 (Gaussian). The latter is mildly stronger than the w constraint (19.86 +/- 0.55). We find that the ep results are more sensitive to photo-z errors than w because ep 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. ep and the angular statistics such as w have their own pros and cons, and they serve an important crosscheck with each other.

• Dokumententyp: Zeitschriftenartikel
• Fakultät: Physik
• Themengebiete: 500 Naturwissenschaften und Mathematik > 530 Physik
• ISSN: 2470-0010
• Sprache: Englisch