Journal
PHYSICAL REVIEW D
Volume 106, Issue 12, Pages -Publisher
AMER PHYSICAL SOC
DOI: 10.1103/PhysRevD.106.123502
Keywords
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Funding
- National Science Foundation of China [11873102, 12273121]
- China Manned Space Project [CMS-CSST-2021-B01]
- Science and Technology Program of Guangzhou, China [202002030360]
- Spanish Agencia Estatal de Investigacion through the grant IFT Centro de Excelencia Severo Ochoa [CEX2020-001007-S, EU-HORIZON-2020-776247]
- Atraccion de Talento Program - Comunidad de Madrid in Spain [2019-T1/TIC-12702]
- U.S. Department of Energy
- U.S. National Science Foundation
- Ministry of Science and Education of Spain
- Science and Technology Facilities Council of the United Kingdom
- Higher Education Funding Council for England
- National Center for Supercomputing Applications at the University of Illinois at UrbanaChampaign
- Center for Cosmology and Astro-Particle Physics at the Ohio State University
- Mitchell Institute for Fundamental Physics and Astronomy at Texas AM University
- Financiadora de Estudos e Projetos
- Fundacao Carlos Chagas Filho de Amparo a Pesquisa do Estado do Rio de Janeiro
- Conselho Nacional de Desenvolvimento Cientifico e Tecnologico
- Deutsche Forschungsgemeinschaft
- Collaborating Institutions in the Dark Energy Survey
- University of California at Santa Cruz
- University of Cambridge
- Centro de Investigaciones Energeticas
- Medioambientales y Tecnologicas-Madrid
- University of Chicago
- University College London
- DES-Brazil Consortium
- University of Edinburgh
- Eidgenossische Technische Hochschule (ETH) Zurich
- Fermi National Accelerator Laboratory
- University of Illinois at Urbana-Champaign
- Institut de Ciencies de l'Espai (IEEC/CSIC)
- Institut de Fisica d'Altes Energies
- Lawrence Berkeley National Laboratory
- Ludwig-Maximilians Universitat Munchen and the associated Excellence Cluster Universe
- University of Michigan
- NSF's NOIRLab
- University of Nottingham
- Ohio State University
- University of Pennsylvania
- University of Portsmouth
- Stanford University, the University of Sussex
- Texas AM University
- OzDES Membership Consortium
- National Science Foundation [AST-1138766, AST-1536171]
- MICINN [ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, MDM-2015-0509]
- European Union
- CERCA program of the Generalitat de Catalunya
- European Research Council under the European Union [FP7/2007-2013]
- ERC Grant [240672, 291329, 306478]
- Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq) [465376/2014-2]
- Fermi Research Alliance
- LLC [DE-AC02-07CH11359]
- U.S. Department of Energy, Office of Science, Office of High Energy Physics
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The study utilizes the projected three-dimensional correlation function to measure the correlation of large-scale structure and explores the constraints on the baryonic acoustic oscillations (BAO) scale. By considering the realistic redshift distributions and using a Gaussian stacking window function, the research obtains constraints on DM(zeff)/rs.
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.
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