The Dark Energy Survey Year 3 high-redshift sample: Selection, characterization, and analysis of galaxy clustering

(DES Collaboration)

doi:10.1093/mnras/stad2402

The Dark Energy Survey Year 3 high-redshift sample: Selection, characterization, and analysis of galaxy clustering

(DES Collaboration)

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Abstract

The fiducial cosmological analyses of imaging surveys like DES typically probe the Universe at redshifts z < 1. We present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around z ∼0.9, 1.2, and 1.5, which extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions.

Original language	English
Pages (from-to)	3896-3922
Number of pages	27
Journal	Monthly Notices of the Royal Astronomical Society
Volume	525
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stad2402
State	Published - Nov 1 2023

Funding

The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA programme of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). CS acknowledges financial support from Ramón y Cajal project RYC2021-031194-I, funded by MCIN/AEI/ 10.13039/501100011033 and by the ‘European Union NextGenerationEU/PRTR’, and by a Junior Leader fellowship from the ‘la Caixa’ Foundation (ID 100010434), with code LCF/BQ/PI22/11910018. CS and GMB are supported by grants AST-2009210 from the U.S. National Science Foundation, and DE-SC0007901 from the U.S. Department of Energy (DOE). Argonne National Laboratory’s work was supported by the U.S. Department of Energy, Office of High Energy Physics. Argonne, a U.S. Department of Energy Office of Science Laboratory, is operated by UChicago Argonne LLC under contract no. DE-AC02-06CH11357. This research used resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility located at Lawrence Berkeley National Laboratory, operated under Contract No. DE-AC02-05CH11231. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the DES.

Keywords

cosmological parameters
galaxies: high-redshift
large-scale structure of Universe

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10.1093/mnras/stad2402

Cite this

@article{232e0c10027748179fd4a09d79007111,

title = "The Dark Energy Survey Year 3 high-redshift sample: Selection, characterization, and analysis of galaxy clustering",

abstract = "The fiducial cosmological analyses of imaging surveys like DES typically probe the Universe at redshifts z < 1. We present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around z ∼0.9, 1.2, and 1.5, which extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions.",

keywords = "cosmological parameters, galaxies: high-redshift, large-scale structure of Universe",

author = "{(DES Collaboration)} and C. S{\'a}nchez and A. Alarcon and Bernstein, {G. M.} and J. Sanchez and S. Pandey and M. Raveri and J. Prat and N. Weaverdyck and I. Sevilla-Noarbe and C. Chang and E. Baxter and Y. Omori and B. Jain and O. Alves and A. Amon and K. Bechtol and Becker, {M. R.} and J. Blazek and A. Choi and A. Campos and Rosell, {A. Carnero} and Kind, {M. Carrasco} and M. Crocce and D. Cross and J. Derose and Diehl, {H. T.} and S. Dodelson and A. Drlica-Wagner and K. Eckert and Eifler, {T. F.} and J. Elvin-Poole and S. Everett and X. Fang and P. Fosalba and D. Gruen and Gruendl, {R. A.} and I. Harrison and Hartley, {W. G.} and H. Huang and Huff, {E. M.} and N. Kuropatkin and N. Maccrann and J. McCullough and J. Myles and E. Krause and A. Porredon and M. Rodriguez-Monroy and Rykoff, {E. S.} and Secco, {L. F.} and E. Suchyta",

note = "Publisher Copyright: {\textcopyright}m and the Hubble parameter h and 2-3 per cent measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, bσ8. A companion paper (in preparation) will present the cross-correlations of these high-z samples with cosmic microwave background lensing from Planck and South Pole Telescope, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work. ",

year = "2023",

month = nov,

day = "1",

doi = "10.1093/mnras/stad2402",

language = "English",

volume = "525",

pages = "3896--3922",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

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T1 - The Dark Energy Survey Year 3 high-redshift sample

T2 - Selection, characterization, and analysis of galaxy clustering

AU - (DES Collaboration)

AU - Sánchez, C.

AU - Alarcon, A.

AU - Bernstein, G. M.

AU - Sanchez, J.

AU - Pandey, S.

AU - Raveri, M.

AU - Prat, J.

AU - Weaverdyck, N.

AU - Sevilla-Noarbe, I.

AU - Chang, C.

AU - Baxter, E.

AU - Omori, Y.

AU - Jain, B.

AU - Alves, O.

AU - Amon, A.

AU - Bechtol, K.

AU - Becker, M. R.

AU - Blazek, J.

AU - Choi, A.

AU - Campos, A.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Crocce, M.

AU - Cross, D.

AU - Derose, J.

AU - Diehl, H. T.

AU - Dodelson, S.

AU - Drlica-Wagner, A.

AU - Eckert, K.

AU - Eifler, T. F.

AU - Elvin-Poole, J.

AU - Everett, S.

AU - Fang, X.

AU - Fosalba, P.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Harrison, I.

AU - Hartley, W. G.

AU - Huang, H.

AU - Huff, E. M.

AU - Kuropatkin, N.

AU - Maccrann, N.

AU - McCullough, J.

AU - Myles, J.

AU - Krause, E.

AU - Porredon, A.

AU - Rodriguez-Monroy, M.

AU - Rykoff, E. S.

AU - Secco, L. F.

AU - Suchyta, E.

N1 - Publisher Copyright: ©m and the Hubble parameter h and 2-3 per cent measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, bσ8. A companion paper (in preparation) will present the cross-correlations of these high-z samples with cosmic microwave background lensing from Planck and South Pole Telescope, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work.

PY - 2023/11/1

Y1 - 2023/11/1

N2 - The fiducial cosmological analyses of imaging surveys like DES typically probe the Universe at redshifts z < 1. We present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around z ∼0.9, 1.2, and 1.5, which extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions.

AB - The fiducial cosmological analyses of imaging surveys like DES typically probe the Universe at redshifts z < 1. We present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around z ∼0.9, 1.2, and 1.5, which extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions.

KW - cosmological parameters

KW - galaxies: high-redshift

KW - large-scale structure of Universe

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DO - 10.1093/mnras/stad2402

M3 - Article

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VL - 525

SP - 3896

EP - 3922

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

The Dark Energy Survey Year 3 high-redshift sample: Selection, characterization, and analysis of galaxy clustering

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Keywords

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