Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis

I. Ferrero; M. Crocce; I. Tutusaus; A. Porredon; L. Blot; P. Fosalba; A. Carnero Rosell; S. Avila; A. Izard; J. Elvin-Poole; K. C. Chan; H. Camacho; R. Rosenfeld; E. Sanchez; P. Tallada-Crespí; J. Carretero; I. Sevilla-Noarbe; E. Gaztanaga; F. Andrade-Oliveira; J. De Vicente; J. Mena-Fernández; A. J. Ross; D. Sanchez Cid; A. Ferté; A. Brandao-Souza; X. Fang; E. Krause; D. Gomes; M. Aguena; S. Allam; J. Annis; E. Bertin; D. Brooks; M. Carrasco Kind; F. J. Castander; R. Cawthon; A. Choi; C. Conselice; M. Costanzi; L. N. Da Costa; M. E.S. Pereira; H. T. Diehl; P. Doel; A. Drlica-Wagner; S. Everett; A. E. Evrard; B. Flaugher; J. Frieman; J. García-Bellido; D. W. Gerdes; D. Gruen; R. A. Gruendl; J. Gschwend; G. Gutierrez; S. R. Hinton; D. L. Hollowood; K. Honscheid; B. Hoyle; D. Huterer; D. J. James; K. Kuehn; M. Lima; M. A.G. Maia; J. L. Marshall; F. Menanteau; R. Miquel; R. Morgan; J. Muir; R. L.C. Ogando; A. Palmese; F. Paz-Chinchón; W. J. Percival; A. A. Plazas Malagón; M. Rodriguez-Monroy; V. Scarpine; M. Schubnell; S. Serrano; M. Smith; M. Soares-Santos; E. Suchyta; M. E.C. Swanson; G. Tarle; D. Thomas; C. To; D. L. Tucker; T. N. Varga

doi:10.1051/0004-6361/202141744

Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis

I. Ferrero, M. Crocce, I. Tutusaus, A. Porredon, L. Blot, P. Fosalba, A. Carnero Rosell, S. Avila, A. Izard, J. Elvin-Poole, K. C. Chan, H. Camacho, R. Rosenfeld, E. Sanchez, P. Tallada-Crespí, J. Carretero, I. Sevilla-Noarbe, E. Gaztanaga, F. Andrade-Oliveira, J. De VicenteJ. Mena-Fernández, A. J. Ross, D. Sanchez Cid, A. Ferté, A. Brandao-Souza, X. Fang, E. Krause, D. Gomes, M. Aguena, S. Allam, J. Annis, E. Bertin, D. Brooks, M. Carrasco Kind, F. J. Castander, R. Cawthon, A. Choi, C. Conselice, M. Costanzi, L. N. Da Costa, M. E.S. Pereira, H. T. Diehl, P. Doel, A. Drlica-Wagner, S. Everett, A. E. Evrard, B. Flaugher, J. Frieman, J. García-Bellido, D. W. Gerdes, D. Gruen, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, B. Hoyle, D. Huterer, D. J. James, K. Kuehn, M. Lima, M. A.G. Maia, J. L. Marshall, F. Menanteau, R. Miquel, R. Morgan, J. Muir, R. L.C. Ogando, A. Palmese, F. Paz-Chinchón, W. J. Percival, A. A. Plazas Malagón, M. Rodriguez-Monroy, V. Scarpine, M. Schubnell, S. Serrano, M. Smith, M. Soares-Santos, E. Suchyta, M. E.C. Swanson, G. Tarle, D. Thomas, C. To, D. L. Tucker, T. N. Varga

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Abstract

The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.

Original language	English
Article number	A106
Journal	Astronomy and Astrophysics
Volume	656
DOIs	https://doi.org/10.1051/0004-6361/202141744
State	Published - Dec 1 2021

Funding

Acknowledgements. 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 Proje-tos, 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 Forschungsge-meinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investiga-ciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NSF’s NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1 536171. 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 program 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). 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. 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. The simulation production and storage, as well as the processing and analysis tools have been developed, implemented and operated in collaboration with the Port d’Informació Científica (PIC). SA was supported by the MICUES project, funded by the EU’s H2020 MSCA grant agreement no. 713366 (InterTalentum UAM). ACR acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under grant AYA2017-84061-P, co-financed by FEDER (European Regional Development Funds) and by the Spanish Space Research Program “Participation in the NISP instrument and preparation for the science of EUCLID" (ESP2017-84272-C2-1-R). This project has received funding from the European Union’s Horizon 2020 Research and Innovation Programme under the Marie Skłodowska-Curie grant agreement No. 734374.

Funders	Funder number
Brazilian Instituto Nacional de Ciência e Tecnologia
Collaborating Institutions in the Dark Energy Survey	2012B-0001
EU’s H2020 MSCA	713366
Fermi Research Alliance, LLC	DE-AC02-07CH11359
INCT
MICIU	AYA2017-84061-P
Marie Skłodowska-Curie	734374
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign
Science and Technology Facilities Council of the United Kingdom
Spanish Space Research Program
National Science Foundation	AST-1138766, AST-1 536171
National Science Foundation
U.S. Department of Energy
Office of Science
High Energy Physics
Ohio State University
University of Chicago
Horizon 2020 Framework Programme
Seventh Framework Programme
Higher Education Funding Council for England
Ministerio de Ciencia, Innovación y Universidades
European Commission
European Research Council	240672, 306478, 291329
European Research Council
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya
Ministério da Ciência, Tecnologia e Inovação
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Conselho Nacional de Desenvolvimento Científico e Tecnológico
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministerio de Ciencia e Innovación	SEV-2016-0588, SEV-2016-0597, MDM-2015-0509, PGC2018-094773, PGC2018-102021, ESP2017-89838
Ministerio de Ciencia e Innovación
Ministry of Education and Science of Ukraine
European Regional Development Fund
preparation for the science of EUCLID	ESP2017-84272-C2-1-R

Keywords

Catalogs
Galaxies: distances and redshifts
Galaxy: halo
Large-scale structure of Universe
Methods: numerical

Access to Document

10.1051/0004-6361/202141744

Cite this

Ferrero, I., Crocce, M., Tutusaus, I., Porredon, A., Blot, L., Fosalba, P., Carnero Rosell, A., Avila, S., Izard, A., Elvin-Poole, J., Chan, K. C., Camacho, H., Rosenfeld, R., Sanchez, E., Tallada-Crespí, P., Carretero, J., Sevilla-Noarbe, I., Gaztanaga, E., Andrade-Oliveira, F., ... Varga, T. N. (2021). Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis. Astronomy and Astrophysics, 656, Article A106. https://doi.org/10.1051/0004-6361/202141744

@article{f20e83813d514ffca9787e291e863097,

title = "Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis",

abstract = "The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.",

keywords = "Catalogs, Galaxies: distances and redshifts, Galaxy: halo, Large-scale structure of Universe, Methods: numerical",

author = "I. Ferrero and M. Crocce and I. Tutusaus and A. Porredon and L. Blot and P. Fosalba and {Carnero Rosell}, A. and S. Avila and A. Izard and J. Elvin-Poole and Chan, {K. C.} and H. Camacho and R. Rosenfeld and E. Sanchez and P. Tallada-Cresp{\'i} and J. Carretero and I. Sevilla-Noarbe and E. Gaztanaga and F. Andrade-Oliveira and {De Vicente}, J. and J. Mena-Fern{\'a}ndez and Ross, {A. J.} and {Sanchez Cid}, D. and A. Fert{\'e} and A. Brandao-Souza and X. Fang and E. Krause and D. Gomes and M. Aguena and S. Allam and J. Annis and E. Bertin and D. Brooks and {Carrasco Kind}, M. and Castander, {F. J.} and R. Cawthon and A. Choi and C. Conselice and M. Costanzi and {Da Costa}, {L. N.} and Pereira, {M. E.S.} and Diehl, {H. T.} and P. Doel and A. Drlica-Wagner and S. Everett and Evrard, {A. E.} and B. Flaugher and J. Frieman and J. Garc{\'i}a-Bellido and Gerdes, {D. W.} and D. Gruen and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and B. Hoyle and D. Huterer and James, {D. J.} and K. Kuehn and M. Lima and Maia, {M. A.G.} and Marshall, {J. L.} and F. Menanteau and R. Miquel and R. Morgan and J. Muir and Ogando, {R. L.C.} and A. Palmese and F. Paz-Chinch{\'o}n and Percival, {W. J.} and {Plazas Malag{\'o}n}, {A. A.} and M. Rodriguez-Monroy and V. Scarpine and M. Schubnell and S. Serrano and M. Smith and M. Soares-Santos and E. Suchyta and Swanson, {M. E.C.} and G. Tarle and D. Thomas and C. To and Tucker, {D. L.} and Varga, {T. N.}",

note = "Publisher Copyright: {\textcopyright} ESO 2021.",

year = "2021",

month = dec,

day = "1",

doi = "10.1051/0004-6361/202141744",

language = "English",

volume = "656",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

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Ferrero, I, Crocce, M, Tutusaus, I, Porredon, A, Blot, L, Fosalba, P, Carnero Rosell, A, Avila, S, Izard, A, Elvin-Poole, J, Chan, KC, Camacho, H, Rosenfeld, R, Sanchez, E, Tallada-Crespí, P, Carretero, J, Sevilla-Noarbe, I, Gaztanaga, E, Andrade-Oliveira, F, De Vicente, J, Mena-Fernández, J, Ross, AJ, Sanchez Cid, D, Ferté, A, Brandao-Souza, A, Fang, X, Krause, E, Gomes, D, Aguena, M, Allam, S, Annis, J, Bertin, E, Brooks, D, Carrasco Kind, M, Castander, FJ, Cawthon, R, Choi, A, Conselice, C, Costanzi, M, Da Costa, LN, Pereira, MES, Diehl, HT, Doel, P, Drlica-Wagner, A, Everett, S, Evrard, AE, Flaugher, B, Frieman, J, García-Bellido, J, Gerdes, DW, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, Hoyle, B, Huterer, D, James, DJ, Kuehn, K, Lima, M, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Morgan, R, Muir, J, Ogando, RLC, Palmese, A, Paz-Chinchón, F, Percival, WJ, Plazas Malagón, AA, Rodriguez-Monroy, M, Scarpine, V, Schubnell, M, Serrano, S, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, To, C, Tucker, DL & Varga, TN 2021, 'Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis', Astronomy and Astrophysics, vol. 656, A106. https://doi.org/10.1051/0004-6361/202141744

TY - JOUR

T1 - Dark Energy Survey Year 3 Results

T2 - Galaxy mock catalogs for BAO analysis

AU - Ferrero, I.

AU - Crocce, M.

AU - Tutusaus, I.

AU - Porredon, A.

AU - Blot, L.

AU - Fosalba, P.

AU - Carnero Rosell, A.

AU - Avila, S.

AU - Izard, A.

AU - Elvin-Poole, J.

AU - Chan, K. C.

AU - Camacho, H.

AU - Rosenfeld, R.

AU - Sanchez, E.

AU - Tallada-Crespí, P.

AU - Carretero, J.

AU - Sevilla-Noarbe, I.

AU - Gaztanaga, E.

AU - Andrade-Oliveira, F.

AU - De Vicente, J.

AU - Mena-Fernández, J.

AU - Ross, A. J.

AU - Sanchez Cid, D.

AU - Ferté, A.

AU - Brandao-Souza, A.

AU - Fang, X.

AU - Krause, E.

AU - Gomes, D.

AU - Aguena, M.

AU - Allam, S.

AU - Annis, J.

AU - Bertin, E.

AU - Brooks, D.

AU - Carrasco Kind, M.

AU - Castander, F. J.

AU - Cawthon, R.

AU - Choi, A.

AU - Conselice, C.

AU - Costanzi, M.

AU - Da Costa, L. N.

AU - Pereira, M. E.S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Drlica-Wagner, A.

AU - Everett, S.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gerdes, D. W.

AU - Gruen, D.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - Hoyle, B.

AU - Huterer, D.

AU - James, D. J.

AU - Kuehn, K.

AU - Lima, M.

AU - Maia, M. A.G.

AU - Marshall, J. L.

AU - Menanteau, F.

AU - Miquel, R.

AU - Morgan, R.

AU - Muir, J.

AU - Ogando, R. L.C.

AU - Palmese, A.

AU - Paz-Chinchón, F.

AU - Percival, W. J.

AU - Plazas Malagón, A. A.

AU - Rodriguez-Monroy, M.

AU - Scarpine, V.

AU - Schubnell, M.

AU - Serrano, S.

AU - Smith, M.

AU - Soares-Santos, M.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Tarle, G.

AU - Thomas, D.

AU - To, C.

AU - Tucker, D. L.

AU - Varga, T. N.

PY - 2021/12/1

Y1 - 2021/12/1

N2 - The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.

AB - The calibration and validation of scientific analysis in simulations is a fundamental tool to ensure unbiased and robust results in observational cosmology. In particular, mock galaxy catalogs are a crucial resource to achieve these goals in the measurement of baryon acoustic oscillation (BAO) in the clustering of galaxies. Here we present a set of 1952 galaxy mock catalogs designed to mimic the Dark Energy Survey Year 3 BAO sample over its full photometric redshift range 0:6 < zphoto < 1:1. The mocks are based upon 488 ICE-COLA fast N-body simulations of full-sky light cones and were created by populating halos with galaxies, using a hybrid halo occupation distribution halo abundance matching model. This model has ten free parameters, which were determined, for the first time, using an automatic likelihood minimization procedure.We also introduced a novel technique to assign photometric redshift for simulated galaxies, following a two-dimensional probability distribution with VIMOS Public Extragalactic Redshift Survey data. The calibration was designed to match the observed abundance of galaxies as a function of photometric redshift, the distribution of photometric redshift errors, and the clustering amplitude on scales smaller than those used for BAO measurements. An exhaustive analysis was done to ensure that the mocks reproduce the input properties. Finally, mocks were tested by comparing the angular correlation function w(θ), angular power spectrum ζp(rΓ) and projected clustering p(r?) to theoretical predictions and data. The impact of volume replication in the estimate of the covariance is also investigated. The success in accurately reproducing the photometric redshift uncertainties and the galaxy clustering as a function of redshift render this mock creation pipeline as a benchmark for future analyses of photometric galaxy surveys.

KW - Catalogs

KW - Galaxies: distances and redshifts

KW - Galaxy: halo

KW - Large-scale structure of Universe

KW - Methods: numerical

UR - http://www.scopus.com/inward/record.url?scp=85121207003&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202141744

DO - 10.1051/0004-6361/202141744

M3 - Article

AN - SCOPUS:85121207003

SN - 0004-6361

VL - 656

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A106

ER -

Dark Energy Survey Year 3 Results: Galaxy mock catalogs for BAO analysis

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