Dark Energy Survey: Galaxy sample for the baryonic acoustic oscillation measurement from the final dataset

In this paper, we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y6 data. The definition is based on a color and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.6, while ensuring a high-quality photo-$z$ determination. The optimization is performed using a Fisher forecast algorithm, finding the optimal $i$-magnitude cut to be given by $i<19.64+2.894{z}_{\mathrm{ph}}$. For the optimal sample, we forecast an increase in precision in the BAO measurement of $\ensuremath{\sim}25%$ with respect to the Y3 analysis. Our BAO sample has a total of 15,937,556 galaxies in the redshift range $0.6<{z}_{\mathrm{ph}}<1.2$, and its angular mask covers $4,273.42\text{ }\text{ }{\mathrm{deg}}^{2}$ to a depth of $i=22.5$. We validate its redshift distributions with three different methods: directional neighborhood fitting algorithm (DNF), which is our primary photo-$z$ estimation; direct calibration with spectroscopic redshifts from VIPERS, which is a spectroscopic galaxy sample that overlaps with our BAO sample and is complete within our selection cuts; and clustering redshift using SDSS galaxies. The fiducial redshift distribution is a combination of these three techniques performed by modifying the mean and width of the DNF distributions to match those of VIPERS and clustering redshift. In this paper, we also describe the methodology used to mitigate the effect of observational systematics, which is analogous to the one used in the Y3 analysis. This paper is one of the two dedicated to the analysis of the BAO signal in DES Y6. In its companion paper, we present the angular diameter distance constraints obtained through the fitting to the BAO scale.

Authors

Institutions

Publication Details

Journal
Physical review. D/Physical review. D.
Published
2024-09-05
DOI
https://doi.org/10.1103/physrevd.110.063514
Citations
8
Primary Topic
Cosmology and Gravitation Theories
Type
article
Field-Weighted Citation Impact
2.65

Funders

Controls
|||
ALL TIME
JAN
FEB
MAR
APR
MAY
JUN
JUL
AUG
SEP
OCT
article

Dark Energy Survey: Galaxy sample for the baryonic acoustic oscillation measurement from the final dataset

A. Roodman, Will J. Percival, S. Everett, I. Ferrero et al.
8 citations
Physical review. D/Physical review. D.
Cosmology and Gravitation Theories
2.65
article

Dark Energy Survey: Galaxy sample for the baryonic acoustic oscillation measurement from the final dataset

A. Roodman, Will J. Percival, S. Everett, I. Ferrero, J. Myles, H. Camacho, J. García-Bellido, S. Bocquet, L. N. da Costa, M. Adamów, B. Yanny, N. Deiosso, A Drlica-Wagner, Francisco Javier Castander, J. L. Marshall, Santiago Avila, A. A. Plazas, Gregory Tarlé, D. Sanchez Cid, A. Amon, A. Porredon, O. Alves, P. Wiseman, G. Giannini, S. R. Hinton, A. R. Walker, G. Gutierrez, A. Palmese, E. Sheldon, J. Carretero, C. Tucker, Kwan Chuen Chan, Scott Dodelson, T. M. C. Abbott, J. Elvin-Poole, Eusebio Sanchez, J. Weller, J. Mena-Fernández, Ashley J. Ross, A. Carnero Rosell, J. De Vicente, ENRIQUE GAZTAÑAGA, K. Honscheid, M. Rodríguez-Monroy, L. Toribio San Cipriano, K. Kuehn, E. S. Rykoff, C. To, R. A. Gruendl, J. García-Bellido, F. Menanteau, J. Blazek, R. L. C. Ogando, I. Sevilla-Noarbe, M. E. S. Pereira, Christopher E. Lidman, David H. Brooks, H. T. Diehl, F. Andrade-Oliveira, Dragan Huterer A, A. Pieres, C. Doux, R. Cawthon, M. Aguena, S Lee, T. M. Davis, S. Samuroff, M. Yamamoto, H. Lin, B. X. Santiago, R. Miquel, M. Smith, S. Allam, K. Bechtol, J. Annis, M. Soares-Santos, M. Crocce, D. Thomas, O. Lahav, J. Frieman, W. G. Hartley, M. Schubnell, M. E. C. Swanson, S. Desai, C. Conselice, N. Weaverdyck, D. Bacon, R G Rosenfeld
article en
8 citations

Abstract

In this paper, we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y6 data. The definition is based on a color and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.6, while ensuring a high-quality photo-$z$ determination. The optimization is performed using a Fisher forecast algorithm, finding the optimal $i$-magnitude cut to be given by $i<19.64+2.894{z}_{\mathrm{ph}}$. For the optimal sample, we forecast an increase in precision in the BAO measurement of $\ensuremath{\sim}25%$ with respect to the Y3 analysis. Our BAO sample has a total of 15,937,556 galaxies in the redshift range $0.6<{z}_{\mathrm{ph}}<1.2$, and its angular mask covers $4,273.42\text{ }\text{ }{\mathrm{deg}}^{2}$ to a depth of $i=22.5$. We validate its redshift distributions with three different methods: directional neighborhood fitting algorithm (DNF), which is our primary photo-$z$ estimation; direct calibration with spectroscopic redshifts from VIPERS, which is a spectroscopic galaxy sample that overlaps with our BAO sample and is complete within our selection cuts; and clustering redshift using SDSS galaxies. The fiducial redshift distribution is a combination of these three techniques performed by modifying the mean and width of the DNF distributions to match those of VIPERS and clustering redshift. In this paper, we also describe the methodology used to mitigate the effect of observational systematics, which is analogous to the one used in the Y3 analysis. This paper is one of the two dedicated to the analysis of the BAO signal in DES Y6. In its companion paper, we present the angular diameter distance constraints obtained through the fitting to the BAO scale.

Physical review. D/Physical review. D.Vol. 110(6)
University of Geneva (CH), Australian National University (AU), Institució Catalana de Recerca i Estudis Avançats (ES), California Institute of Technology (US), Oak Ridge National Laboratory (US), Centre National de la Recherche Scientifique (FR), Fermi National Accelerator Laboratory (US), Institute of Space Sciences (ES), University of Wisconsin–Madison (US), University of Nottingham (GB), Lawrence Berkeley National Laboratory (US), University of Waterloo (CA), University of Illinois Urbana-Champaign (US), Sun Yat-sen University (CN), Universidad de La Laguna (ES), Universität Hamburg (DE), The University of Queensland (AU), Duke University (US), Perimeter Institute (CA), Brookhaven National Laboratory (US), Princeton University (US), University of Cambridge (GB), Université Paris-Saclay (FR), University of Michigan (US), Lowell Observatory (US), Mitchell Institute (US), SLAC National Accelerator Laboratory (US), University of Manchester (GB), California University of Pennsylvania (US), University of Chicago (US), Max Planck Institute for Extraterrestrial Physics (DE), Institut d'Estudis Espacials de Catalunya (ES), Institute of Particle Physics (CA), Instituto de Física La Plata (AR), Centre for Theoretical Physics and Astrophysics (UZ), National Observatory (BR), Instituto de Astrofísica de Canarias (ES), Barcelona Institute of Science and Technology (ES), Laboratoire de Physique Subatomique et de Cosmologie (FR), NSF NOIRLab (US), Laboratório Interinstitucional de e-Astronomia (BR), Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (ES), University of Southampton (GB), Institute of Science and Technology, Institut des langues et cultures d'Europe, Amérique, Afrique, Asie et Australie (FR), University College London (GB), The Ohio State University (US), William Jewell College (US), University of Portsmouth (GB), Universidad Autónoma de Madrid (ES), Indian Institute of Technology Hyderabad (IN), Carnegie Mellon University (US), Ludwig-Maximilians-Universität München (DE), Universidad del Noreste (MX), Universidade Estadual Paulista (Unesp) (BR), Université Grenoble Alpes (FR), Ruhr University Bochum (DE), Texas A&M University (US), Stanford University (US), Macquarie University (AU)
National Science Foundation, U.S. Department of Energy, Stanford University, University of California, Santa Cruz, University of Pennsylvania, Ohio State University, University of Chicago, University of Michigan, Texas A and M University, University of Portsmouth, Higher Education Funding Council for England, Ministarstvo znanosti i obrazovanja, University of Cambridge, University College London, European Commission, University of Nottingham, University of Sussex, University of Edinburgh, Deutsche Forschungsgemeinschaft, Fundação de Amparo à Pesquisa do Estado de São Paulo, National Natural Science Foundation of China, Generalitat de Catalunya, Ministério da Ciência, Tecnologia e Inovação, 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, Ludwig-Maximilians-Universität München, Instituto Nacional de Ciência e Tecnologia: Física Nuclear e Aplicações, Institut de Física d'Altes Energies, University of Illinois at Urbana-Champaign, Office of Science, Kavli Institute for Cosmological Physics, University of Chicago, HORIZON EUROPE Framework Programme, Science and Technology Facilities Council, European Research Council, European Regional Development Fund, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, High Energy Physics, Argonne National Laboratory, Fermilab, Lawrence Berkeley National Laboratory, H2020 Marie Skłodowska-Curie Actions, SLAC National Accelerator Laboratory
Affordable and clean energy
Openalex Percentile: Top 11%
Cosmology and Gravitation Theories
2.65
DOIOpen Access PDFOpenAlex
AI Navigator

Ask Laika to Summarize, Analyze, and Connect papers live on the map.

Summarize Papers & Methodologies

Extract key findings, datasets, and comparative methods across publications.

Benchmark Rankings & Visual Analytics

Rank top research institutions, authors, funders, topics, and journals by Field-Weighted Citation Impact (FWCI) and paper volume with instant charts.

Connect Distant Disciplines

Bridge topological clusters on the map to find hidden collaborative intersections.