{"paper":{"title":"DESI 2024 III: Baryon Acoustic Oscillations from Galaxies and Quasars","license":"http://creativecommons.org/licenses/by/4.0/","headline":"DESI measures baryon acoustic oscillations to 0.52% combined precision across six redshift bins using 5.7 million galaxies and quasars.","cross_cats":[],"primary_cat":"astro-ph.CO","authors_text":"A. Anand, A. Aviles, A. Bault, A. Brodzeller, A. Carnero Rosell, A. Cuceu, A. de la Macorra, A. de Mattia, A. Dey, A. D. Myers, A. Elliott, A. Font-Ribera, A. J. Ross, A. Kremin, A. Krolewski, A. Leauthaud, A. Meisner, A. Mu\\~noz-Guti\\'errez, A. P\\'erez-Fern\\'andez, A. Porredon, A. Raichoor, A. Rocher, A. Rosado-Marin, A. Slosar, A. Smith, A. X. Gonzalez-Morales, B. A. Weaver, B. Dey, B. Flaugher, B. Hadzhiyska, B. Wang, C. Baltay, C. Blake, C. Garcia-Quintero, C. Gordon, C. Hahn, C. Howlett, C. Magneville, C. Poppett, C. Ram\\'irez-P\\'erez, C. Rockosi, C. Saulder, C. Y\\`eche, C. Zhao, D. Bianchi, D. Brooks, DESI Collaboration: A. G. Adame, D. Forero-S\\'anchez, D. Green, D. Gruen, D. Huterer, D. H. Weinberg, D. J. Eisenstein, D. Kirkby, D. Lang, D. M. Alexander, D. Margala, D. Rabinowitz, D. Schlegel, D. Sprayberry, D. Valcin, E. Armengaud, E. A. Zaborowski, E. Buckley-Geer, E. Burtin, E. Chaussidon, E. F. Schlafly, E. Gazta\\~naga, E. Linder, E. Mueller, E. Paillas, E. Sanchez, F. Beutler, F. Prada, F. Valdes, G. Gutierrez, G. Niz, G. Rossi, G. Tarl\\'e, H. Awan, H. E. Noriega, H. Gil-Mar\\'in, H. K. Herrera-Alcantar, H. Seo, H. Zhang, H. Zou, I. P\\'erez-R\\`afols, J. Aguilar, J. A. Newman, J. Behera, J. Chaves-Montero, J. Edelstein, J. E. Forero-Romero, J. Ereza, J. Guy, J. Lasker, J. L. Cervantes-Cota, J. Mena-Fern\\'andez, J.M. Le Goff, J. Moon, J. Moustakas, J. Nie, J. Pan, J. Rich, J. Silber, J. Swanson, J. Yu, K. Dawson, K. Fanning, K. Honscheid, K. Lodha, L. Le Guillou, L. Medina-Varela, L. Napolitano, L. Samushia, L. Verde, M. Alvarez, M. E. Levi, M. Ishak, M. Landriau, M. Manera, M. Maus, M. M. S Hanif, M. Pieri, M. Pinon, M. Rashkovetskyi, M. Rezaie, M. Schubnell, M. S. Wang, M. Vargas-Maga\\~na, M. Walther, M. White, N.A. Roe, N. Deiosso, N. Findlay, N. G. Kara\\c{c}ayl{\\i}, N. M. Nguyen, N. Mudur, N. Padmanabhan, N. Palanque-Delabrouille, N. Weaverdyck, O. Alves, P. Doel, P. Fagrelius, P. Martini, P. McDonald, P. Zarrouk, R. Blum, R. Calderon, R. Canning, R. Cereskaite, R. Gsponer, R. H. Wechsler, R. Kehoe, R. Miquel, R. Neveux, R. Ruggeri, R. Sharples, R. Vaisakh, R. Zhao, R. Zhou, S. Ahlen, S. Alam, S. Avila, S. Bailey, S. BenZvi, S. Brieden, S. Chabanier, S. Chen, S. Cole, S. Eftekharzadeh, S. Ferraro, S. Gontcho A Gontcho, S. Juneau, S. Kent, S. Moore, S. Nadathur, S. Penmetsa, S. Ramirez-Solano, S. Trusov, S. Yuan, T. Claybaugh, T. M. Davis, T. S. Li, T. Tan, T.-W. Lan, U. Andrade, V. Gonzalez-Perez, V. Ir\\v{s}i\\v{c}, V. Ruhlmann-Kleider, W. J. Percival, X. Chen, Y. Lai, Y. Yu, Z. Ding","submitted_at":"2024-04-03T18:41:49Z","abstract_excerpt":"We present the DESI 2024 galaxy and quasar baryon acoustic oscillations (BAO) measurements using over 5.7 million unique galaxy and quasar redshifts in the range 0.1<z<2.1. Divided by tracer type, we utilize 300,017 galaxies from the magnitude-limited Bright Galaxy Survey with 0.1<z<0.4, 2,138,600 Luminous Red Galaxies with 0.4<z<1.1, 2,432,022 Emission Line Galaxies with 0.8<z<1.6, and 856,652 quasars with 0.8<z<2.1, over a ~7,500 square degree footprint. The analysis was blinded at the catalog-level to avoid confirmation bias. All fiducial choices of the BAO fitting and reconstruction method"},"claims":{"count":4,"items":[{"kind":"strongest_claim","text":"With the total effective survey volume of ~18 Gpc³, the combined precision of the BAO measurements across the six different redshift bins is ~0.52%, marking a 1.2-fold improvement over the previous state-of-the-art results using only first-year data. We detect the BAO in all of these six redshift bins.","source":"verdict.strongest_claim","status":"machine_extracted","claim_id":"C1","attestation":"unclaimed"},{"kind":"weakest_assumption","text":"All fiducial choices of the BAO fitting and reconstruction methodology, as well as the size of the systematic errors, were determined on the basis of the tests with mock catalogs and the blinded data catalogs; this assumes the mocks faithfully reproduce all relevant observational systematics present in the real data.","source":"verdict.weakest_assumption","status":"machine_extracted","claim_id":"C2","attestation":"unclaimed"},{"kind":"one_line_summary","text":"DESI measures BAO scales in six redshift bins with 0.52% combined precision using 5.7 million objects, detecting the signal at up to 9.1 sigma and finding larger scales than Planck LCDM at z<0.8.","source":"verdict.one_line_summary","status":"machine_extracted","claim_id":"C3","attestation":"unclaimed"},{"kind":"headline","text":"DESI measures baryon acoustic oscillations to 0.52% combined precision across six redshift bins using 5.7 million galaxies and quasars.","source":"verdict.pith_extraction.headline","status":"machine_extracted","claim_id":"C4","attestation":"unclaimed"}],"snapshot_sha256":"06b2b86cfaa19509ef9b6ef3247862ac5465d3c10772bd58c6313711255fd7bb"},"source":{"id":"2404.03000","kind":"arxiv","version":1},"verdict":{"id":"729a2b0c-6419-48e2-878f-1328e9965a61","model_set":{"reader":"grok-4.3"},"created_at":"2026-05-17T06:29:49.122187Z","strongest_claim":"With the total effective survey volume of ~18 Gpc³, the combined precision of the BAO measurements across the six different redshift bins is ~0.52%, marking a 1.2-fold improvement over the previous state-of-the-art results using only first-year data. We detect the BAO in all of these six redshift bins.","one_line_summary":"DESI measures BAO scales in six redshift bins with 0.52% combined precision using 5.7 million objects, detecting the signal at up to 9.1 sigma and finding larger scales than Planck LCDM at z<0.8.","pipeline_version":"pith-pipeline@v0.9.0","weakest_assumption":"All fiducial choices of the BAO fitting and reconstruction methodology, as well as the size of the systematic errors, were determined on the basis of the tests with mock catalogs and the blinded data catalogs; this assumes the mocks faithfully reproduce all relevant observational systematics present in the real data.","pith_extraction_headline":"DESI measures baryon acoustic oscillations to 0.52% combined precision across six redshift bins using 5.7 million galaxies and quasars."},"references":{"count":147,"sample":[{"doi":"","year":2013,"title":"Observational Probes of Cosmic Acceleration","work_id":"eb8c88d3-4422-44f1-926e-0b0445e63265","ref_index":1,"cited_arxiv_id":"1201.2434","is_internal_anchor":true},{"doi":"","year":2022,"title":"Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies","work_id":"d2c29043-63d3-4f74-946c-760d7348fd04","ref_index":2,"cited_arxiv_id":"2203.06142","is_internal_anchor":true},{"doi":"","year":2022,"title":"A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team","work_id":"5dac78be-e29e-4ec2-9a41-4adf05fc6a6a","ref_index":3,"cited_arxiv_id":"2112.04510","is_internal_anchor":true},{"doi":"","year":2005,"title":"Eisenstein, Dark energy and cosmic sound [review article] , New A Rev","work_id":"3b38f3c7-cb6e-4e44-a90c-e1df7ff9d714","ref_index":5,"cited_arxiv_id":"","is_internal_anchor":false},{"doi":"","year":2010,"title":"B. Bassett and R. Hlozek, Baryon acoustic oscillations , in Dark Energy: Observational and Theoretical Approaches, P. Ruiz-Lapuente, ed., p. 246 (2010), DOI","work_id":"886bb652-0256-44e0-8de6-fbafbabc8b15","ref_index":6,"cited_arxiv_id":"","is_internal_anchor":false}],"resolved_work":147,"snapshot_sha256":"a81061edb95a70e1e093a8a50824dbd90a2bed8d17b45e7bb2a5ae4cf5ac8004","internal_anchors":53},"formal_canon":{"evidence_count":2,"snapshot_sha256":"fac1aba152caf625edb2492b9b54148d5b86a52e6c04c3ed081c6b9efb0ca263"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}