DESI DR2 results. II. Measurements of baryon acoustic oscillations and cosmological constraints

作者：M. Abdul Karim, J. Aguilar, S. P. Ahlen, Shadab Alam, L. Allen, Carlos Allende Prieto, O. Alves, Abhijeet Anand, U. Andrade, E. Armengaud, Alejandro Avilés, S. Bailey, C. Baltay, P. Bansal, A. Bault, Jayashree Behera, S. BenZvi, D. Bianchi, Chris Blake, S. Brieden, A. Brodzeller, D. Brooks, E. Buckley‐Geer, E. Burtin, R. Calderón, R. Canning, A. Carnero Rosell, P. Carrilho, Lidia Casas, F. J. Castander, M. Charles, E. Chaussidon, J. Chaves-Montero, D. Chebat, Xinyi Chen, T. Claybaugh, Shaun Cole, Andrew P. Cooper, Andrei Cuceu, Kyle Dawson, Axel de la Macorra, Arnaud de Mattia, N. Deiosso, J. Della Costa, R. Demina, Arjun Dey, Biprateep Dey, Z. Ding, P. Doel, Jerry Edelstein, Daniel J. Eisenstein, Willem Elbers, Parker Fagrelius, K. Fanning, E. Fernández-García, Simone Ferraro, Andreu Font-Ribera, J. E. Forero-Romero, Carlos S. Frenk, C. García-Quintero, Lehman H. Garrison, E. Gaztañaga, Héctor Gil-Marín, Satya Gontcho A Gontcho, D. Gonzalez, Alma X. González‐Morales, C. Gordon, D. Green, G. Gutiérrez, J. Guy, Boryana Hadzhiyska, ChangHoon Hahn, S. He, M. Herbold, H. K. Herrera-Alcantar, Ming-Feng Ho, K. Honscheid, Cullan Howlett, Dragan Huterer, Mustapha Ishak, S. Juneau, N. V. Kamble, Naim Göksel Karaçaylı, R. Kehoe, S. Kent, Alex Kim, D. Kirkby, Theodore Kisner, S. E. Koposov, Anthony Kremin, Alex Krolewski, O Lahav, C. Lamman, Martin Landriau, Dustin Lang, J. Lasker, J.M. Le Goff, L. Le Guillou, Alexie Leauthaud, M. E. Levi, Qinxun Li, Ting S. Li, K. Lodha, Martine Lokken, F. Lozano-Rodríguez, C. Magneville, Marc Manera, Paul Martini, William L. Matthewson, Aaron Meisner, J. Mena-Fernández, A. Menegas, Thiago Mergulhão, R. Miquel, John Moustakas, A. Muñoz-Gutiérrez, D. Muñoz-Santos, A. D. Myers, S. Nadathur, Krishna Naidoo, L. Napolitano, Jeffrey A. Newman, Gustavo Niz, H. E. Noriega, E. Paillas, N. Palanque‐Delabrouille, Jiaming Pan, J. A. Peacock, Marcos Pellejero-Ibáñez, Will J. Percival, A. Pérez-Fernández, Ignasi Pérez-Ràfols, Matthew M. Pieri, Claire Poppett, Francisco Prada, D. Rabinowitz, Anand Raichoor, C. Ramírez-Pérez, M. Rashkovetskyi, C. Ravoux, J. Rich, A. Rocher, Constance M. Rockosi, J. Rohlf, J. O. Román-Herrera, Ashley J. Ross, G. Rossi, Rossana Ruggeri, V. Ruhlmann-Kleider, Lado Samushia, E. Sánchez, Nicole M. Sanders, David J. Schlegel, M. Schubnell, Hee‐Jong Seo, Arman Shafieloo, R. M. Sharples, J. Silber, Francesco Sinigaglia, David Sprayberry, T. Tan, G. Tarlé, Peter L. Taylor, W. Turner, L. Arturo Ureña–López, R. Vaisakh, F. Valdés, Georgios Valogiannis, M. Vargas-Magaña, Licia Verde, Michael Walther, B. A. Weaver, David H. Weinberg, Martin White, Molly Wolfson, Christophe Yèche, Jiaxi Yu, E.A. Zaborowski, Pauline Zarrouk, Zhongxu Zhai, Hanyu Zhang, Cheng Zhao, Gong‐Bo Zhao, Rongpu Zhou, Hu Zou · 发表于：Physical review. D/Physical review. D. · 年份：2025 · DOI：10.1103/tr6y-kpc6 · 被引用次数：468 · 研究领域：Cosmology and Gravitation Theories、Galaxies: Formation, Evolution, Phenomena、Pulsars and Gravitational Waves Research

We present baryon acoustic oscillation (BAO) measurements from more than 14 million galaxies and quasars drawn from the Dark Energy Spectroscopic Instrument (DESI) Data Release 2 (DR2), based on three years of operation. For cosmology inference, these galaxy measurements are combined with DESI Lyman- α forest BAO results presented in a companion paper (M. Abdul-Karim , companion paper, .). The DR2 BAO results are consistent with DESI DR1 and the Sloan Digital Sky Survey, and their distance-redshift relationship matches those from recent compilations of supernovae (SNe) over the same redshift range. The results are well described by a flat Λ cold dark matter ( Λ CDM ) model, but the parameters preferred by BAO are in mild, 2.3 σ tension with those determined from the cosmic microwave background (CMB), although the DESI results are consistent with the acoustic angular scale θ * that is well measured by Planck. This tension is alleviated by dark energy with a time-evolving equation of state parametrized by w 0 and w a , which provides a better fit to the data, with a favored solution in the quadrant with w 0 > − 1 and w a < 0 . This solution is preferred over Λ CDM at 3.1 σ for the combination of DESI BAO and CMB data. When also including SNe, the preference for a dynamical dark energy model over Λ CDM ranges from 2.8 − 4.2 σ depending on wh...