Статья

Towards testing the theory of gravity with DESI: summary statistics, model predictions and future simulation requirements

Shadab AlamInstitute for Astronomy, University of Edinburgh, Edinburgh, U.KChristian ArnoldInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KAlejandro AvilésConsejo Nacional de Ciencia y Tecnologıa, Av. Insurgentes Sur 1582, Colonia Credito Constructor, Del. Benito Juárez C.P. 03940, México D.F. MéxicoRachel BeanDepartment of Astronomy, Cornell University, Ithaca, NY 14853, U.S.AYan-Chuan CaiInstitute for Astronomy, University of Edinburgh, Edinburgh, U.KMarius CautunInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KJorge L. Cervantes–CotaDepartamento de Física, Instituto Nacional de Investigaciones Nucleares, Apartado Postal 18-1027, Col. Escandón, Ciudad de México,11801, MéxicoCarolina Cuesta-LazaroInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KN. Chandrachani DeviDepartment of Physics, Manipur University, Canchipur, 795003, Manipur, IndiaAlexander EggemeierArgelander-Institut für Astronomie, Auf dem Hügel 71, D-53121 Bonn, GermanyS. FromenteauInstituto de Ciencias Físicas, Universidad Nacional Autónoma de México, Av. Universidad s/n, 62210 Cuernavaca, Mor., MéxicoAlma X. González‐MoralesConsejo Nacional de Ciencia y Tecnologıa, Av. Insurgentes Sur 1582, Colonia Credito Constructor, Del. Benito Juárez C.P. 03940, México D.F. MéxicoV. HalenkaUniversity of Michigan, Department of Physics, 1085 South University, Ann Arbor, 48109, U.S.AJian-hua HeInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KWojciech A. HellwingCenter for Theoretical Physics, Polish Academy of Sciences, Al. Lotników 32/46, 02-668 Warsaw, PolandCésar Hernández‐AguayoExcellence Cluster ORIGINS, Boltzmannstrasse 2, D-85748 Garching, GermanyMustapha IshakDepartment of Physics, The University of Texas at Dallas, Richardson, Texas 75080, U.S.AK. KoyamaInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, Hampshire, PO 3FX, U.KBaojiu LiInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KAxel de la MacorraInstituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Ciudad de México, MéxicoJennifer Meneses RizoInstituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Ciudad de México, MéxicoChristopher J. MillerUniversity of Michigan, Department of Astronomy, Department of Physics, 1085 South University, Ann Arbor, 48109, U.S.AEva-Maria MuellerDepartment of Physics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH, U.KGustavo NizDepartamento de Física, División de Ciencias e Ingenierías, Campus León, Universidad de Guanajuato, León 37150, MéxicoPierros NtelisAix Marseille Univ, CNRS/IN2P3, CPPM, Marseille, FranceMatia Rodríguez OteroInstituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Ciudad de México, MéxicoCristiano G. SabiuNatural Science Research Institute, University of Seoul, 163 Seoulsiripdaero, Dongdaemun-gu, Seoul, 02504, Republic of KoreaZachary SlepianDepartment of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, U.S.AAlejo StarkUniversity of Michigan, Department of Astronomy, Department of Physics, 1085 South University, Ann Arbor, 48109, U.S.AO. ValenzuelaInstituto de Astronomia, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, MéxicoGeorgios ValogiannisDepartment of Astronomy, Cornell University, Ithaca, NY 14853, U.S.AM. Vargas-MagañaInstituto de Física, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, Ciudad de México, MéxicoHans A. WintherInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, Hampshire, PO 3FX, U.KPauline ZarroukInstitute for Computational Cosmology, Department of Physics, Durham University, South Road, Durham DH1 3LE, U.KGong‐Bo ZhaoInstitute of Cosmology and Gravitation, University of Portsmouth, Portsmouth, Hampshire, PO 3FX, U.KYi ZhengSchool of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Tangjia, Zhuhai, 519082, China

2021en

ABI

Аннотация

Abstract Shortly after its discovery, General Relativity (GR) was applied to predict the behavior of our Universe on the largest scales, and later became the foundation of modern cosmology. Its validity has been verified on a range of scales and environments from the Solar system to merging black holes. However, experimental confirmations of GR on cosmological scales have so far lacked the accuracy one would hope for — its applications on those scales being largely based on extrapolation and its validity there sometimes questioned in the shadow of the discovery of the unexpected cosmic acceleration. Future astronomical instruments surveying the distribution and evolution of galaxies over substantial portions of the observable Universe, such as the Dark Energy Spectroscopic Instrument (DESI), will be able to measure the fingerprints of gravity and their statistical power will allow strong constraints on alternatives to GR. In this paper, based on a set of N -body simulations and mock galaxy catalogs, we study the predictions of a number of traditional and novel summary statistics beyond linear redshift distortions in two well-studied modified gravity models — chameleon f ( R ) gravity and a braneworld model — and the potential of testing these deviations from GR using DESI. These summary statistics employ a wide array of statistical properties of the galaxy and the underlying dark matter field, including two-point and higher-order statistics, environmental dependence, redshift space distortions and weak lensing. We find that they hold promising power for testing GR to unprecedented precision. The major future challenge is to make realistic, simulation-based mock galaxy catalogs for both GR and alternative models to fully exploit the statistic power of the DESI survey (by matching the volumes and galaxy number densities of the mocks to those in the real survey) and to better understand the impact of key systematic effects. Using these, we identify future simulation and analysis needs for gravity tests using DESI.

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Идентификаторы

DOI: 10.1088/1475-7516/2021/11/050

Цитирования и источники

Цитирований: 4Использованных источников: 0

Показатели — AkademScholar