Статья

The EAGLE project: simulating the evolution and assembly of galaxies and their environments

Joop Schaye1Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the NetherlandsRobert A. Crain1Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, the NetherlandsR. G. BowerInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKMichelle FurlongInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKMatthieu SchallerInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKTom TheunsDepartment of Physics, University of Antwerp, Groenenborgerlaan 171, B-2020 Antwerpen, BelgiumClaudio Dalla VecchiaDepartamento de Astrofica, Universidad de La Laguna, Av. del Astrofsico Franciso Snchez s/n, E-38206 La Laguna, Tenerife, SpainCarlos S. FrenkInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKIan G. McCarthyAstrophysics Research Institute, Liverpool John Moores University, 146 Brownlow Hill, Liverpool L3 5RF, UKJohn HellyInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKAdrian JenkinsInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKYetli Rosas-GuevaraInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKSimon D. M. WhiteMax-Planck-Institut fur Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, GermanyM. BaesSterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281-S9, B-9000 Gent, BelgiumC. M. BoothDepartment of Astronomy & Astrophysics, The University of Chicago, Chicago, IL 60637, USAPeter CampsSterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281-S9, B-9000 Gent, BelgiumJulio F. NavarroDepartment of Physics and Astronomy, University of Victoria, Victoria, BC V8P 5C2, CanadaYan QuInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKAlireza RahmatiMax-Planck-Institut fur Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, GermanyTill SawalaInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UKP. ThomasAstronomy Centre, University of Sussex, Falmer, Brighton BN1 9QH, UKJames W. TrayfordInstitute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK

2014en

ABI

Аннотация

We introduce the Virgo Consortium's Evolution and Assembly of GaLaxies and their Environments (EAGLE) project, a suite of hydrodynamical simulations that follow the formation of galaxies and supermassive black holes in cosmologically representative volumes of a standard cold dark matter universe. We discuss the limitations of such simulations in light of their finite resolution and poorly constrained subgrid physics, and how these affect their predictive power. One major improvement is our treatment of feedback from massive stars and active galactic nuclei (AGN) in which thermal energy is injected into the gas without the need to turn off cooling or decouple hydrodynamical forces, allowing winds to develop without predetermined speed or mass loading factors. Because the feedback efficiencies cannot be predicted from first principles, we calibrate them to the present-day galaxy stellar mass function and the amplitude of the galaxy-central black hole mass relation, also taking galaxy sizes into account. The observed galaxy stellar mass function is reproduced to 0.2 dex over the full resolved mass range, 10 8 < M * /M 10 11 , a level of agreement close to that attained by semi-analytic models, and unprecedented for hydrodynamical simulations. We compare our results to a representative set of low-redshift observables not considered in the calibration, and find good agreement with the observed galaxy specific star formation rates, passive fractions, Tully-Fisher relation, total stellar luminosities of galaxy clusters, and column density distributions of intergalactic C IV and O VI. While the mass-metallicity relations for gas and stars are consistent with observations for M * 10 9 M (M * 10 10 M at intermediate resolution), they are insufficiently steep at lower masses. For the reference model, the gas fractions and temperatures are too high for clusters of galaxies, but for galaxy groups these discrepancies can be resolved by adopting a higher heating temperature in the subgrid prescription for AGN feedback. The EAGLE simulation suite, which also includes physics variations and higher resolution zoomed-in volumes described elsewhere, constitutes a valuable new resource for studies of galaxy formation.

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Идентификаторы

DOI: 10.1093/mnras/stu2058

Цитирования и источники

Цитирований: 4Использованных источников: 0

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