GOGREEN: A critical assessment of environmental trends in cosmological hydrodynamical simulations at z ≈ 1

Author:

Kukstas Egidijus123ORCID,Balogh Michael L45ORCID,McCarthy Ian G1ORCID,Bahé Yannick M6ORCID,De Lucia Gabriella7ORCID,Jablonka Pascale89ORCID,Vulcani Benedetta10ORCID,Baxter Devontae C11ORCID,Biviano Andrea712ORCID,Cerulo Pierluigi13ORCID,Chan Jeffrey C14ORCID,Cooper M C11ORCID,Demarco Ricardo15ORCID,Finoguenov Alexis16ORCID,Font Andreea S1ORCID,Lidman Chris1718ORCID,Marchioni Justin4,McGee Sean19ORCID,Muzzin Adam20ORCID,Nantais Julie21ORCID,Old Lyndsay22ORCID,Pintos-Castro Irene23ORCID,Poggianti Bianca10ORCID,Reeves Andrew M M45ORCID,Rudnick Gregory24ORCID,Sarron Florian25,van der Burg Remco26ORCID,Webb Kristi45ORCID,Wilson Gillian14ORCID,Yee Howard K C27ORCID,Zaritsky Dennis28ORCID

Affiliation:

1. Astrophysics Research Institute, Liverpool John Moores University , Liverpool L3 5RF, UK

2. Department of Physics, The University of Liverpool , Liverpool L69 3BX, UK

3. The Cockcroft Institute of Accelerator Science and Technology , Warrington WA4 4AD, UK

4. Department of Physics and Astronomy, University of Waterloo , Waterloo ON N2L 3G1, Canada

5. Waterloo Centre for Astrophysics, University of Waterloo , Waterloo ON N2L 3G1, Canada

6. Leiden Observatory, Leiden University , PO Box 9513, NL-2300 RA Leiden, the Netherlands

7. INAF – Osservatorio Astronomico di Trieste , via G.B. Tiepolo 11, I-34143 Trieste, Italy

8. Laboratoire d’astrophysique, École Polytechnique Fédérale de Lausanne (EPFL) , CH-1290 Sauverny, Switzerland

9. GEPI, Observatoire de Paris, Université PSL, CNRS , Place Jules Janssen, F-92190 Meudon, France

10. INAF – Osservatorio astronomico di Padova , Vicolo Osservatorio 5, I-35122 Padova, Italy

11. Department of Physics and Astronomy, University of California , Irvine, 4129 Reines Hall, Irvine, CA 92697, USA

12. IFPU, Institute for Fundamental Physics of the Universe , via Beirut 2, I-34014 Trieste, Italy

13. Departamento de Ingeniería Informática y Ciencias de la Computación, Universidad de Concepción , Concepción, Chile

14. Department of Physics and Astronomy, University of California , Riverside, 900 University Avenue, Riverside, CA 92521, USA

15. Departamento de Astronomía, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción , Concepción, Chile

16. Department of Physics, University of Helsinki , Gustaf Hällströmin katu 2a, FI-00014 Helsinki, Finland

17. Research School of Astronomy and Astrophysics, The Australian National University , ACT 2601, Australia

18. Centre for Gravitational Astrophysics, College of Science, The Australian National University , ACT 2601, Australia

19. School of Physics and Astronomy, University of Birmingham , Edgbaston, Birmingham B15 2TT, England

20. Department of Physics and Astronomy, York University , 4700 Keele Street, Toronto, Ontario ON MJ3 1P3, Canada

21. Departamento de Ciencias Físicas, Universidad Andres Bello , Fernandez Concha 700, Las Condes 7591538, Santiago, Región Metropolitana, Chile

22. European Space Agency (ESA), European Space Astronomy Centre , Villanueva de la Cañada, E-28691 Madrid, Spain

23. Centro de Estudios de Física del Cosmos de Aragón (CEFCA) , Plaza San Juan 1, E-44001 Teruel, Spain

24. Department of Physics and Astronomy, The University of Kansas , 1251 Wescoe Hall Drive, Lawrence, KS 66045, USA

25. Institut de Recherche en Astrophysique et Planétologie , 14 Avenue Edouard Belin, 31400, Toulouse, France

26. European Southern Observatory , Karl-Schwarzschild-Str. 2, D-85748 Garching, Germany

27. Department of Astronomy and Astrophysics, University of Toronto , Toronto, M5S 3H4, Canada

28. Steward Observatory and Department of Astronomy, University of Arizona , 933 N. Cherry Ave., Tucson, AZ 85721, USA

Abstract

ABSTRACT Recent observations have shown that the environmental quenching of galaxies at z ∼ 1 is qualitatively different to that in the local Universe. However, the physical origin of these differences has not yet been elucidated. In addition, while low-redshift comparisons between observed environmental trends and the predictions of cosmological hydrodynamical simulations are now routine, there have been relatively few comparisons at higher redshifts to date. Here we confront three state-of-the-art suites of simulations (BAHAMAS+MACSIS, EAGLE+Hydrangea, IllustrisTNG) with state-of-the-art observations of the field and cluster environments from the COSMOS/UltraVISTA and GOGREEN surveys, respectively, at z ∼ 1 to assess the realism of the simulations and gain insight into the evolution of environmental quenching. We show that while the simulations generally reproduce the stellar content and the stellar mass functions of quiescent and star-forming galaxies in the field, all the simulations struggle to capture the observed quenching of satellites in the cluster environment, in that they are overly efficient at quenching low-mass satellites. Furthermore, two of the suites do not sufficiently quench the highest mass galaxies in clusters, perhaps a result of insufficient feedback from AGN. The origin of the discrepancy at low stellar masses ($M_* \lesssim 10^{10}$ M⊙), which is present in all the simulations in spite of large differences in resolution, feedback implementations, and hydrodynamical solvers, is unclear. The next generation of simulations, which will push to significantly higher resolution and also include explicit modelling of the cold interstellar medium, may help us to shed light on the low-mass tension.

Funder

NSERC

European Research Council

NWO

National Science Foundation

NASA

Space Telescope Science Institute

ANID

BEIS

STFC

Durham University

Spanish Ministry of Science and Innovation

Brinson Foundation

Moore Foundation

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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