Статья

The AGORA High-resolution Galaxy Simulations Comparison Project. VI. Similarities and Differences in the Circumgalactic Medium

Clayton StrawnDepartment of Physics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA; [email protected], [email protected]S. Roca-FàbregaDepartamento de Física de la Tierra y Astrofísica, Facultad de Ciencias Físicas, Plaza Ciencias, 1, E-28040 Madrid, SpainJoel R. PrimackDepartment of Physics, University of California at Santa Cruz, Santa Cruz, CA 95064, USA; [email protected], [email protected]Ji-hoon KimCenter for Theoretical Physics, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of KoreaAnna GeninaMax-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1, D-85748, Garching, GermanyLoïc HausammannInstitute of Physics, Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, SwitzerlandHyeonyong KimCenter for Theoretical Physics, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of KoreaAlessandro LupiDiSAT, Università degli Studi dell’Insubria, via Valleggio 11, I-22100 Como, ItalyKentaro NagamineDepartment of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka, Osaka, 560-0043, JapanJohnny W. PowellDepartment of Physics, Reed College, Portland, OR 97202, USAYves RevazInstitute of Physics, Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL), CH-1015 Lausanne, SwitzerlandIkkoh ShimizuShikoku Gakuin University, 3-2-1 Bunkyocho, Zentsuji, Kagawa, 765-8505, JapanHéctor VelázquezInstituto de Astronomía, Universidad Nacional Autónoma de México, A.P. 70-264, 04510, Mexico, D.F., MexicoTom AbelDepartment of Physics, Stanford University, Stanford, CA 94305, USADaniel CeverinoCIAFF, Facultad de Ciencias, Universidad Autónoma de Madrid, E-28049 Madrid, SpainBili DongDepartment of Physics, Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA 92093, USAMinyong JungCenter for Theoretical Physics, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of KoreaThomas QuinnDepartment of Astronomy, University of Washington, Seattle, WA 98195, USAEun-jin ShinCenter for Theoretical Physics, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of KoreaKirk S. S. BarrowDepartment of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USAAvishai DekelBoon Kiat OhCenter for Theoretical Physics, Department of Physics and Astronomy, Seoul National University, Seoul 08826, Republic of KoreaNir MandelkerRomain TeyssierDepartment of Astrophysical Sciences, Princeton University, Princeton, NJ 08544, USACameron HummelsTAPIR, California Institute of Technology, Pasadena, CA 91125, USASoumily MajiA Manchester ManGreen Valley High School, Henderson, NV 89014, USAPaul Mayerhofer

2024en

ABI

Аннотация

Abstract We analyze the circumgalactic medium (CGM) for eight commonly-used cosmological codes in the AGORA collaboration. The codes are calibrated to use identical initial conditions, cosmology, heating and cooling, and star formation thresholds, but each evolves with its own unique code architecture and stellar feedback implementation. Here, we analyze the results of these simulations in terms of the structure, composition, and phase dynamics of the CGM. We show properties such as metal distribution, ionization levels, and kinematics are effective tracers of the effects of the different code feedback and implementation methods, and as such they can be highly divergent between simulations. This is merely a fiducial set of models, against which we will in the future compare multiple feedback recipes for each code. Nevertheless, we find that the large parameter space these simulations establish can help disentangle the different variables that affect observable quantities in the CGM, e.g., showing that abundances for ions with higher ionization energy are more strongly determined by the simulation’s metallicity, while abundances for ions with lower ionization energy are more strongly determined by the gas density and temperature.

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Идентификаторы

DOI: 10.3847/1538-4357/ad12cb

Цитирования и источники

Цитирований: 2Использованных источников: 0

Показатели — AkademScholar