The AGORA High-resolution Galaxy Simulations Comparison Project. III. Cosmological Zoom-in Simulation of a Milky Way

DOI：

10.3847/1538-4357/ac088a

发表时间：

2021-06

期刊：

The Astrophysical Journal

影响因子：

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中科院分区：

其他

文献类型：

作者：

S. Roca-Fàbrega;Ji-hoon Kim;L. Hausammann;K. Nagamine;A. Lupi;Johnny W. Powell;I. Shimizu;D. Ceverino;J. Primack;Thomas R. Quinn;Y. Revaz;Héctor Velázquez;Tom Abel;M. Buehlmann;A. Dekel;Bili Dong;O. Hahn;C. Hummels;Ki-won Kim;Britton D. Smith;C. Strawn;R. Teyssier;M. Turk

我们提出了一套高分辨率的宇宙学放大模拟z = 4的1012 M的晕在z = 0，获得使用7个当代天体物理模拟代码（艺术-I，恩佐，拉美西斯，昌加，小工具-3，齿轮，和Gizmo）广泛使用的数值星系形成社区。气体冷却和加热以及星星形成的物理学处方与我们以前在解析解剖学（AGORA）磁盘比较中使用的处方相同，但现在考虑了宇宙学过程的影响，如宇宙膨胀，星系际气体流入，以及大质量恒星和类星体发出的宇宙紫外线背景辐射。在这项工作中，我们介绍了最仔细的比较，但不同的代码组运行的星系形成模拟，连同一系列的四个校准步骤，每个步骤的目的是减少在最终运行中采用的可调模拟参数的数量。在前两个步骤中，我们在没有星星形成的模拟中有条不紊地校准气体物理，如冷却和加热。在第三步中，我们在无恒星反馈模拟中寻求与AGORA盘比较中使用的常见星星形成处方产生的恒星总质量的一致。在最后的校准步骤中，我们激活恒星反馈，每个代码组被要求将反馈处方设置为尽可能接近其代码社区中最广泛使用的反馈处方，同时旨在将z = 4的恒星质量收敛到半经验模型预测的值。在所有参与的代码组成功完成校准步骤后，我们实现了一套宇宙学模拟，具有相似的质量组装历史，直到z = 4。通过解析目标晕的内部结构的数值精度（在z = 4时为100物理pc），我们发现代码总体上彼此一致，例如，在气体和恒星的性质，但也显示出差异，例如，环星系介质（CGM）的性质。我们认为，如果按照我们提出的校准步骤和共同的参数进行充分的测试，高分辨率宇宙学放大模拟可以有强大的和可重复的结果。邀请新的代码组加入并通过生成等效模型来丰富这种比较，或者通过采用共同的初始条件、共同的易于实现的物理包和建议的校准步骤来测试代码的兼容性。进一步的分析放大模拟在这里提出的将在未来的报告AGORA合作，包括CGM的研究，模拟额外的代码，并在较低的红移结果。

We present a suite of high-resolution cosmological zoom-in simulations to z = 4 of a 1012 M ⊙ halo at z = 0, obtained using seven contemporary astrophysical simulation codes (Art-I, Enzo, Ramses, Changa, Gadget-3, Gear, and Gizmo) widely used in the numerical galaxy formation community. The physics prescriptions for gas cooling and heating and star formation are the same as the ones used in our previous Assembling Galaxies of Resolved Anatomy (AGORA) disk comparison but now account for the effects of cosmological processes such as the expansion of the universe, intergalactic gas inflow, and the cosmic ultraviolet background radiation emitted by massive stars and quasars. In this work, we introduce the most careful comparison yet of galaxy formation simulations run by different code groups, together with a series of four calibration steps each of which is designed to reduce the number of tunable simulation parameters adopted in the final run. In the first two steps, we methodically calibrate the gas physics, such as cooling and heating, in simulations without star formation. In the third step, we seek agreement on the total stellar mass produced with the common star formation prescription used in the AGORA disk comparison, in stellar-feedback-free simulations. In the last calibration step, we activate stellar feedback, where each code group is asked to set the feedback prescription to as close to the most widely used one in its code community as possible, while aiming for convergence in the stellar mass at z = 4 to the values predicted by semiempirical models. After all the participating code groups successfully complete the calibration steps, we achieve a suite of cosmological simulations with similar mass assembly histories down to z = 4. With numerical accuracy that resolves the internal structure of a target halo (≲100 physical pc at z = 4), we find that the codes overall agree well with one another, e.g., in gas and stellar properties, but also show differences, e.g., in circumgalactic medium (CGM) properties. We argue that, if adequately tested in accordance with our proposed calibration steps and common parameters, high-resolution cosmological zoom-in simulations can have robust and reproducible results. New code groups are invited to join and enrich this comparison by generating equivalent models or to test the code’s compatibility on their own, by adopting the common initial conditions, the common easy-to-implement physics package, and the proposed calibration steps. Further analyses of the zoom-in simulations presented here will be presented in forthcoming reports from the AGORA Collaboration, including studies of the CGM, simulations by additional codes, and results at lower redshift.

The AGORA High-resolution Galaxy Simulations Comparison Project. III. Cosmological Zoom-in Simulation of a Milky Way–mass Halo

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