EDEN：探索嵌入Symphony中银河系质量晕N体模拟的星系盘
EDEN: Exploring Disks Embedded in N-body simulations of Milky-Way-mass halos from Symphony
AI总结：
本研究使用新模拟套件EDEN，通过嵌入随吸积演化的星系盘势重新模拟Symphony中的45个银河系质量晕，发现星系盘显著增强冷暗物质子晕的潮汐剥离，且较重的盘导致子晕丰度大幅下降，揭示了银河系因盘质量比较大和形成较早而比典型星系剥离子晕更高效。
摘要：
我们使用一套新的模拟套件EDEN，研究了星系盘对银河系（MW）质量晕（$M_{\rm vir}\sim 10^{12}\mathrm{M_{\odot}}$）内冷暗物质子晕潮汐剥离的影响。通过使用嵌入的盘势重新模拟来自N体Symphony汇编的45个MW质量放大晕，这些盘势根据UniverseMachine模型预测的恒星形成历史演化，我们将盘生长与晕吸积率自洽地联系起来，并显著扩展了所研究的盘质量和形成历史范围。我们使用基于粒子追踪的子晕查找器Symfind来增强子晕追踪的鲁棒性。我们发现，接近我们样本盘与晕质量比中位数（$M_{\ast, \rm Disk}/M_{\rm vir, host} = 2\\%$）的盘，将100 kpc内峰值质量高于$ 10^8\mathrm{M_{\odot}}$的子晕峰值质量函数降低了约$10\\%$。更重的、类似MW/M31的盘（$M_{\ast, \rm Disk}/M_{\rm vir, host} \gtrsim 5\\%$）导致降低超过$40\\%$。子晕丰度抑制在晕中心附近更为显著，对于在8 Gyr前吸积且近心点< 100 kpc轨道上的子晕，剥离尤为增强。当在固定的晕和盘组装历史内增加盘质量时，抑制进一步放大。在所有情况下，我们测量的抑制应被解释为剥离至低于质量分辨率极限，而非子晕的完全瓦解。本研究重塑了我们对MW对其卫星星系影响的理解，表明由于其较大的盘与晕质量比和较早的盘形成，它剥离子晕的效率比典型的MW质量星系更高。
英文摘要：
We investigate the impact of galactic disks on the tidal stripping of cold dark matter subhalos within Milky Way (MW)-mass halos ($M_{\rm vir}\sim 10^{12}\mathrm{M_{\odot}}$) using a new simulation suite, EDEN. By re-simulating 45 MW-mass zoom-in halos from the N-body Symphony compilation with embedded disk potentials, which evolve according to star formation histories predicted by the UniverseMachine model, we self-consistently tie disk growth to halo accretion rate and significantly expand the range of disk masses and formation histories studied. We use the particle-tracking-based subhalo finder Symfind to enhance the robustness of subhalo tracking. We find that disks near the median disk-to-halo mass ratio of our sample ($M_{\ast, \rm Disk}/M_{\rm vir, host} = 2\%$) reduce subhalo peak mass functions within 100 kpc by about $10\%$ for peak masses above $ 10^8\mathrm{M_{\odot}}$. Heavier, MW/M31-like disks ($M_{\ast, \rm Disk}/M_{\rm vir, host} \gtrsim 5\%$) lead to a reduction of more than $40\%$. Subhalo abundance suppression is more pronounced near halo centers, with particularly enhanced stripping for subhalos accreted over 8 Gyr ago on orbits with pericenters < 100 kpc. Suppression is further amplified when disk mass is increased within fixed halo and disk assembly histories. In all cases, the suppression we measure should be interpreted as stripping below the mass resolution limit rather than complete subhalo disruption. This study reshapes our understanding of the MW's impact on its satellites, suggesting it strips subhalos more efficiently than typical MW-mass galaxies due to its larger disk-to-halo mass ratio and earlier disk formation.
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