论文标题
宇宙学流体动力学模拟中的大量椎间盘星系是太暗物质主导的
Massive disc galaxies in cosmological hydrodynamical simulations are too dark matter-dominated
论文作者
论文摘要
我们研究了从宇宙流体动力学模拟和Illustristng中的大规模（MSTAR/MSUN> 5E10）圆盘星系中的圆盘 - 半连接，并将其与从烈性旋转曲线的研究研究中推断出的，并从Spitzer光度计和准确的旋转曲线（Sparc）数据集（SPARC）数据集进行了比较。我们发现，模拟和观察到的光盘之间的差异在全局和本地尺度上都出现。在全球范围内，模拟光盘居住在一个因子〜4（在鹰中）和〜2（在Illustristng中）的光晕比观察到的数据集的旋转曲线分析得出的光盘更大。我们还使用模拟盘的合成旋转曲线，以证明从旋转曲线中恢复了光环质量的质量没有系统地偏置。我们发现，模拟预测，在所有半径上，其恒星与总封闭的质量比的深色主导系统比实际星系小1.5-2。这是“反馈问题”的替代表现，因为它表明模拟的Halos托管大量盘子过于低效，无法将其重子转换为恒星，这可能是由于过于有效的恒星和/或AGN反馈实现。
We investigate the disc-halo connection in massive (Mstar/Msun>5e10) disc galaxies from the cosmological hydrodynamical simulations EAGLE and IllustrisTNG, and compare it with that inferred from the study of HI rotation curves in nearby massive spirals from the Spitzer Photometry and Accurate Rotation Curves (SPARC) dataset. We find that discrepancies between the the simulated and observed discs arise both on global and on local scales. Globally, the simulated discs inhabit halos that are a factor ~4 (in EAGLE) and ~2 (in IllustrisTNG) more massive than those derived from the rotation curve analysis of the observed dataset. We also use synthetic rotation curves of the simulated discs to demonstrate that the recovery of the halo masses from rotation curves are not systematically biased. We find that the simulations predict dark-matter dominated systems with stellar-to-total enclosed mass ratios that are a factor of 1.5-2 smaller than real galaxies at all radii. This is an alternative manifestation of the `failed feedback problem', since it indicates that simulated halos hosting massive discs have been too inefficient at converting their baryons into stars, possibly due to an overly efficient stellar and/or AGN feedback implementation.
