银晕和暗物质在棒星系动力学中的作用
The Role of Baryonic and Dark Matter in Bar Kinematics
AI总结：
研究通过观测30个MaNGA样本星系，发现棒旋特征速度与总动力学质量呈显著负相关，但暗物质质量无显著关联，揭示棒旋减速与星系质量分布的关系。
摘要：
模拟预测星系棒会随时间减速，通常归因于棒与其它区域如外盘和暗物质晕之间角动量交换。然而观测证据有限。本文通过Tremaine-Weinberg方法测量棒动力学，并结合Jeans各向异性模型估计宿主星系质量，发现棒模式速度与恒星及总动力学质量呈显著负相关，表明最慢的棒存在于最 massive 的星系中。尽管棒模式速度与暗物质质量的斜率为负，但不显著。此外，低模式速度棒具有更扩展的NFW暗物质分布，中心密度更低。同时，同步半径与恒星质量、暗物质质量及总动力学质量呈显著正相关。最后，暗物质分数或R无显著关联，可能由于测量这些参数的固有挑战。
英文摘要：
Simulations predict that bars in galaxies should slow down over time. This is often attributed to the exchange of angular momentum between the bar and other regions of the galaxy, such as the outer disc and dark matter halo, which implies that galaxies with a more massive halo or disc should be able to slow down the bar more efficiently. However, observational evidence for this process has been limited. In this work, we provide observational support for the slowing down of bars as predicted by simulations. We combine bar kinematics measurements obtained with the Tremaine-Weinberg method and host galaxy mass estimates derived from Jeans anisotropic models for a sample of 30 galaxies from the MaNGA survey. We find a statistically significant anti-correlation (>4sigma) between the bar pattern speed and both the stellar and total dynamical mass, which suggests that the slowest bars reside in the most massive galaxies. However, while the slope of the best-fit line between the pattern speed and dark matter mass is negative, it is not statistically significant (2.43sigma). We also find that bars with lower pattern speeds have more extended NFW dark matter profiles with lower central densities. Additionally, we find statistically significant correlations (>3sigma) between the corotation radius and the stellar mass, dark matter mass, and total dynamical mass. Finally, we find no significant correlations that involve the dark matter fraction or R, likely due to the inherent challenges associated with measuring these specific parameters accurately.
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