一种新的计算星系盘共转半径的方法：顶点偏差映射
A novel method to bracket the corotation radius in galaxy disks: vertex deviation maps
摘要：
利用速度椭球顶点偏差（l $_v$）映射了具有旋臂的模拟星系盘中恒星的运动学。我们使用测试粒子模拟，并首次完全自洽的高分辨率N体模型。我们比较我们的地图与紧缠绕近似模型的分析预测。我们看到，对于所有的棒模型，旋臂旋转接近刚体的方式和顶点偏差值与密度峰值的位置由过密和欠密区域界定。在这种情况下，当在圆盘旋转方向上穿过螺旋臂时，在螺旋臂处于共转（CR）和外林德布拉德共振（OLR）之间的区域中，顶点偏差符号从负变为正。相比之下，当臂部分在CR内部和OLR外部时，l $_v$从负变为正。我们建议可以使用顶点偏差模式的测量来跟踪螺旋臂的主共振的位置。我们建议，这种技术可能会利用未来的数据从盖亚和APOGEE调查。对于无限制的N-体模拟的旋臂与磁盘材料在所有半径，我们的分析表明，没有明确的相关性之间存在l $_v$和密度结构。
英文摘要：
We map the kinematics of stars in simulated galaxy disks with spiral arms using the velocity ellipsoid vertex deviation (l$_v$). We use test particle simulations, and for the first time, fully self-consistent high resolution N-body models. We compare our maps with the Tight Winding Approximation model analytical predictions. We see that for all barred models spiral arms rotate closely to a rigid body manner and the vertex deviation values correlate with the density peaks position bounded by overdense and underdense regions. In such cases, vertex deviation sign changes from negative to positive when crossing the spiral arms in the direction of disk rotation, in regions where the spiral arms are in between corotation (CR) and the Outer Lindblad Resonance (OLR). By contrast, when the arm sections are inside the CR and outside the OLR, l$_v$ changes from negative to positive.We propose that measurements of the vertex deviations pattern can be used to trace the position of the main resonances of the spiral arms. We propose that this technique might exploit future data from Gaia and APOGEE surveys. For unbarred N-body simulations with spiral arms corotating with disk material at all radii, our analysis suggests that no clear correlation exists between l$_v$ and density structures.
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