在过去的11 Gyr中盘星系强动力学演化的证据。GHASP VIII：用于高红移研究的旋转盘星系局域参考样本
Evidence for strong dynamical evolution in disk galaxies through the last 11 Gyr. GHASP VIII: A local reference sample of rotating disk galaxies for high redshift studies
摘要：
[摘要]由于它们的距离很大，高z星系在非常低的空间分辨率下被观察到。为了解开星系运动学的演化从低分辨率的影响，我们已经使用的法布里-珀罗3D哈数据立方体附近的153个孤立星系的GHASP调查，以模拟数据立方体的星系在z=1.7。我们发现，内部的速度梯度降低，是负责的速度色散图中的峰值。为了从低分辨率数据中恢复参数，建立了旋转圆盘的玩具模型。分辨率差使得运动学倾角不确定，中心难以恢复。对于70%的样品，主轴的检索精度高于5度。玩具模型还能以令人满意的精度从统计上反演星系的最大速度和平均速度色散。这验证了Tully-Fisher关系在高z星系中的应用，但分辨率的损失导致了高z星系的较低斜率。我们的结论是，主要的运动学参数更好地约束的光学半径大于三倍的看到的星系。模拟的数据已经与实际的高z星系的数据在红移范围3>z>0.4进行了比较。对于旋转主导的星系，我们发现，使用速度色散中心峰作为旋转盘的签名可能会错误分类缓慢和固体旋转体（约30%的样本）。我们表明，投影数据不能再现高z星系中观察到的高速色散，除非没有光束拖尾校正。这无疑意味着，在当地的演化星系的相反，在高红移至少存在一个人口的盘星系，其中很大一部分的动力学支持是由于随机运动。
英文摘要：
[Abridged] Due to their large distances, high-z galaxies are observed at a very low spatial resolution. In order to disentangle the evolution of galaxy kinematics from low resolution effects, we have used Fabry-Perot 3D Ha data-cubes of 153 nearby isolated galaxies from the GHASP survey to simulate data-cubes of galaxies at z=1.7. We show that the inner velocity gradient is lowered and is responsible for a peak in the velocity dispersion map. Toy-models of rotating disks have been built to recover the parameters from low resolution data. The poor resolution makes the kinematical inclination uncertain and the center difficult to recover. The major axis is retrieved with an accuracy higher than 5deg for 70% of the sample. Toy-models also enable to retrieve statistically the maximum velocity and the mean velocity dispersion of galaxies with a satisfying accuracy. This validates the use of the Tully-Fisher relation for high-z galaxies but the loss of resolution induces a lower slope at high-z. We conclude that the main kinematic parameters are better constrained for galaxies with an optical radius larger than three times the seeing. The simulated data have been compared to actual high-z galaxies data in the redshift range 3>z>0.4. For rotation-dominated galaxies, we find that the use of the velocity dispersion central peak as a signature of rotating disks may misclassify slow and solid body rotators (~30% of our sample). We show that the projected data cannot reproduce the high velocity dispersion observed in high-z galaxies except when no beam smearing correction is applied. This unambiguously means that, at the opposite of local evolved galaxies, there exists at high redshift at least a population of disk galaxies for which a large fraction of the dynamical support is due to random motions.
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