GHASP：螺旋星系和不规则星系的Halpha运动学巡天- VI。108个星系的新Halalpha数据立方体
GHASP : An Halpha kinematic survey of spiral and irregular galaxies - VI. New Halpha data cubes for 108 galaxies
摘要：
我们提出了一组新的108个星系，完成GHASP调查（Gassendi HAlpha调查的螺旋）获得的法布里-珀罗观测。GHASP巡天由203个螺旋星系和不规则星系的三维Ha数据立方体组成，涵盖了大范围的形态类型和绝对星等，用于运动学分析。GHASP样本是迄今为止公布的法布里-珀罗数据中最大的样本。我们推导出了Ha数据立方体，从中计算出了几乎所有星系的Ha图、径向速度场和剩余速度场、位置-速度图、自转曲线和运动学参数。在确定运动学参数，旋转曲线及其不确定性的原始改进已实施的减少过程。这种新方法是基于整个二维速度场和剩余速度场的功率谱，比传统的在速度场中使用连续冠的方法更好。其中，我们指出，形态的位置角有系统的更高的不确定性比运动学的，特别是对于星系的低倾角。星系的形态倾角没有强大的确定其形态的位置角不能正确地约束。具有高倾角的星系在其运动学倾角和其形态学倾角之间显示出更好的一致性，假设是一个薄圆盘。我们的旋转曲线的速度振幅的一致性已被检查使用塔利-费舍尔关系。我们的数据是在良好的协议与文献中发现以前的决心。然而，低倾角的星系在统计上的速度比预期的要高，而快速旋转的星系比预期的要暗。
英文摘要：
We present the Fabry-Perot observations obtained for a new set of 108 galaxies that completes the GHASP survey (Gassendi HAlpha survey of SPirals). The GHASP survey consists of 3D Ha data cubes for 203 spiral and irregular galaxies, covering a large range in morphological types and absolute magnitudes, for kinematics analysis. The GHASP sample is by now the largest sample of Fabry-Perot data ever published. We have derived Ha data cubes from which are computed Ha maps, radial velocity fields as well as residual velocity fields, position-velocity diagrams, rotation curves and the kinematical parameters for almost all galaxies. Original improvements in the determination of the kinematical parameters, rotation curves and their uncertainties have been implemented in the reduction procedure. This new method is based on the whole 2D velocity field and on the power spectrum of the residual velocity fieldrather than the classical method using successive crowns in the velocity field. Among the results, we point out that morphological position angles have systematically higher uncertainties than kinematical ones, especially for galaxies with low inclination. Morphological inclination of galaxies having no robust determination of their morphological position angle cannot be constrained correctly. Galaxies with high inclination show a better agreement between their kinematical inclination and their morphological inclination computed assuming a thin disk. The consistency of the velocity amplitude of our rotation curves have been checked using the Tully-Fisher relationship. Our data are in good agreement with previous determinations found in the literature. Nevertheless, galaxies with low inclination have statistically higher velocities than expected and fast rotators are less luminous than expected.
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