ATLAS3D项目- XVII。早型星系中恒星盘的光度学和运动学特征的联系
The ATLAS3D project - XVII. Linking photometric and kinematic signatures of stellar discs in early-type galaxies
摘要：
[摘要]我们通过拟合单个Sersic轮廓并将所有非棒对象（260个对象中的180个）分解为由指数和一般Sersic函数参数化的两个分量来分析ATLAS 3D样本的星系中的形态结构。这项分析的目的是寻找附近的早期型星系的光分布中的光盘的签名，并将它们与运动学特性进行比较。不推荐使用单分量的Sersic指数来区分慢转星系和快转星系，甚至晚型星系和早型星系。假设n>3的天体是慢旋天体（或椭圆天体），那么只有22%的概率将其正确分类为慢旋天体（或37%的概率）。我们表明，指数的子组件，以及光配置文件只配备了一个单一的组成部分，低Sersic指数，可以与运动学证据盘在早期类型的星系。快旋和慢旋的圆盘与总光之比的中位数分别为0.41和0.0。同样，中位Sersic指数的隆起（一般Sersic分量）是1.7和4.8的快速和慢速旋转，分别。总的来说，盘或盘状结构存在于83%的早期类型星系中，这些星系没有酒吧，并且它们显示了完整的盘与总光比。早期星系中的圆盘占分析（非棒）物体总质量的40%左右。圆盘和凸起的分解可以作为快速和慢速旋转体之间分离的粗略近似，但它不能替代，因为正确识别慢速旋转体的概率只有59%。动能（即投射角动量）仍然是减轻倾斜效应影响的最佳方法。
英文摘要：
[Abridged] We analyse the morphological structures in galaxies of the ATLAS3D sample by fitting a single Sersic profile and decomposing all non-barred objects (180 of 260 objects) in two components parameterised by an exponential and a general Sersic function. The aim of this analysis is to look for signatures of discs in light distributions of nearby early-type galaxies and compare them to kinematic properties. Using Sersic index from single component fits for a distinction between slow and fast rotators, or even late- and early-type galaxies, is not recommended. Assuming that objects with n>3 are slow rotators (or ellipticals), there is only a 22 per cent probability to correctly classify objects as slow rotators (or 37 per cent of previously classified as ellipticals). We show that exponential sub-components, as well as light profiles fitted with only a single component of a low Sersic index, can be linked with the kinematic evidence for discs in early-type galaxies. The median disk-to-total light ratio for fast and slow rotators is 0.41 and 0.0, respectively. Similarly, the median Sersic indices of the bulge (general Sersic component) are 1.7 and 4.8 for fast and slow rotators, respectively. Overall, discs or disc-like structures, are present in 83 per cent of early-type galaxies which do not have bars, and they show a full range of disk-to-total light ratios. Discs in early-type galaxies contribute with about 40 per cent to the total mass of the analysed (non-barred) objects. The decomposition into discs and bulges can be used as a rough approximation for the separation between fast and slow rotators, but it is not a substitute, as there is only a 59 per cent probability to correctly recognise slow rotators. Kinematics (i.e. projected angular momentum) remains the best approach to mitigate the influence of the inclination effects.
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