定量HI形态II：WHISP柱密度图中的偏心性和相互作用
Quantified HI Morphology II : Lopsidedness and Interaction in WHISP Column Density Maps
摘要：
旋涡星系气体盘的不对称性是盘的形态、轮廓和运动学中的一种普遍现象。同时，星系星盘的不对称性，结合其他形态参数，已经被广泛用作星系样本中最近合并或相互作用的指示。恒星螺旋盘的量化形态是确定宇宙大部分年龄合并率的一种途径。本文利用Westerbork不规则星系和螺旋星系中性氢的观测数据，测量了HI柱密度图的定量形态学参数。这些是浓度，不对称性，平滑度，基尼系数，M20，以及我们自己的一个附加参数，二阶矩（GM）的基尼系数。我们的目的是确定是否可以确定这些参数不平衡或相互作用的磁盘。我们的样本141 HI地图有所有以前的分类，他们的片面性和相互作用。我们发现，不对称性，M20，我们的新GM参数相关性弱，与以前的形态片面性量化。这三个参数可以用来计算一个HI盘在形态上是不平衡的概率，但不能明确地确定它，然而，我们确实发现用形态参数可以很好地解决HI盘是否相互作用的问题。来自文献的参数切割不直接从紫外转换为HI，但是使用不对称性和M20或浓度和M20的组合的新选择标准非常有效。我们建议，未来的全天HI调查可能会使用这些参数的列密度图，以确定合并的分数，从而在本地宇宙的高精度率。
英文摘要：
Lopsidedness of the gaseous disk of spiral galaxies is a common phenomenon in disk morphology, profile and kinematics. Simultaneously, the asymmetry of a galaxy's stellar disk, in combination with other morphological parameters, has seen extensive use as an indication of recent merger or interaction in galaxy samples. Quantified morphology of stellar spiral disks is one avenue to determine the merger rate over much of the age of the Universe. In this paper, we measure the quantitative morphology parameters for the HI column density maps from the Westerbork observations of neutral Hydrogen in Irregular and SPiral galaxies (WHISP). These are Concentration, Asymmetry, Smoothness, Gini, M20, and one addition of our own, the Gini parameter of the second order moment (GM). Our aim is to determine if lopsided or interacting disks can be identified with these parameters. Our sample of 141 HI maps have all previous classifications on their lopsidedness and interaction. We find that the Asymmetry, M20, and our new GM parameter correlate only weakly with the previous morphological lopsidedness quantification. These three parameters may be used to compute a probability that an HI disk is morphologically lopsided but not unequivocally to determine it. However, we do find that that the question whether or not an HI disk is interacting can be settled well using morphological parameters. Parameter cuts from the literature do not translate from ultraviolet to HI directly but new selection criteria using combinations of Asymmetry and M20 or Concentration and M20, work very well. We suggest that future all-sky HI surveys may use these parameters of the column density maps to determine the merger fraction and hence rate in the local Universe with a high degree of accuracy.
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