定量HI形态学I：THINGS半导体的多波长分析
Quantified HI Morphology I: Multi-Wavelengths Analysis of the THINGS Galaxies
摘要：
星系的演化在很大程度上是由与其他星系的相互作用和合并所驱动的，星系中的气体对相互作用非常敏感。测量这种相互作用的一种方法是使用星系图像的量化形态。公认的参数是星系图像的浓度，不对称性，平滑度，基尼系数和M20。到目前为止，这项技术的应用主要局限于restframe紫外线和光学图像。然而，随着新的射电天文台（MeerKAT，ASKAP，EVLA，WSRT/APERTIF，最终SKA）的投入使用，将打开一个关于大量星系中性原子氢气（HI）形态的新窗口。螺旋气盘的量化形态可以作为相互作用水平和频率的替代指标。星系中的HI通常在空间上更广泛，对低质量或弱相互作用更敏感。在本文中，我们探索六个形态参数计算的恒星（光学）盘的范围和气体盘的范围内的波长范围跨越紫外线，光学，近红外和远红外和21厘米（HI）的28个星系的HI附近星系调查（THINGS）。虽然THINGS样本很小，只包含一个正在进行的相互作用，但它涵盖了非相互作用和后相互作用的星系，并提供了丰富的多波长数据。我们发现，选择的区域的形态参数的计算是一个问题，比波长，它们被测量。相互作用的信号在HI中和在任何其他波长中一样好，在这些波长中，形态学被用来追踪迄今为止的相互作用率，大多数是恒星形成主导的（近紫外和远紫外）。在21厘米谱线观测中，非对称性和M20参数是最有希望作为相互作用示踪剂的参数。
英文摘要：
Galaxy evolution is driven to a large extent by interactions and mergers with other galaxies and the gas in galaxies is extremely sensitive to the interactions. One method to measure such interactions uses the quantified morphology of galaxy images. Well-established parameters are Concentration, Asymmetry, Smoothness, Gini, and M20 of a galaxy image. Thus far, the application of this technique has mostly been restricted to restframe ultra-violet and optical images. However, with the new radio observatories being commissioned (MeerKAT, ASKAP, EVLA, WSRT/APERTIF, and ultimately SKA), a new window on the neutral atomic hydrogen gas (HI) morphology of a large numbers of galaxies will open up. The quantified morphology of gas disks of spirals can be an alternative indicator of the level and frequency of interaction. The HI in galaxies is typically spatially more extended and more sensitive to low-mass or weak interactions. In this paper, we explore six morphological parameters calculated over the extent of the stellar (optical) disk and the extent of the gas disk for a range of wavelengths spanning UV, Optical, Near- and Far-Infrared and 21 cm (HI) of 28 galaxies from The HI Nearby Galaxy Survey (THINGS). Though the THINGS sample is small and contains only a single ongoing interaction, it spans both non-interacting and post-interacting galaxies with a wealth of multi-wavelength data. We find that the choice of area for the computation of the morphological parameters is less of an issue than the wavelength at which they are measured. The signal of interaction is as good in the HI as in any of the other wavelengths in which morphology has been used to trace the interaction rate to date, mostly star-formation dominated ones (near- and far-ultraviolet). The Asymmetry and M20 parameters are the ones which show the most promise as tracers of interaction in 21 cm line observations.
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