M81群矮不规则星系DDO 165。II。将最近的恒星形成与ISM结构和动力学联系起来
The M81 Group Dwarf Irregular Galaxy DDO 165. II. Connecting Recent Star Formation with ISM Structures and Kinematics
摘要：
我们比较的恒星星族和复杂的中性气体动力学的M81组dIrr星系DDO 165使用的数据从HST和VLA。论文我确定了两个运动学上不同的HI组件，多个本地化的高速气体功能，和八个HI孔和壳（其中最大的跨度约2.2x1.1千秒差距）。利用DDO 165中恒星星族的时空信息，我们比较了过去5亿年中恒星形成的模式与HI动力学。我们提取本地化的恒星形成的历史，在6的8个HI孔中确定的文件I，以及其他23个地区的样本范围内的恒星密度和中性气体的性质。从人口合成模型，我们得出的能量输出（从恒星风和超新星）的恒星星族在这些地区在过去的1亿年，并与精细的估计所需的能量创建HI孔比较。在所有的情况下，我们发现，“反馈”是积极的，能够创造所观察到的结构在ISM。许多地区的显着的能量输入反馈缺乏相干HI结构，但显示出突出的本地化的高速气体功能，这种反馈签名是一个自然的产品的时间和空间分布的恒星形成。在DDO 165中，恒星形成活动的延长期（持续超过1 Gyr）能够在中性ISM中产生观测到的空穴和高速气体特征。
英文摘要：
We compare the stellar populations and complex neutral gas dynamics of the M81 group dIrr galaxy DDO 165 using data from the HST and the VLA. Paper I identified two kinematically distinct HI components, multiple localized high velocity gas features, and eight HI holes and shells (the largest of which spans ~2.2x1.1 kpc). Using the spatial and temporal information from the stellar populations in DDO 165, we compare the patterns of star formation over the past 500 Myr with the HI dynamics. We extract localized star formation histories within 6 of the 8 HI holes identified in Paper I, as well as 23 other regions that sample a range of stellar densities and neutral gas properties. From population synthesis modeling, we derive the energy outputs (from stellar winds and supernovae) of the stellar populations within these regions over the last 100 Myr, and compare with refined estimates of the energies required to create the HI holes. In all cases, we find that "feedback" is energetically capable of creating the observed structures in the ISM. Numerous regions with significant energy inputs from feedback lack coherent HI structures but show prominent localized high velocity gas features; this feedback signature is a natural product of temporally and spatially distributed star formation. In DDO 165, the extended period of heightened star formation activity (lasting more than 1 Gyr) is energetically capable of creating the observed holes and high velocity gas features in the neutral ISM.
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