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NGC 1569 - II的双子座GMOS/IFU光谱学：绘制银河外流的根源

Gemini GMOS/IFU spectroscopy of NGC 1569 - II: Mapping the roots of the galactic outflow

M. S. Westmoquette, L. J. Smith, J. S. Gallagher, K. M. Exter

备注：
21 pages, 23 figures, 3 tables. Accepted for publication in MNRAS
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摘要：

我们提出了一组四个双子北GMOS/IFU观测矮不规则星暴星系NGC 1569的中心扰动区，周围的著名的超级星团A和B。这直接从一篇配套论文中继续下去，在该论文中，我们描述了所采用的数据简化和分析技术，并介绍了对其中一个IFU点的分析。通过分解IFU字段中的发射线轮廓，我们绘制出识别的每个单独组件的属性，并识别出许多关系和相关性，使我们能够详细研究电离ISM的状态。我们的观察结果支持并扩展了对第一个IFU位置的分析的主要发现，在那里我们得出结论，明亮的星云发射线背后的宽（< 400 km/s）分量是在冷气体结表面的湍流混合层中产生的，该层是由快速流动的星团风的影响建立的。我们详细讨论了每个区域的运动学，电子密度和激发图，并将我们的结果与以前的研究进行了比较。我们的分析揭示了一个非常复杂的环境，有许多重叠和叠加的成分，包括溶解气体结，快速膨胀的冲击壳和嵌入的电离源，但没有证据表明有组织的整体运动。我们的结论是，这里提出的四个IFU的位置位于恒星暴区域内的能量注入，并从缺乏大量有序的气流，在准流体静力区的风内部的音速点。净流出发生在半径超过100-200 pc，但我们的数据意味着，即使在风的根部，热ISM的质量负载也是活跃的。

英文摘要：

We present a set of four Gemini-North GMOS/IFU observations of the central disturbed regions of the dwarf irregular starburst galaxy NGC 1569, surrounding the well-known super star clusters A and B. This continues on directly from a companion paper, in which we describe the data reduction and analysis techniques employed and present the analysis of one of the IFU pointings. By decomposing the emission line profiles across the IFU fields, we map out the properties of each individual component identified and identify a number of relationships and correlations that allow us to investigate in detail the state of the ionized ISM. Our observations support and expand on the main findings from the analysis of the first IFU position, where we conclude that a broad (< 400 km/s) component underlying the bright nebular emission lines is produced in a turbulent mixing layer on the surface of cool gas knots, set up by the impact of the fast-flowing cluster winds. We discuss the kinematic, electron density and excitation maps of each region in detail and compare our results to previous studies. Our analysis reveals a very complex environment with many overlapping and superimposed components, including dissolving gas knots, rapidly expanding shocked shells and embedded ionizing sources, but no evidence for organised bulk motions. We conclude that the four IFU positions presented here lie well within the starburst region where energy is injected, and, from the lack of substantial ordered gas flows, within the quasi-hydrostatic zone of the wind interior to the sonic point. The net outflow occurs at radii beyond 100-200 pc, but our data imply that mass-loading of the hot ISM is active even at the roots of the wind.

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