Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
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DOI：
10.3847/1538-3881/aced8e
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发表时间：
2023-09
期刊：
影响因子：
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通讯作者：
L. C. Hunter;L. van Zee;K. McQuinn;R. E. Cohen;Madison Markham;A. Dolphin
中科院分区：
文献类型：
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作者：
L. C. Hunter;L. van Zee;K. McQuinn;R. E. Cohen;Madison Markham;A. Dolphin
了解星际介质（ISM）中恒星反馈和湍流的相互作用对于模拟星系的演化至关重要。为了确定恒星反馈驱动ISM中湍流的时间尺度，我们对附近的恒星形成矮星系UGC 4305进行了空间分辨的多波长研究。作为局部尺度（400 pc）湍流的指标，我们利用了来自IFU Hα观测的电离气体速度色散和来自甚大阵H i合成观测的原子气体速度色散和能量表面密度。这些指标的湍流进行了测试，对星星形成的历史，在过去的560万年来自颜色星等图使用斯皮尔曼的等级相关系数。在400秒差距尺度下，H i湍流的测量值与70- 1.4亿年前的星星形成之间的相关性最强。我们重复了我们对UGC 4305当前湍流和过去星星形成活动在多个物理尺度（1560和800 pc）上的分析，以确定是否有迹象表明相关时间尺度随着物理尺度的变化而变化。在更大的物理尺度上没有发现明显的相关性，强调了将星星形成驱动的湍流作为局部现象进行分析的重要性。
Understanding the interplay of stellar feedback and turbulence in the interstellar medium (ISM) is essential to modeling the evolution of galaxies. To determine the timescales over which stellar feedback drives turbulence in the ISM, we performed a spatially resolved, multiwavelength study of the nearby star-forming dwarf galaxy UGC 4305. As indicators of turbulence on local scales (400 pc), we utilized ionized gas velocity dispersion derived from IFU Hα observations and atomic gas velocity dispersion and energy surface densities derived from H i synthesis observations with the Very Large Array. These indicators of turbulence were tested against star formation histories over the past 560 Myr derived from color–magnitude diagrams using Spearman’s rank correlation coefficient. The strongest correlation identified at the 400 pc scale is between measures of H i turbulence and star formation 70–140 Myr ago. We repeated our analysis of UGC 4305's current turbulence and past star formation activity on multiple physical scales (∼560 and 800 pc) to determine whether there are indications of changes in the correlation timescale with changes to the physical scale. No notable correlations were found at larger physical scales, emphasizing the importance of analyzing star formation-driven turbulence as a local phenomenon.