论文标题
台风调查，附近星系中的广阔田间整体光谱法
Wide Field Integral Spectroscopy in Nearby Galaxies with the TYPHOON Survey
论文作者
论文摘要
台风计划正在生产一个由44个大型星系的光谱数据立方体的地图集，其完全空间覆盖范围为3650-9000 A.该调查为研究星际介质（ISM）属性的变化提供了一个无与伦比的机会，可以在整个星际型星系中的单个HII区域内的HII区域中进行变化。这可以为ISM的空间分布和解决特性提供关键的见解，以了解如何将金属有效地在螺旋和矮星系中重新分布。在此程序中，我们介绍了附近六个螺旋星系的早期科学结果，这是Grasha等人的台风计划的一部分。 （2022）。我们使用HIIPHOT根据H-Alpha发射线的表面亮度来鉴定银河系中的HII区域，并测量HII区域氧丰度的变化。在这项最初的工作中，我们发现，虽然螺旋模式在组织ISM中起着作用，但它并不能建立我们在所有星系中观察到的相对均匀的方位角变化。金属丰度的差异更有可能是由于与局部物理条件的牢固相关性驱动。我们发现，通过相对金属偏移$δ$（O/h）测量的电离参数与局部丰度之间存在很强的正相关，这表明局部物理条件与ISM的局部富集之间存在紧密的关系。这些变化可以通过局部，恒星形成驱动的自我增强和大规模混合驱动稀释稀释的结合来解释。
The TYPHOON program is producing an atlas of spectroscopic data cubes of 44 large-angular-sized galaxies with complete spatial coverage from 3650-9000 A. This survey provides an unparalleled opportunity to study variations in the interstellar medium (ISM) properties within individual HII regions across the entire star-forming disks of nearby galaxies. This can provide key insights into the spatial distribution and resolved properties of the ISM to understand how efficiently metals are mixed and redistributed across spirals and dwarf galaxies. In this Proceeding, we present early science results from six nearby spiral galaxies as part of the TYPHOON program from Grasha et al. (2022). We use HIIPhot to identify the HII regions within the galaxy based on the surface brightness of the H-alpha emission line and measure variations of the HII region oxygen abundance. In this initial work, we find that while the spiral pattern plays a role in organizing the ISM, it alone does not establish the relatively uniform azimuthal variations we observe across all the galaxies. Differences in the metal abundances are more likely driven by the strong correlations with the local physical conditions. We find a strong and positive correlation between the ionization parameter and the local abundances as measured by the relative metallicity offset $Δ$(O/H), indicating a tight relationship between local physical conditions and their localized enrichment of the ISM. These variations can be explained by a combination of localized, star formation-driven self-enrichment and large-scale mixing-driven dilution due to the passing of spiral density waves.
