标题： 沿银河平面的银河红外气泡的系统研究，使用AKARI和赫歇尔。 II. 气泡周围尘埃组分的空间分布 显示英文标题

标题： A systematic study of Galactic infrared bubbles along the Galactic plane with AKARI and Herschel. II. Spatial distributions of dust components around the bubbles

摘要： 银河系红外（IR）气泡，在中红外波长下表现为壳状结构，已知在其壳边界内存在大质量恒星。在我们之前的研究中，Hanaoka 等（2019）将研究区域扩展到整个银河平面（$0^{\circ} \leq l \leq 360^{\circ}$，$|b| \leq 5^{\circ}$），并研究了内银河和外银河区域中壳形态和IR气泡的IR光度之间的系统性差异。在本研究中，利用AKARI和WISE在中红外以及Herschel在远红外的高空间分辨率数据，我们调查了每个IR气泡周围尘埃组分的空间分布，以讨论恒星形成活动与IR气泡尘埃特性之间的关系。对于Hanaoka 等（2019）研究的247个IR气泡，本研究调查了其中165个IR气泡，它们具有Herschel数据（$|b| \leq 1^{\circ}$）和已知的距离。我们为每个IR气泡周围创建了像素级的光谱能量分布，并使用由多环芳烃（PAHs）、热尘、温尘和冷尘组成的尘埃模型对其进行分解。结果表明，内银河区域中尘埃加热源相对于壳中心的偏移量系统性地大于外银河区域。许多内银河区域中的破裂气泡显示出偏移方向与从中心出发的破裂壳方向之间的大角度。此外，内银河区域中IR气泡周围的PAH强度和冷尘发射率的空间变化大于外银河区域。我们根据星际环境和与IR气泡相关的高质恒星形成机制来讨论这些结果。 显示英文摘要

摘要： Galactic infrared (IR) bubbles, which can be seen as shell-like structures at mid-IR wavelengths, are known to possess massive stars within their shell boundaries. In our previous study, Hanaoka et al. (2019) expanded the research area to the whole Galactic plane ($0^{\circ} \leq l \leq 360^{\circ}$, $|b| \leq 5^{\circ}$) and studied systematic differences in the shell morphology and the IR luminosity of the IR bubbles between inner and outer Galactic regions. In this study, utilizing high spatial-resolution data of AKARI and WISE in the mid-IR and Herschel in the far-IR, we investigate the spatial distributions of dust components around each IR bubble to discuss the relation between the star-formation activity and the dust properties of the IR bubbles. For the 247 IR bubbles studied in Hanaoka et al. (2019), 165 IR bubbles are investigated in this study, which have the Herschel data ($|b| \leq 1^{\circ}$) and known distances. We created their spectral energy distributions on a pixel-by-pixel basis around each IR bubble, and decomposed them with a dust model consisting of polycyclic aromatic hydrocarbons (PAHs), hot dust, warm dust and cold dust. As a result, we find that the offsets of dust heating sources from the shell centers in inner Galactic regions are systematically larger than those in outer Galactic regions. Many of the broken bubbles in inner Galactic regions show large angles between the offset and the broken shell directions from the center. Moreover, the spatial variations of the PAH intensity and cold dust emissivity around the IR bubbles in inner Galactic regions are larger than those in outer Galactic regions. We discuss these results in light of the interstellar environments and the formation mechanism of the massive stars associated with the IR bubbles.