论文标题
震动破坏了低露珠性活性银核中的小PAH分子的证据
Evidence that Shocks Destroy Small PAH Molecules in Low-luminosity Active Galactic Nuclei
论文作者
论文摘要
我们将映射模式中红外Spitzer光谱与互补的红外成像结合在一起，以对来自66个附近星系中央区域的多环芳烃（PAHS）发射进行空间解决研究，大致均匀地均匀地分为星形型系统和低亮型环境质量和低亮型壁式核核（Agns）。结合用于类星体的类似测量结果，我们旨在了解PAH在广泛的黑洞积聚功率上的物理特性，目的是识别可用于探测AGN对宿主星系影响的观察诊断。尽管PAH发射与星形形成区域的远程脉络膜光度密切相关，而AGN的空间解析区域往往是PAH缺陷的。此外，AGN区域平均表现出较小的PAH6.2μm/7.7μm，较大的PAH11.3μm/7.7μm带比。尽管当前的数据是高度限制的，但他们认为这些异常的PAH带比不能单独用AGN辐射场的影响来解释。取而代之的是，他们暗示，辐射过程和冲击的综合效应可能会破坏小晶粒，这些晶粒与喷气机和流出的辐射和流出有可能与高度亚埃德丁顿，辐射效率低下的AGN相关联。尽管类星体也呈现出PAH赤字和不寻常的PAH带比，但与更弱的AGN中观察到的特征相比，它们的特征在细节上有所不同，这可能是其能量反馈方式基本差异的可能指标。
We combined mapping-mode mid-infrared Spitzer spectra with complementary infrared imaging to perform a spatially resolved study of polycyclic aromatic hydrocarbons (PAHs) emission from the central regions of 66 nearby galaxies, roughly evenly divided into star-forming systems and low-luminosity active galactic nuclei (AGNs). In conjunction with similar measurements available for quasars, we aim to understand the physical properties of PAHs across a broad range of black hole accretion power, with the goal of identifying observational diagnostics that can be used to probe the effect of AGNs on the host galaxy. Whereas the PAH emission correlates tightly with far-ultraviolet luminosity in star-forming regions, the spatially resolved regions of AGNs tend to be PAH-deficient. Moreover, AGN regions exhibit on average smaller PAH 6.2 μm/7.7 μm and larger PAH 11.3 μm/7.7 μm band ratios. Although the current data are highly restrictive, they suggest that these anomalous PAH band ratios cannot be explained by the effects of the AGN radiation field alone. Instead, they hint that small grains may be destroyed by the combined effects of radiative processes and shocks, which are plausibly linked to jets and outflows preferentially associated with highly sub-Eddington, radiatively inefficient AGNs. While quasars also present a PAH deficit and unusual PAH band ratios, their characteristics differ in detail compared to those observed in more weakly accreting AGNs, a possible indicator of fundamental differences in their modes of energy feedback.
