ULIRGs中温暖高速致密气体的起源
Origin of Warm High-Velocity Dense Gas in ULIRGs
摘要：
基于银河系中心区域恒星形成星际气体的3-D流体动力学模型，研究了在某些ULIRGs中发现的分子吸收的可能来源。IRAS 08752+3915中的CO吸收表明，蓝移、温暖（$\sim 200-300$ K）、致密（$>10^6$ cm $^{-3}$）的分子气体可能是由超大质量黑洞周围的非均匀星际介质（ISM）的最内部区域引起的。在ULIRGs和Seyfert 2星系中很少观察到具有吸收的致密气体，这可能只是表明高密度区域只占遮蔽物质的很小体积分数。如果ISM的不均匀结构是由不稳定性的非线性发展引起的，这是自然预期的。该模型预测的湍流速度场的遮蔽材料，因此蓝移和红移的气体应观察到几乎相同的概率为足够大的统计样本。
英文摘要：
Possible origins of the molecular absorption discovered in some ULIRGs are investigated, based on a 3-D hydrodynamic model of star-forming interstellar gas in a galactic central region. The blue-shifted, warm ($\sim 200-300$ K), dense ($>10^6$ cm$^{-3}$) molecular gas suggested by CO absorption in IRAS 08752+3915 could be caused by the innermost region of the inhomogeneous inter-stellar medium (ISM) around a supermassive black hole. The infrequent observations of the dense gas with absorption in ULIRGs and Seyfert 2 galaxies could simply suggest that the high-density regions occupy only a very small volume fraction of the obscuring material. This is naturally expected if the inhomogeneous structure of the ISM is caused by non-linear development of instabilities. The model predicts a turbulent velocity field in the obscuring material, therefore blue- and red-shifted gases should be observable with nearly the same probability for the large enough statistical samples.
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