论文标题
NGC253和银河系中心的湍流气体结构
The turbulent gas structure in the centers of NGC253 and the Milky Way
论文作者
论文摘要
我们使用树状图和分辨率，CO（1-0）和CO（3-2）中的分辨率和分辨率，区域，面积和噪声匹配的数据集比较了NGC253的Starbursting中心和银河系中心（GC）的分子气体性质和银河系中心（GC）。我们发现NGC253中的尺寸线宽度关系和GC具有相似的斜率，但是NGC253的线宽度较大，构成〜2-3的因素。 $σ^2/r $依赖性对列密度的依赖性表明，在GC中，在10-100 pc的尺度上，$ n> 3 \ 3 \ times10^{21} $ cm $^{ - 2} $与重力结构兼容。在NGC253中，这仅是列密度$ n> 3 \ times10^{22} $ cm $^{ - 2} $的情况。 NGC253中的线宽度增加起源于下柱密度气体。这种高速分散体，而不是重力自我结合的气体可能是由于高平均密度和星爆反馈的组合所产生的瞬态结构。高密度在整个Starburst的体积中转动气体分子，并且反馈注射能量和动量会显着增加给定空间尺度上的速度散布，超过了GC中观察到的速度。
We compare molecular gas properties in the starbursting center of NGC253 and the Milky Way Galactic Center (GC) on scales of ~1-100 pc using dendograms and resolution-, area- and noise-matched datasets in CO (1-0) and CO (3-2). We find that the size-line width relations in NGC253 and the GC have similar slope, but NGC253 has larger line widths by factors of ~2-3. The $σ^2/R$ dependency on column density shows that, in the GC, on scales of 10-100 pc the kinematics of gas over $N>3\times10^{21}$ cm$^{-2}$ are compatible with gravitationally bound structures. In NGC253 this is only the case for column densities $N>3\times10^{22}$ cm$^{-2}$. The increased line widths in NGC253 originate in the lower column density gas. This high-velocity dispersion, not gravitationally self-bound gas is likely in transient structures created by the combination of high average densities and feedback in the starburst. The high densities turns the gas molecular throughout the volume of the starburst, and the injection of energy and momentum by feedback significantly increases the velocity dispersion at a given spatial scale over what is observed in the GC.
