论文标题
阿尔玛揭示的，以银河系形成区域的内部结构的演变
The evolution of the internal structure of massive star forming regions in the Milky Way as revealed by ALMA
论文作者
论文摘要
我们使用ALMA-IMF大型计划中的1.3美元的连续排放图分析了银河系的15个原始组形成区域的结构。云结构的分析是使用Delta-Ariancians频谱技术进行的。计算出的光谱在小尺度上显示了一个自相似的制度，以及在较大尺度上存在突出的颠簸，其物理尺寸$ l _ {\ rm Hub} $，范围为$ \ 7000 $ au至$ 60000 $ au。这些量表对应于原始群集形成云中最紧凑的团块的尺寸。在$ l _ {\ rm集线器} $和根据H41 $α$重组线$ \ weft（σ_{\ rmH41α}^{\ rm rm rm rm rm rm rmm free-free-free and and and use and and Incortation）$ rym and and y and and Incortion n之间的$ lmm and and Incortion n之间的$ lmmime and and and and and and y n of and and and（n q rim and）集线器} $以及1.3毫米与3毫米连续发射通量的比率$ \ left（s _ {\ rm 1.3 mm}^{\ rm cloud}/s _ {\ rm 3 mm}^{\ rm 3 mm}^{\ rm cloud} \ right）$。 $ \左的较小值（s _ {\ rm 1.3 mm}^{\ rm cloud}/s _ {\ rm 3 mm}^{\ rm cloud} \ right）$和$σ_{\ rmH41α}^{\ rmh41α}^{\ rm free-free-free-free free free verund的$ qut clumpers的$ clumplunce clunce clunce clunce complation compers的$ clunces complations in因此，我们的结果表明，云中最密集的区域的大小直接链接到它们的进化阶段，以及其恒星形成活性，而更具进化的云层具有更大的原始簇形成团块。这表明重力在调节这些团块的大小和质量生长以及恒星形成活动中起着至关重要的作用
We analyze the structure of 15 protocluster forming regions in the Milky Way using their $1.3$ mm continuum emission maps from the ALMA-IMF large program. The analysis of the clouds structure is performed using the delta-variance spectrum technique. The calculated spectra display a self-similar regime on small scales as well as the presence of a prominent bump on larger scales and whose physical size, $L_{\rm hub}$, falls in the range of $\approx 7000$ au to $60000$ au. These scales correspond to the sizes of the most compact clumps within the protocluster forming clouds. A significant correlation is found between $L_{\rm hub}$ and the surface density of the free-free emission estimated from the integrated flux of the H41$α$ recombination line $\left(Σ_{\rm H41α}^{\rm free-free}\right)$ as well as a significant anti-correlation between $L_{\rm hub}$ and the ratio of the 1.3 mm to 3 mm continuum emission fluxes $\left(S_{\rm 1.3 mm}^{\rm cloud}/S_{\rm 3 mm}^{\rm cloud}\right)$. Smaller values of $\left(S_{\rm 1.3 mm}^{\rm cloud}/S_{\rm 3 mm}^{\rm cloud}\right)$ and larger values of $Σ_{\rm H41α}^{\rm free-free}$ correspond to more advanced evolutionary stages of the protocluster forming clumps. Hence, our results suggest that the sizes of the densest regions in the clouds are directly linked to their evolutionary stage and to their star formation activity with more evolved clouds having larger protocluster forming clumps. This is an indication that gravity plays a vital role in regulating the size and mass growth and star formation activity of these clumps with ongoing gas accretion
