ATLASGAL – evolutionary trends in high-mass star formation
ATLASGAL – evolutionary trends in high-mass star formation
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ATLASGAL — 高质量恒星形成的演化趋势
DOI：
10.1093/mnras/stab3511
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发表时间：
2022
影响因子：
4.8
通讯作者：
Yang, A Y
中科院分区：
文献类型：
--
作者：
Urquhart, J S;Wells, M R;Pillai, T;Leurini, S;Giannetti, A;Moore, T J;Thompson, M A;Figura, C;Colombo, D;Yang, A Y
ATLASGAL是一个870微米的尘埃测量，测量范围为银河系内平面的420 ° 2，已被用来识别10000个致密的分子团。专门的后续观测和补充调查被用来描述这些团块的物理特性，绘制银河系分布图，并调查高质量星星形成的演化序列。ATLASGAL数据的分析正在进行中：我们提供了最新版本的目录。我们已经将5007块分为四个演化阶段（静止，原恒星，年轻的恒星物体和Hiiregions），并发现在每个阶段相似数量的块，这表明类似的寿命。亮度质量比（Lbol/Mfwhm）曲线显示了一个平滑的分布，没有显着的扭结或不连续的演化阶段的平均值相比，表明星星的形成过程是连续的，观测阶段并不代表根本不同的阶段或变化的物理机制。我们比较进化的样本与其他星星形成示踪剂（甲醇和水脉泽，扩展绿色对象和分子流出），并发现与这些增加的关联率作为进化阶段的函数，证实我们的分类是可靠的。这也揭示了静止源和分子流出之间的高关联率，揭示了流出是星星形成已经开始的最早迹象，并且星星形成已经在许多即使在70 µm处也很暗的团块中进行。
ATLASGAL is an 870-µm dust survey of 420 deg2the inner Galactic plane and has been used to identify ∼10 000 dense molecular clumps. Dedicated follow-up observations and complementary surveys are used to characterize the physical properties of these clumps, map their Galactic distribution, and investigate the evolutionary sequence for high-mass star formation. The analysis of the ATLASGAL data is ongoing: We present an up-to-date version of the catalogue. We have classified 5007 clumps into four evolutionary stages (quiescent, protostellar, young stellar objects and Hiiregions) and find similar numbers of clumps in each stage, suggesting a similar lifetime. The luminosity-to-mass (Lbol/Mfwhm) ratio curve shows a smooth distribution with no significant kinks or discontinuities when compared to the mean values for evolutionary stages indicating that the star formation process is continuous and that the observational stages do not represent fundamentally different stages or changes in the physical mechanisms involved. We compare the evolutionary sample with other star formation tracers (methanol and water masers, extended green objects and molecular outflows) and find that the association rates with these increases as a function of evolutionary stage, confirming that our classification is reliable. This also reveals a high association rate between quiescent sources and molecular outflows, revealing that outflows are the earliest indication that star formation has begun and that star formation is already ongoing in many of the clumps that are dark even at 70 µm.