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arXiv 2103.04965astro-ph.GA
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IRDC核心G34 .43+00.24 MM1中的多个分子流出和断裂

Multiple molecular outflows and fragmentation in the IRDC core G34.43+00.24 MM1

N. L. Isequilla, M. E. Ortega, M. B. Areal, S. Paron

备注：
Accepted in A&A. March 8, 2021
发表信息：
A&A 649, A139 (2021)
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摘要：

导致大质量恒星形成的分子云的碎裂发生在不同空间尺度的层次上。巨大的分子云中隐藏着巨大的分子团，其中嵌有巨大的核心。这些核心的碎裂可能决定了初始质量函数和最终恒星的质量。因此，研究核心的碎裂过程对于了解大质量恒星的形成至关重要。位于IRDC G34.34+00.24中的热分子核G34-MM 1位于3.6kpc处，是研究碎裂和外流过程的一个很有前途的目标。使用从阿塔卡马大型毫米波阵列（ALMA）数据库中获得的93和334 GHz的数据，我们非常详细地研究了G34-MM 1。在334 GHz的数据的角分辨率使我们能够解决约0.014 pc（$\sim$ 2900 au）的结构。我们发现了在两个不同的空间尺度上向分子热核G34-MM 1分裂的证据。尘埃凝结物MM 1-A（约0.06 pc大小）含有三个分子亚核候选者（SC 1至SC 3），在$^{12}$ CO J=3-2的排放中检测到，典型的大小约为0.02 pc。从HCO $^+$ J=1-0发射，我们确定，具有更好的角分辨率比以前的观察，两个垂直的分子流出产生的MM 1-A。我们认为，子核心SC 1和SC2，嵌入在MM 1-A，海港的主要和次要的分子外流，分别负责的来源。最后，从334 GHz的无线电连续辐射中，我们勉强检测到另一个尘埃凝结，名为MM 1-E，从中产生一个年轻，大规模和充满活力的分子外流。热分子核心G34-MM 1在两个不同空间尺度上的碎裂，以及与之相关的多个分子外流的存在，将支持竞争性吸积的情景。

英文摘要：

The fragmentation of a molecular cloud that leads to the formation of high-mass stars occurs on a hierarchy of different spatial scales. The large molecular clouds harbour massive molecular clumps with massive cores embedded in them. The fragmentation of these cores may determine the initial mass function and the masses of the final stars. Therefore, studying the fragmentation processes in the cores is crucial to understand how massive stars form. The hot molecular core G34-MM1, embedded in IRDC G34.34+00.24 located at a distance of 3.6 kpc, is a promising object to study both the fragmentation and outflow processes. Using data at 93 and 334 GHz obtained from the Atacama Large Millimeter Array (ALMA) database we studied G34-MM1 with great detail. The angular resolution of the data at 334 GHz allowed us to resolve structures of about 0.014 pc ($\sim$2900 au). We found evidence of fragmentation towards the molecular hot core G34-MM1 at two different spatial scales. The dust condensation MM1-A (about 0.06 pc in size) harbours three molecular subcores candidates (SC1 through SC3) detected in $^{12}$CO J=3-2 emission, with typical sizes of about 0.02 pc. From the HCO$^+$ J=1-0 emission, we identify, with better angular resolution than previous observations, two perpendicular molecular outflows arising from MM1-A. We suggest that subcores SC1 and SC2, embedded in MM1-A, harbour the sources responsible of the main and the secondary molecular outflow, respectively. Finally, from the radio continuum emission at 334 GHz, we marginally detected another dust condensation, named MM1-E, from which a young, massive, and energetic molecular outflow arises. The fragmentation of the hot molecular core G34-MM1 at two different spatial scales, together with the presence of multiple molecular outflows associated with it, would support a competitive accretion scenario.

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