HOPS 108: Star-formation triggered by a non-thermal jet?
A. K. Díaz Rodríguez, M. Osorio, G. Anglada, S. T. Megeath, L. F. Rodríguez, J. J. Tobin, E. Furlan, J. F. Gómez, A. M. Stutz, W. Fischer, P. Manoj, B. González… 展开作者
A. K. Díaz Rodríguez, M. Osorio, G. Anglada, S. T. Megeath, L. F. Rodríguez, J. J. Tobin, E. Furlan, J. F. Gómez, A. M. Stutz, W. Fischer, P. Manoj, B. González-García, T. Stanke, J. Booker, B. Ali
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Proceedings of the Star Formation in Different Environments, ICISE, Quy Nhon, Vietnam, 2016, (eds. D. Johnstone, T. Hoang, F. Nakamura, Q. Nguyen-Luong, and J. T. Tranh Van)
The nature of the far-IR source HOPS 108 has been a matter of debate in the last years. Previous radio observations detected a 3.6 cm source (VLA 12), coincident with HOPS 108, that was interpreted as a radio jet from this protostar. We present new multi-wavelength (0.7-5 cm), multi-configuration VLA observations as well as archive data (3.6 cm) that reveal VLA 12 as three knots of non-thermal emission, with HOPS 108 close to the central knot. We show that these knots have not been ejected by HOPS 108. We propose that the VLA 12 knots are actually part of a radio jet driven by VLA 11 (HOPS 370), a strong nearby source clearly elongated in the direction of the knots. The position of HOPS 108 in the path of the VLA 11-VLA 12 jet suggests an appealing new scenario: the triggered formation of HOPS 108 by the interaction of the jet with the surrounding medium.
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars IV. Unveiling the Embedded Intermediate-Mass Protostar and Disk within OMC2-FIR3/HOPS-370
Complex AGN feedback in the Teacup galaxy. A powerful ionised galactic outflow, jet-ISM interaction, and evidence for AGN-triggered star formation in a giant bubble
The Structure and Kinematics of Three Class 0 Protostellar Jets from JWST
Ritter Astrophysical Research Center, Dept. of Physics and Astronomy, University of Toledo（托莱多大学物理与天文学系里特天文研究中心）；INAF-Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；Jet Propulsion Laboratory, California Institute of Technology（加州理工学院喷气推进实验室）；Tata Institute of Fundamental Research（塔塔基础研究所）；Department of Astronomy, The University of Texas at Austin（德克萨斯大学奥斯汀分校天文学系）；Dipartimento di Fisica, Università degli Studi di Milano（米兰大学物理系）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Departamento de Astronomía, Universidad de Concepción（康塞普西翁大学天文学系）
Cold gas formation triggered by active galactic nuclei jet feedback in galaxy cluster cores
Università di Bologna（博洛尼亚大学）；INAF - Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（意大利国家天体物理研究所博洛尼亚天文与空间科学观测站）；University of Hertfordshire（赫特福德大学）；University of Cambridge（剑桥大学）；Istituto di Radio Astronomia, INAF（意大利国家天体物理研究所射电天文研究所）；University of California Observatories/Lick Observatory（加州大学天文台/利克天文台）
The double signature of local cosmic-ray acceleration in star-forming regions
近年来，人们对原恒星表面或沿原恒星喷流的激波产生低能宇宙射线（< 1 TeV）的研究越来越感兴趣。这些局部加速的CR提供了一个有吸引力的解释，高水平的非热发射和电离率，$ζ$，观察接近这些来源。在一些原恒星源中观察到的高$ζ$通常归因于激波产生的紫外光子。本文的目的是表明，当在同一空间区域测量同步辐射和高$ζ$时，局部冲击加速的CR通量足以解释这两种现象。假设相对论粒子按一阶费米加速机制加速，计算了$ζ$和厘米波段的非热辐射。然后，我们将我们的模型应用到恒星形成区域OMC-2 FIR 3/FIR 4。使用贝叶斯分析，我们约束模型的参数和估计的光谱指数的非热无线电发射。我们证明，本地CR加速模型，使它有可能同时解释同步辐射沿HOPS 370喷流在FIR 3区域和$ζ$附近观察到的FIR 4原星团。我们的模型约束的磁场强度（~250-450 $~μ$ G），其湍流分量（~20-40 $~μ$ G），并为HOPS 370喷流（~350-1000 km s $^{-1}$）的三个非热源的冲击参考系中的喷流速度。除了OMC-2 FIR 3/FIR 4系统的建模，我们展示了如何在厘米波长和分子跃迁的连续观测的组合是一个强大的新工具，用于分析恒星形成区域：这两种类型的观测可以同时解释调用只存在局部加速CR，而不必诉诸冲击产生的UV光子。
The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars I. Identifying and Characterizing the Protostellar Content of the OMC2-FIR4 and OMC2-FIR3 Regions
