Galactic Cold Cores. VIII. Filament formation and evolution: Filament properties in context with evolutionary models
A. Rivera-Ingraham, I. Ristorcelli, M. Juvela, J. Montillaud, A. Men'shchikov, J. Malinen, V. -M. Pelkonen, A. Marston, P. G. Martin, L. Pagani, R. Paladini, D.… 展开作者
A. Rivera-Ingraham, I. Ristorcelli, M. Juvela, J. Montillaud, A. Men'shchikov, J. Malinen, V. -M. Pelkonen, A. Marston, P. G. Martin, L. Pagani, R. Paladini, D. Paradis, N. Ysard, D. Ward-Thompson, J. -P. Bernard, D. J. Marshall, L. Montier, L. V. Toth
Filaments are key for star formation models. As part of the study carried out by the Herschel GCC Programme, here we study the filament properties presented in GCC.VII in context with theoretical models of filament formation and evolution. A conservative sample of filaments at a distance D<500pc was extracted with the Getfilaments algorithm. Their physical structure was quantified according to two main components: the central (Gaussian) region (core component), and the power-law like region dominating the filament column density profile at larger radii (wing component). The properties and behaviour of these components relative to the total linear mass density of the filament and its environmental column density were compared with theoretical models describing the evolution of filaments under gravity-dominated conditions. The feasibility of a transition to supercritical state by accretion is dependent on the combined effect of filament intrinsic properties and environmental conditions. Reasonably self-gravitating (high Mline-core) filaments in dense environments (av\sim3mag) can become supercritical in timescales of t\sim1Myr by accreting mass at constant or decreasing width. The trend of increasing Mline-tot (Mline-core and Mline-wing), and ridge Av with background also indicates that the precursors of star-forming filaments evolve coevally with their environment. The simultaneous increase of environment and filament Av explains the association between dense environments and high Mline-core values, and argues against filaments remaining in constant single-pressure equilibrium states. The simultaneous growth of filament and background in locations with efficient mass assembly, predicted in numerical models of collapsing clouds, presents a suitable scenario for the fulfillment of the combined filament mass-environment criterium that is in quantitative agreement with Herschel observations.
Virgo Filaments VIII: Characterizing the Structural Parameters of Virgo Galaxies with Machine Learning to Probe Environmental Quenching
University of Kansas（堪萨斯大学）；Siena University（锡耶纳大学）；Union College（联合学院）；INAF- Osservatorio astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Steward Observatory, University of Arizona（亚利桑那大学斯图尔德天文台）；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体物理学与空间科学观测站）；Observatoire de Paris, LUX, Collège de France, CNRS, PSL University, Sorbonne University（巴黎天文台，法国学院，法国国家科学研究中心，巴黎文理研究大学，索邦大学）；INAF – Osservatorio Astronomico di Trieste（意大利国家天体物理研究所的里雅斯特天文台）；Dipartimento di Fisica G. Occhialini, Università degli Studi di Milano-Bicocca（米兰比可卡大学G. Occhialini物理系）；Laboratoire d’Astrophysique, École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院天体物理实验室）
Filamentary Fragmentation and Accretion in High-Mass Star-Forming Molecular Clouds
丝状结构在大质量恒星形成分子云中无处不在。它们与高质量恒星形成的关系仍有待了解。在这里，我们报告对8个连续的高质量恒星形成云的干涉观测。在这些云中总共发现了50个致密的核心，其中大多数都是高质量恒星形成的标志。其中五颗没有任何恒星形成的迹象，因此是星前核心的候选者。这些核心的演化阶段和它们的线宽，温度，NH $_3$丰度，维里参数被发现是相关的。在一个子样本的4形态定义良好的细丝，我们发现，它们的碎片不能单独解释的热或湍流压力的支持。我们还研究了沿暗条的气体温度和非热运动的分布，并发现了非热线宽和恒星形成活动之间的空间相关性。我们发现沿这些细丝的气体流动的证据，并推导出沿细丝的$\sim$ 10 $^{-4}$ M $_\odot$ yr $^{-1}$的吸积率。这些结果表明大质量暗条和大质量恒星形成之间存在着密切的关系，通过i）在非常早期的演化阶段的惯性碎裂形成致密的核心，ii）沿着暗条的吸积流对致密核心和原恒星的生长非常重要，iii）在恒星形成过程中通过反馈或吸积增强暗条中的非热运动。
Linear filament and nested cluster evolution tomography (LANCET) I. Capture the evolution of dense gas in 14-parsec filament G316.8
Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学科维理天文与天体物理研究所）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；I. Physikalisches Institut, Universität zu Köln（科隆大学第一物理研究所）；Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México（墨西哥国立自治大学无线电天文学与天体物理研究所）；SRON Netherlands Institute for Space Research & Kapteyn Astronomical Institute, University of Groningen（荷兰空间研究研究所与格罗宁根大学卡普坦天文学研究所）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Department of Astronomy, University of Virginia（弗吉尼亚大学天文学系）；Department of Space, Earth & Environment, Chalmers University of Technology（查尔姆斯理工大学空间、地球与环境系）；Department of Physics, National Sun Yat-Sen University（国立中山大学物理系）；Center of Astronomy and Gravitation, National Taiwan Normal University（国立台湾师范大学天文与引力研究中心）
Chemical study of two starless cores in the B213/L1495 filament
Centro de Astrobiología (CSIC-INTA)（天体生物学中心）；European Space Agency (ESA)（欧洲航天局）；European Space Astronomy Centre (ESAC)（欧洲航天天文中心）；Observatorio Astronómico Nacional (OAN)（国家天文台）；Observatorio de Yebes (IGN)（耶韦斯天文台）；Instituto de Astrofísica de Canarias (IAC)（加那利群岛天体物理研究所）；Departamento de Astrofísica, Universidad de La Laguna（拉帕尔马大学天体物理学系）
Evolution of magnetized hub-filament systems: Comparing the observed properties of W3(OH), W3 Main, and S 106
Institute for Advanced Study, Kyushu University（九州大学高等研究院）；Department of Earth and Planetary Sciences, Faculty of Science, Kyushu University（九州大学理学部地球行星科学系）；Division of Science, National Astronomical Observatory of Japan（日本国立天文台科学部）；Department of Physics, Graduate School of Science, Nagoya University（名古屋大学大学院理学研究科物理学专业）；Institute of Liberal Arts and Sciences Tokushima University（德岛大学文理学院）；Kavli Institute for Astronomy and Astrophysics, Peking University（北京大学柯夫利天体物理研究所）
本文通过比较 W3(OH)、W3 Main 和 S 106 三个不同演化阶段的磁化枢纽-纤维系统，结合 JCMT/POL-2 偏振观测与档案数据，揭示了纤维线质量函数、偏振分数和磁场-纤维排列随演化变化的规律，并发现枢纽尺寸与年轻星团半径相似及“双节点”恒星形成的普遍性。
The dense cores and filamentary structure of the molecular cloud in Corona Australis. Herschel SPIRE and PACS observations from the Herschel Gould Belt Survey
An Ammonia Spectral Map of the L1495-B218 Filaments in the Taurus Molecular Cloud: II CCS & HC$_7$N Chemistry and Three Modes of Star Formation in the Filaments
Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions
Korea Astronomy and Space Science Institute（韩国天文学与空间科学研究所）；National Astronomical Observatory of Japan（日本国立天文台）；Center for Computational Astrophysics, National Astronomical Observatory of Japan（日本国立天文台计算天体物理中心）；Astronomical Science Program, The Graduate University for Advanced Studies (SOKENDAI)（高级研究院（SOKENDAI）天文学科学项目）；Department of Physics, Konan University（神户学院大学物理系）
Observations of DNC and DCO$^+$ toward the $\int$-shaped Filament and Starless Cores in the Orion Molecular Clouds
Nobeyama Radio Observatory, National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台野边山无线电观测站，国立自然科学研究所）；SOKENDAI (The Graduate University for Advanced Studies)（综合研究大学院大学）；Department of Physics, Graduate School of Science, Osaka Metropolitan University（大阪公立大学理学研究科物理学系）；Star and Planet Formation Laboratory, RIKEN（理化学研究所星与行星形成实验室）；Graduate School of Informatics and Engineering, The University of Electro-Communications（电波大学信息工学与研究科）；Faculty of Education, Kagawa University（香川大学教育学部）；Department of Earth and Planetary Sciences, Faculty of Science, Kyushu University（九州大学理学部地球惑星科学系）
