ALMA-IMF VI -- Investigating the origin of stellar masses: Core mass function evolution in the W43-MM2&MM3 mini-starburst
Y. Pouteau, F. Motte, T. Nony, M. Gonzalez, I. Joncour, J. -F. Robitaille, G. Busquet, R. Galvan-Madrid, A. Gusdorf, P. Hennebelle, A. Ginsburg, T. Csengeri, P.… 展开作者
Y. Pouteau, F. Motte, T. Nony, M. Gonzalez, I. Joncour, J. -F. Robitaille, G. Busquet, R. Galvan-Madrid, A. Gusdorf, P. Hennebelle, A. Ginsburg, T. Csengeri, P. Sanhueza, P. Dell'Ova, A. M. Stutz, A. P. M. Towner, N. Cunningham, F. Louvet, A. Men'shchikov, M. Fernandez-Lopez, N. Schneider, M. Armante, J. Bally, T. Baug, M. Bonfand, S. Bontemps, L. Bronfman, N. Brouillet, D. Diaz-Gonzalez, F. Herpin, B. Lefloch, H. -L. Liu, X. Lu, F. Nakamura, Q. Nguyen Luong, F. Olguin, K. Tatematsu, M. Valeille-Manet
备注：
Accepted for publication in A&A (december, 5th 2022) after language editing; 25 pages, 14 figures
关于恒星初始质量函数（IMF），最核心的未决问题之一是环境如何影响核质量函数（CMF）的形状，并由此可能影响 IMF。ALMA-IMF 大型计划旨在研究核分布随云团特征的变化，将其作为云团形成过程和演化的诊断观测量。本研究聚焦于 W43-MM2&MM3 迷你星暴；最近发现，其 CMF 相对于 Salpeter 斜率呈顶重型。W43-MM2&MM3 拥有一个富星团，其中包含在统计上数量显著的核；此前 Paper III 已对其进行了表征。我们将多尺度分解技术应用于 ALMA 1.3 mm 和 3 mm 连续谱图像，以划定六个子区域。对于每个子区域，我们利用 1.3 mm 图像表征了高柱密度概率分布函数（n-PDF）以及云气体的形态。利用核目录，我们研究了 CMF 与云团性质及核性质之间的相关性。根据核的面数密度、外流数量以及 UCHii 的存在情况，我们将这些子区域划分为从宁静到星暴再到星暴后的不同演化阶段。各子区域 CMF 的大质量端从接近 Salpeter 斜率（宁静期）变化为顶重型（星暴期和星暴后）。此外，n-PDF 的第二尾部从陡峭变化为平坦，正如在大质量恒星形成云中观测到的那样。我们发现，具有平坦第二 n-PDF 尾部的子区域表现出顶重型 CMF。在从宁静阶段到星暴阶段的恒星形成过程中，CMF 可能从 Salpeter 型演化为顶重型。这一情景引出了一个问题：随着云团接近其恒星形成阶段的终点，CMF 是否可能再次恢复为 Salpeter 型；该假说仍有待检验。
英文摘要：
Among the most central open questions regarding the initial mass function (IMF) of stars is the impact of environment on the shape of the core mass function (CMF) and thus potentially on the IMF. The ALMA-IMF Large Program aims to investigate the variations in the core distributions with cloud characteristics, as diagnostic observables of the formation process and evolution of clouds. The present study focuses on the W43-MM2&MM3 mini-starburst, whose CMF has recently been found to be top-heavy with respect to the Salpeter slope. W43-MM2&MM3 harbors a rich cluster that contains a statistically significant number of cores, which was previously characterized in Paper III. We applied a multi-scale decomposition technique to the ALMA 1.3 mm and 3 mm continuum images to define six subregions. For each subregion we characterized the high column density probability distribution function, n-PDF, and the shape of the cloud gas using the 1.3 mm image. Using the core catalog, we investigate correlations between the CMF and cloud and core properties. We classify the subregions into different stages of evolution, from quiescent to burst to post-burst, based on the surface number density of cores, number of outflows, and UCHii presence. The high-mass end of the subregion CMFs varies from being close to the Salpeter slope (quiescent) to top-heavy (burst and post-burst). Moreover, the second tail of the n-PDF varies from steep, to flat like observed for the high mass star-forming clouds. We found that subregions with flat second n-PDF tails display top-heavy CMFs. The CMF may evolve from Salpeter to top-heavy throughout the star formation process from the quiescent to the burst phase. This scenario raises the question of if the CMF might revert again to Salpeter as the cloud approaches the end of its star formation stage, a hypothesis that remains to be tested.
ALMA-IMF XXII. Role of core subfragmentation in the IMF origin: Hierarchical fragmentation cascade and CMF in W43-MM1
Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；LPC2E, CNRS, Univ. Orléans（奥尔良大学）；Laboratoire d’astrophysique de Bordeaux, Univ. Bordeaux, CNRS（波尔多大学）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Laboratoire de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris（巴黎文理研究大学）；Observatoire de Paris, PSL University, Sorbonne Université, LUX（巴黎天文台）；Departamento de Astronomía, Universidad de Concepción（孔多西比托大学）
The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). XIII. Core Mass Function, Lifetime, and Growth of Prestellar Cores
The University of Tokyo（东京大学）；National Astronomical Observatory of Japan, National Institutes of Natural Sciences（日本国立天文台，国立自然科学研究院）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，IPAG）；Max Planck Institute for Astronomy（马克斯·普朗克天体物理研究所）；Kyoto University（京都大学）；Xiamen University（厦门大学）；Chalmers University of Technology（查尔姆斯理工大学）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Chinese Academy of Sciences（中国科学院）
ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- IV. Radio Recombination Lines and evolution of star formation efficiencies
Rotation and stability of the circumnuclear gas disk in the Galactic Center potential by the ALMA CMZ Exploration Survey (ACES)
Institute of Astronomy, The University of Tokyo（东京大学天文研究所）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔大学天体物理研究所）；CCosmic Origins Of Life (COOL)（宇宙生命起源研究（COOL））；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Center for Astrophysics and Space Astronomy（科罗拉多大学博尔德分校天体物理与行星科学系空间天体物理研究中心）；Department of Astrophysical and Planetary Sciences（欧洲南方天文台）；University of Colorado, Boulder（康涅狄格大学物理系）；European Southern Observatory (ESO)（西班牙国家航空航天技术研究所/西班牙高等科学研究委员会天体生物学中心）；Department of Physics, University of Connecticut；Centro de Astrobiología (CAB), CSIC-INTA
The Nature of High ${\rm [OIII]}_{\rm 88μm}$/${\rm [CII]}_{\rm 158μm}$ Galaxies in the Epoch of Reionization: Low Carbon Abundance and a Top-Heavy IMF?
Automated Mining of the ALMA Archive in the COSMOS Field (A3COSMOS): I. Robust ALMA Continuum Photometry Catalogs and Stellar Mass and Star Formation Properties for ~700 Galaxies at z=0.5-6
Low-Metallicity Star Formation Survey in Sh2-284 (LZ-STAR): The Core Mass Function
National Astronomical Observatory of Japan（日本国立天文台）；University of Virginia（弗吉尼亚大学）；Chalmers University of Technology（查尔姆斯理工大学）；European Southern Observatory（欧洲南方天文台）；Instituto de Astrofísica de Andalucía, CSIC（安达卢西亚天体物理研究所，西班牙高等科学研究委员会）；Institute of Science Tokyo（东京科学大学）；Shanghai Jiao Tong University（上海交通大学）
The Stellar Initial Mass Function down to 0.16M$_{\odot}$ Towards the Small Magellanic Cloud
Rutgers the State University of New Jersey（新泽西州立罗格斯大学）；Eureka Scientific Inc.（尤里卡科学公司）；Space Telescope Science Institute（太空望远镜科学研究所）；Johns Hopkins University（约翰斯·霍普金斯大学）；INAF Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；ASI-Space Science Data Center（意大利空间局空间数据中心）；Center for Astrophysics, Harvard & Smithsonian（哈佛-史密森尼天体物理中心）
A pilot method to determine the high mass end of the Stellar Initial Mass Function in galaxies using UVIT, H$α$-MUSE observations and applied to NGC628
