ALMA Central molecular zone Exploration Survey (ACES) VI: ALMA Large Program Reveals a Highly Filamentary Central Molecular Zone
Cara Battersby, Miriam G. Santa-Maria, Dani Lipman, Dylan M. Paré, Rachel R. Lee, Pablo García, Izaskun Jiménez-Serra, Xing Pan, Daniel L. Walker, Jack Sullivan… 展开作者
Cara Battersby, Miriam G. Santa-Maria, Dani Lipman, Dylan M. Paré, Rachel R. Lee, Pablo García, Izaskun Jiménez-Serra, Xing Pan, Daniel L. Walker, Jack Sullivan, Danya Alboslani, H Perry Hatchfield, Yue Hu, Alex Lazarian, Jennifer Wallace, Qizhou Zhang, Xing Lu, Elisabeth A. C. Mills, Adam Ginsburg, Ashley T. Barnes, Pei-Ying Hsieh, Jonathan D. Henshaw, Steven N. Longmore, John Bally, Laura Colzi, Paul T. P. Ho, Maya A. Petkova, Mattia C. Sormani, N. Bijas, Alyssa Bulatek, Natalie O. Butterfield, Christoph Federrath, Simon C. O. Glover, Mark D. Gorski, Savannah R. Gramze, Christian Henkel, Janik Karoly, Ralf S. Klessen, Sergio Martín, Francisco Nogueras-Lara, Jaime E. Pineda, Denise Riquelme-Vásquez, Víctor M. Rivilla, Álvaro Sánchez-Monge, Anika Schmiedeke, Yoshiaki Sofue, Volker Tolls
The Central Molecular Zone (CMZ) of the Milky Way is the way station that primarily controls how much gas flows from the disk of the Galaxy towards the central nucleus. While this region is well documented to have extreme gas properties that clearly distinguish it from the rest of the Galaxy, the properties of the bulk molecular gas at high angular resolution are relatively unexplored. Band 3 data from the ALMA (Atacama Large Millimeter/Submillimeter Array) large program ACES (ALMA CMZ Exploration Survey) reveal the highly filamentary nature of CMZ molecular gas at high resolution (3" or 0.1pc) across the entire CMZ. Visual inspection of these data suggests that there are at least two general classes of elongated structures, which we identify as: i) large-scale (10 pc) filamentary structures (LFs) and ii) a ubiquitous population of small-scale (about 1 pc) filamentary structures (SFs). We present detailed morphological and kinematic properties towards three structures in each category, as well as their association with magnetic fields and the correlation of HNCO 4(0,4)-3(0,3) with other molecular species. Our investigation reveals that these structures are largely coherent in position-position-velocity space. The alignment with the magnetic field structure is mixed, with some parallel, some perpendicular, and some intermediate alignments. We find that LFs likely trace pieces of contiguous CMZ orbital structures and are a manifestation of global CMZ dynamics. The second class, SFs, are pervasive and may be the result of complicated turbulence and shearing dynamics in the CMZ gas flows, as seen in numerical simulations.
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
Electron temperature and emission measure of HII regions in the central molecular zone (CMZ) from H40 αrecombination line and continuum emissions by ALMA CMZ Exploration Survey - ACES -
Institute of Astronomy, The University of Tokyo（东京大学天文学研究所）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；CCosmic Origins Of Life (COOL)（宇宙生命起源中心（COOL））；UK ALMA Regional Centre Node, Jodrell Bank Centre for Astrophysics, Oxford Road, The University of Manchester（曼彻斯特大学约德尔银行天体物理学中心英国ALMA区域中心节点）；Department of Astronomy, University of Florida（佛罗里达大学天文学系）；Max Planck Institute for Astronomy（马克斯·普朗克天体物理学研究所）；Center for Astrophysics and Space Astronomy（科罗拉多大学博尔德分校天体物理学与空间天文中心；天体物理与行星科学系）；Department of Astrophysical and Planetary Sciences；University of Colorado, Boulder
ALMA 0.1 pc View of Molecular Clouds Associated with High-Mass Protostellar Systems in the Small Magellanic Cloud: Are Low-Metallicity Clouds Filamentary or Not?
ACES: The Magnetic Field in Large Filaments in the Galactic Center
Institute for Advanced Study（高等研究院）；Chalmers University of Technology（查尔姆斯理工大学）；University of Connecticut（康涅狄格大学）；EPFL（洛桑联邦理工学院）；University College London（伦敦大学学院）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Nanjing University（南京大学）；University of Colorado, Boulder（科罗拉多大学博尔德分校）；Australian National University（澳大利亚国立大学）；Chinese Academy of Sciences South America Center for Astronomy（中国科学院南美天文中心）；National Astronomical Observatories, CAS（中国科学院国家天文台）；University of Florida（佛罗里达大学）；Liverpool John Moores University（利物浦约翰摩尔斯大学）；Max Planck Institute for Astronomy（马克斯·普朗克天文学研究所）；Academia Sinica（中央研究院）；National Astronomical Observatory of Japan（日本国立天文台）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）
SiO emission in the filamentary Infrared Dark Cloud G035.39-00.33: An ALMA view
National Astronomical Observatories of China, Chinese Academy of Sciences（中国科学院国家天文台）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；Centro de Astrobiología (CAB), CSIC-INTA（天体生物学中心（CAB），西班牙国家研究委员会-国家航空航天技术研究所）；Institute de Radioastronomie Millimétrique（毫米波射电天文研究所）；European Southern Observatory (ESO)（欧洲南方天文台）；Chalmers University of Technology（查尔姆斯理工大学）；University of Virginia（弗吉尼亚大学）；INAF Osservatorio Astronomico di Arcetri（意大利国家天体物理研究所阿切特里天文台）；Max Planck Institute for Extraterrestrial Physics（马克斯·普朗克地外物理学研究所）
ALMA Observations of Giant Molecular Clouds in M33 I: Resolving Star Formation Activities in the Giant Molecular Filaments Possibly Formed by a Spiral Shock
An ALMA view of molecular filaments in the Large Magellanic Cloud II: An early stage of high-mass star formation embedded at colliding clouds in N159W-South
ALMA Survey of Orion Planck Galactic Cold Clumps (ALMASOP): Discovery of an extremely dense and compact object embedded in the prestellar core G208.68-19.92-N2
ACES VII. Compact Continuum Source Catalog of the Central Molecular Zone
University of Connecticut（康涅狄格大学）；University of Florida（佛罗里达大学）；Instituto de Física Fundamental (CSIC)（基础物理研究所（西班牙国家科学研究委员会））；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；Green Bank Observatory（格林班克天文台）；University of Kansas（堪萨斯大学）
Probing Star-Forming Properties via ALMA Observations of Massive Protocluster IRAS 15596-5301
Kunming University of Science and Technology（昆明理工大学）；Chuxiong Normal University（楚雄师范学院）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；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）；Yunnan University（云南大学）；Anqing Normal University（安庆师范大学）；Peking University（北京大学）
ACES VIII: A Survey of Compact, High-Velocity Features Observed in CS(2-1)
University of Connecticut（康涅狄格大学）；University of Florida（佛罗里达大学）；University of Kansas（堪萨斯大学）；Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS（中国科学院国家天文台南美天体物理中心）；Instituto de Astronomía, Universidad Católica del Norte（北天主教大学天文学研究所）
A Multi-Scale Picture of Magnetic Field and Gravity from Large-Scale Filamentary Envelope to Core-Accreting Dust Lanes in the High-Mass Star-Forming Region W51
An ALMA view of molecular filaments in the Large Magellanic Cloud I: The formation of high-mass stars and pillars in the N159E-Papillon Nebula triggered by a cloud-cloud collision
The ALMA-QUARKS Survey: Discovery of Superfine Dusty Fibrils inside Massive Star-forming Clumps
Shanghai Astronomical Observatory, Chinese Academy of Sciences（中国科学院上海天文台）；University of Chinese Academy of Sciences（中国科学院大学）；Taiyuan Normal University（太原师范学院）
An ALMA study of the massive molecular clump N159W-North in the Large Magellanic Cloud: A possible gas flow penetrating one of the most massive protocluster systems in the Local Group
ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions-IX. A pilot study towards IRDC G034.43+00.24 on multi-scale structures and gas kinematics
