ALMA Central Molecular Zone Exploration Survey (ACES) I: Overview
Steven N. Longmore, John Bally, Ashley T. Barnes, Cara Battersby, Laura Colzi, Adam Ginsburg, Jonathan D. Henshaw, Paul T. P. Ho, Izaskun Jiménez-Serra, J. M. D… 展开作者
Steven N. Longmore, John Bally, Ashley T. Barnes, Cara Battersby, Laura Colzi, Adam Ginsburg, Jonathan D. Henshaw, Paul T. P. Ho, Izaskun Jiménez-Serra, J. M. Diederik Kruijssen, Elisabeth A. C. Mills, Maya A. Petkova, Mattia C. Sormani, Robin G. Tress, Daniel L. Walker, Jennifer Wallace, Emad Alkhuja, Lucia Armillotta, Nazar Budaiev, Rojita Buddhacharya, Alyssa Bulatek, Michael Burton, Natalie O. Butterfield, Laura A. Busch, Paola Caselli, Mélanie Chevance, Claire Cook, Samuel Crowe, Ana Karla Díaz-Rodríguez, Enrico DiTeodoro, Simon R. Dicker, Katarzyna M. Dutkowska, Adam Fairley, Christoph Federrath, Rubén Fedriani, Zi-Xuan Feng, Karl Fiteni, Gary Fuller, Pablo García, Javier Goicoechea, Philipp Girichidis, Simon C. O. Glover, Mark Gorski, Savannah R. Gramze, Qi-Lao Gu, H. Perry Hatchfield, Christian Henkel, Rebecca J. Houghton, Pei-Ying Hsieh, Yue Hu, Katharina Immer, Desmond Jeff, Janik Karoly, Jens Kauffmann, Ralf S. Klessen, Mark R. Krumholz, Alex Lazarian, Emily M. Levesque, Fu-Heng Liang, Dani Lipman, Xunchuan Liu, Xing Lu, Qiu-yi Luo, Alessandro Lupi, Laura McCafferty, S. Martín, Farideh Mazoochi, Mark R. Morris, Marie Nonhebel, Francisco Nogueras-Lara, Tomoharu Oka, Juergen Ott, Marco Padovani, Xing Pan, Jaime E. Pineda, Thushara G. S. Pillai, Marc W. Pound, Miguel Requena Torres, Denise Riquelme-Vásquez, Víctor M. Rivilla, Galaxy Salo, Álvaro Sánchez-Monge, Miriam G. Santa-Maria, Rainer Schoedel, Anika Schmiedeke, Matthias Schultheis, Howard A. Smith, Yoshiaki Sofue, Leonardo Testi, Grant R. Tremblay, Arianna Vasini, Gijs Vermariën, Alexey Vikhlinin, Serena Viti, Q. Daniel Wang, Fengwei Xu, Suinan Zhang, Qizhou Zhang
The mass flows and energy cycles within the inner regions of galaxies exert a powerful influence on the evolution of the galaxy population. The centre of the Milky Way is the only galactic nucleus for which it is possible to resolve the physical mechanisms that drive these cycles, namely star formation and feedback, while also tracing global (>100 pc) processes which determine where and when star formation and feedback occur. We present an overview of ACES, the 'Atacama Large Millimeter/submillimeter Array (ALMA) CMZ Exploration Survey', a ~1.5" angular resolution, 0.2-3 km/s spectral resolution ALMA Band 3 (85-102 GHz), survey of the 'Central Molecular Zone' (CMZ) -- the inner-100 pc of the Galaxy (l = 359.4 deg to 0.8 deg). ACES spectral setup is tuned to observe optimal tracers of the physical, chemical, and kinematic conditions in over 70 spectral features (e.g. HCO+, HNCO, SiO, H40alpha, complex molecules) of the gas in the CMZ, to derive the properties of all potentially star-forming Galactic Centre gas, from global scales (100 pc) to dense ~0.05 pc structures that are expected to host individual star-forming cores, down to sub-sonic (<0.4 km/s) velocity resolution. In this overview paper, we provide the scientific justification for the ACES survey, explain the choice of observational setup, and describe the data legacy products. Finally, we show some of the initial ACES data which highlight the power of ACES' combination of high angular resolution, unprecedented spatial dynamic range, sensitivity, spectral resolution and spectral bandwidth as an illustration of how ACES aims to understand how global processes set the location, intensity, and timescales for star formation and feedback in the CMZ.
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
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）
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）
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）
Complex Organic Molecules in Protostars with ALMA Spectral Surveys (COMPASS): I. Overview of the ALMA Large Program
Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse（图卢兹大学天体物理与行星学研究所以）；Physikalisch-Meteorologisches Observatorium Davos und Weltstrahlungszentrum (PMOD/WRC)（达沃斯物理气象观测站和世界辐射中心）；Department of Chemistry, Biochemistry and Pharmaceutical Sciences (DCBP), Universität Bern（伯尔尼大学化学、生物化学和药学系）；Department of Physics and Astronomy, Seoul National University（首尔大学物理与天文学系）；National Radio Astronomy Observatory（美国国家射电天文台）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学）；Max-Planck-Institut für Radioastronomie（马克斯·普朗克射电天文研究所）；Institute of Astronomy, Department of Physics, National Tsinghua University（国立清华大学物理系天文学研究所）；Department of Astronomy, University of Virginia（弗吉尼亚大学天文学系）；Purdue University（普渡大学）；Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Scienc（孔科利天文台，匈牙利研究与教育网络天文学与地球科学研究中心）
FRagmentation and Evolution of dense cores Judged by ALMA (FREJA). I (Overview). Inner $\sim$1000 au structures of prestellar/protostellar cores in Taurus
VAPOLA -- A multi-year, multi-band polarization survey of AGN and Sgr A* at mm wavelengths with ALMA I. Survey Overview and Science-Ready Archival Products
Università degli Studi di Cagliari（卡利亚里大学）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；University of Balearic Islands（巴利阿里群岛大学）；Institute of the Balearic Islands (IAIB)（巴利阿里群岛研究所）；Health Research Institute of the Balearic Islands (IdISBa)（巴利阿里群岛健康研究所）；Universidade São Paulo, Instituto de Astronomia, Geofísica e Ciéencias Atmosféricas（圣保罗大学天文、地球物理与大气科学研究所）；INAF-Istituto di Radioastronomia（意大利国家天体物理研究所射电天文学研究所）；INAF–Italian Centre for Astronomical Archive（意大利天体物理研究所意大利天文档案中心）
ALMA Chemical Evolution (ACE) survey: an overview -- extending dust and gas inference to low metallicities at cosmic noon
Centro de Astrobiología (CAB), CSIC-INTA（西班牙太空生物研究中心）；European Southern Observatory（欧洲南方天文台）；Leiden Observatory, Leiden University（莱顿大学莱顿天文台）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Department of Physics, University of California, Santa Barbara（加州大学圣塔芭芭拉分校物理系）；Cosmic Dawn Center at the Niels Bohr Institute, University of Copenhagen and DTU-Space, Technical University of Denmark（哥本哈根大学尼尔斯·玻尔学院宇宙黎明中心及丹麦技术大学DTU空间）；Université Paris-Saclay, Université Paris Cité, CEA, CNRS, AIM（巴黎萨克雷大学、巴黎西岱大学、法国原子能和替代能源委员会、法国国家科学研究中心）；Research School of Astronomy and Astrophysics, Australian National University（澳大利亚国立大学天体物理学研究学院）；Department of Physics and Astronomy（物理与天文学系）
The ALMA survey to Resolve exoKuiper belt Substructures (ARKS) IV: CO gas imaging and overview
Universidad de Santiago, Chile（圣地亚哥大学）；Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan（东京大学理学研究科天文学系）；Institute of Physics and Astronomy, ELTE Eötvös Loránd University, Pázmány Péter sétány 1/A, 1117 Budapest, Hungary（厄特沃什·罗兰大学物理与天文学研究所）；Max-Planck-Insitut für Astronomie, Königstuhl 17, 69117 Heidelberg, Germany（马克斯·普朗克天文研究所）；Department of Physics & Astronomy, University of Victoria, 3800 Finnerty Rd, Victoria, BC V8P 5C2, Canada（维多利亚大学物理与天文学系）；Joint ALMA Observatory, Avenida Alonso de Córdova 3107, Vitacura 7630355, Santiago, Chile（ALMA联合天文台）；Departamento de Astrofísica, Universidad de La Laguna, La Laguna, E-38200, Teneri（拉帕尔马大学天体物理学系）
How much gas and dust is in the $z=5.7$ Lyman Break Galaxy HZ10? An ALMA Band 10 to 4 and JWST/NIRSpec study of its interstellar medium
Academia Sinica（中央研究院）；Universidad de Concepción（康塞普西翁大学）；Millennium Institute for Galaxies (MINGAL)（银河系千年研究所）；Universidad Diego Portales（迭戈·波特莱斯大学）；Chalmers University of Technology（查尔姆斯理工大学）；University of Maryland, College Park（马里兰大学帕克分校）；Leiden University（莱顿大学）；University of Western Australia（西澳大学）；University of Toronto（多伦多大学）；Ghent University（根特大学）；Foundation for Research and Technology Hellas (FORTH)（希腊研究与技术基金会）；European University Cyprus（塞浦路斯欧洲大学）；Caltech/IPAC（加州理工学院/IPAC）；Scuola Normale Superiore（比萨高等师范学院）；Space Telescope Science Institute（太空望远镜科学研究所）；SOKENDAI (The Graduate University for Advanced Studies)（综合研究大学院大学）；National Astronomical Observatory of Japan（日本国立天文台）；Hiroshima University（广岛大学）；University of Cambridge（剑桥大学）；National Radio Astronomy Observatory（美国国家无线电天文台）；Universidad de Granada（格拉纳达大学）；INAF – Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Flatiron Institute（平托研究所）；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台）；University of Sussex（萨塞克斯大学）
Nonthermal Pressures: Key to Energy Balance and Structure Formation Near Sgr A* in the Milky Way
Institute for Research in Fundamental Sciences (IPM), School of Astronomy（伊朗基础科学研究所天文学院）；Chinese Academy of Sciences South America Center for Astronomy, National Astronomical Observatories, CAS（中国科学院南美天文中心，国家天文台）；Institute for Advanced Study（高等研究院）；Astrophysics Research Institute, Liverpool John Moores University（利物浦约翰摩尔斯大学天体物理研究所）；Cosmic Origins Of Life (COOL) Research DAO（宇宙生命起源（COOL）研究去中心化自治组织）；Department of Astronomy, University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校天文学系）；Department of Physics, Aberystwyth University（阿伯里斯特威斯大学物理系）；Shanghai Astronomical Observatory, Chinese Academy of Sciences（上海天文台，中国科学院）
Stellar feedback in M83 as observed with MUSE -- I. Overview, an unprecedented view of the stellar and gas kinematics and evidence of outflowing gas
我们提出了一个大的VLT/MUSE马赛克（3.8 × 3.8千秒差距）附近的旋涡星系M83，空间分辨率约20秒差距。我们得到了恒星和电离气体的运动学，并与ALMA CO（2-1）的分子气体运动学进行了比较。我们将电离气体分为HII区和扩散电离气体（DIG），并确定了来自DIG的Ha光度分数（f_DIG）。我们观察到，恒星和气体跟踪银河系盘旋转，以及快速旋转的核组件，可能连接到长期的过程驱动的银河酒吧。在气体运动学中，我们观察到原子核以东的气流，相对于圆盘发生了红移。该流被一个扩展的电离气体区域所包围，该电离气体区域具有增强的速度分散和高电离状态，这在很大程度上与被慢冲击电离一致。我们解释这一功能的叠加盘和平面外层的DIG，或作为一个酒吧驱动的冲击气体流入。一个双高斯分量拟合的Ha线也揭示了存在一个核的双锥结构，其对称轴是垂直于酒吧。这两个锥沿着视线出现蓝移和红移，并突出具有Ha发射，其与盘的分离高达200 km s-1，以及高速色散~80-200 km s-1。在锥体的远端，我们观察到气体与被冲击电离一致。这些特征以前从未在M83中观察到过;我们假设它们是在追踪一个恒星暴驱动的外流，冲击周围的ISM。最后，我们在我们的视野中获得f_DIG ~ 13%。我们检查发射的HII地区和DIG的“BPT”图，发现在HII地区的光电离占99.8%的哈通量，而DIG有混合贡献的光电离（94.9%…
Accurate dust temperature and star formation rate in the most luminous $z>6$ quasar in the HYPerluminous quasars at the Epoch of ReionizatION (HYPERION) sample
本文通过ALMA Band 9高频观测精确测定z>6最亮类星体J0100+2802的尘埃温度、质量和恒星形成率，揭示其超大质量黑洞在黑洞-星系增长中占主导地位。
