机构地区：[1]Kavli Institute for Astronomy and Astrophysics,Peking University,Beijing 100871,China [2]Department of Astronomy,School of Physics,Peking University,Beijing 100871,China [3]Shanghai Astronomical Observatory,Chinese Academy of Sciences,Shanghai 200030,China [4]Chinese Academy of Sciences South America Center for Astronomy,National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [5]Departamento de Astronomía,Universidad de Chile,Las Condes,7591245 Santiago,Chile [6]Jet Propulsion Laboratory,California Institute of Technology,4800 Oak Grove Drive,Pasadena CA 91109,USA [7]Center for Astrophysics|Harvard&Smithsonian,60 Garden Street,Cambridge,MA 02138,USA [8]National Astronomical Observatory of Japan,National Institutes of Natural Sciences,2-21-1 Osawa,Mitaka,Tokyo 181-8588,Japan [9]Astronomical Science Program,The Graduate University for Advanced Studies,SOKENDAI,2-21-1 Osawa,Mitaka,Tokyo 181-8588,Japan [10]School of Physics and Astronomy,Yunnan University,Kunming 650091,China [11]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [12]Department of Physics,University of Helsinki,PO Box 64,FI-00014 Helsinki,Finland [13]Indian Institute of Space Science and Technology,Thiruvananthapuram 695547,Kerala,India [14]Max Planck Institute for Astronomy,Königstuhl 17,D-69117 Heidelberg,Germany [15]Department of Astronomy,Graduate School of Science,The University of Tokyo,7-3-1 Hongo,Bunkyo-ku,Tokyo 113-0033,Japan [16]Max-Planck-Institut für Radioastronomie,Auf dem Hügel 69,53121 Bonn,Germany [17]Departamento de AstronomÂıa,Universidad de Concepcion,Casilla 160-C,Concepci on,Chile [18]Department of Astronomy,The University of Texas at Austin,Texas 78712-1205,USA [19]Korea Astronomy and Space Science Institute,776 Daedeokdae-ro,Yuseong-gu,Daejeon 34055,Republic of Korea [20]Institute of Astronomy and Astrophysics,Academia Sinica,Roosevelt Road,Taipei 10617,Taiwan,China [21]South-Western Institute for Astronomy Research,Yunnan University,Kunming 650091,China [22]Korea Astrono
出 处：《Research in Astronomy and Astrophysics》2024年第6期119-139,共21页天文和天体物理学研究（英文版）
基 金：upported by the National Natural Science Foundation of China(NSFC,Grant No.12033005);the National Key R&D Program of China(No.2022YFA1603102);the China Manned Space Project(CMS-CSST-2021-A09,CMS-CSST-2021-B06);the China-Chile Joint Research Fund(CCJRF No.2211);support from the Tianchi Talent Program of Xinjiang Uygur Autonomous Region。
摘 要：Leveraging the high resolution,sensitivity,and wide frequency coverage of the Atacama Large Millimeter/submillimeter Array(ALMA),the QUARKS survey,standing for“Querying Underlying mechanisms of massive star formation with ALMA-Resolved gas Kinematics and Structures”,is observing 139 massive starforming clumps at ALMA Band 6(λ~1.3 mm).This paper introduces the Atacama Compact Array(ACA)7 m data of the QUARKS survey,describing the ACA observations and data reduction.Combining multiwavelength data,we provide the first edition of QUARKS atlas,offering insights into the multiscale and multiphase interstellar medium in high-mass star formation.The ACA 1.3 mm catalog includes 207 continuum sources that are called ACA sources.Their gas kinetic temperatures are estimated using three formaldehyde transitions with a non-LTE radiation transfer model,and the mass and density are derived from a dust emission model.The ACA sources are massive(16–84 percentile values of 6–160 M_(⊙)),gravity-dominated(M∝R^(1.1))fragments within massive clumps,with supersonic turbulence(M>1)and embedded star-forming protoclusters.We find a linear correlation between the masses of the fragments and the massive clumps,with a ratio of 6%between the two.When considering fragments as representative of dense gas,the ratio indicates a dense gas fraction(DGF)of 6%,although with a wide scatter ranging from 1%to 10%.If we consider the QUARKS massive clumps to be what is observed at various scales,then the size-independent DGF indicates a self-similar fragmentation or collapsing mode in protocluster formation.With the ACA data over four orders of magnitude of luminosity-to-mass ratio(L/M),we find that the DGF increases significantly with L/M,which indicates clump evolutionary stage.We observed a limited fragmentation at the subclump scale,which can be explained by a dynamic global collapse process.
关 键 词：stars:formation ISM:kinematics and dynamics ISM:clouds stars:protostars
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