Sequential Star Formation in RCW 34: A Spectroscopic Census of the Stellar Content of High-mass Star-forming Regions
A. Bik, E. Puga, L. B. F. M. Waters, M. Horrobin, Th. Henning, T. Vasyunina, H. Beuther, H. Linz, L. Kaper, M. van den Ancker, A. Lenorzer, E. Churchwell, S. Ku… 展开作者
A. Bik, E. Puga, L. B. F. M. Waters, M. Horrobin, Th. Henning, T. Vasyunina, H. Beuther, H. Linz, L. Kaper, M. van den Ancker, A. Lenorzer, E. Churchwell, S. Kurtz, M. B. N. Kouwenhoven, A. Stolte, A. de Koter, W-. F. Thi, F. Comeron, Ch. Waelkens
We present VLT/SINFONI integral field spectroscopy of RCW 34 along with Spitzer/IRAC photometry of the surroundings. RCW 34 consists of three different regions. A large bubble has been detected on the IRAC images in which a cluster of intermediate- and low-mass class II objects is found. At the northern edge of this bubble, an HII region is located, ionized by 3 OB stars. Intermediate mass stars (2 - 3 Msun) are detected of G- and K- spectral type. These stars are still in the pre-main sequence (PMS) phase. North of the HII region, a photon-dominated region is present, marking the edge of a dense molecular cloud traced by H2 emission. Several class 0/I objects are associated with this cloud, indicating that star formation is still taking place. The distance to RCW 34 is revised to 2.5 +- 0.2 kpc and an age estimate of 2 - 1 Myrs is derived from the properties of the PMS stars inside the HII region. The most likely scenario for the formation of the three regions is that star formation propagates from South to North. First the bubble is formed, produced by intermediate- and low-mass stars only, after that, the HII region is formed from a dense core at the edge of the molecular cloud, resulting in the expansion as a champagne flow. More recently, star formation occurred in the rest of the molecular cloud. Two different formation scenarios are possible: (a) The bubble with the cluster of low- and intermediate mass stars triggered the formation of the O star at the edge of the molecular cloud which in turn induces the current star-formation in the molecular cloud. (b) An external triggering is responsible for the star-formation propagating from South to North. [abridged]
MOLLId: software for automatic identification of spectral molecular lines in the sub-millimeter and millimeter bands and its application to the spectra of protostars from the region RCW 120
Institute of Astronomy, Russian Academy of Sciences（俄罗斯科学院天文研究所）；Ural Federal University named after the first President of Russia B. N. Yeltsin（叶利钦乌拉尔联邦大学）
Substellar population of the young massive cluster RCW 36 in Vela
Universidade de Lisboa（里斯本大学）；Université de Bordeaux（波尔多大学）；Institut universitaire de France (IUF)（法国高等教育研究院）；NSF NOIRLab/Vera C. Rubin Observatory（美国国家科学基金会NOIRLab/维拉·C·鲁宾天文台）；Istituto Nazionale di Astrofisica (INAF) – Osservatorio Astronomico di Palermo（意大利国家天体物理研究所巴勒莫天文台）；European Southern Observatory（欧洲南方天文台）；University of St Andrews（圣安德鲁斯大学）；Stockholm University（斯德哥尔摩大学）；American Museum of Natural History（美国自然历史博物馆）；Universidad Diego Portales（迭戈·波特莱斯大学）；Millennium Nucleus on Young Exoplanets and their Moons (YEMS)（年轻系外行星及其卫星千年核心）；Canada-France-Hawaii Telescope Corporation（加拿大-法国-夏威夷望远镜公司）；Instituto de Astrofísica de Andalucía (CSIC)（安达卢西亚天体物理研究所）
该研究通过分析 RCW 36 星团的 IMF 和恒星-褐矮星比值，揭示了其亚恒星群体的分布特征及可能的原始质子分离现象。
JWST Spectroscopic Census of ALMA Faint Submillimeter Galaxies in the Hubble Ultra Deep Field
The Graduate University for Advanced Studies, SOKENDAI（日本高级研究院）；National Astronomical Observatory of Japan（日本国立天文台）；Institute for Cosmic Ray Research, The University of Tokyo（东京大学宇宙射线研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo（东京大学 Kavli 宇宙物理数学研究所）；David A. Dunlap Department of Astronomy and Astrophysics, University of Toronto（多伦多大学大卫·邓普天文学与天体物理学系）；Dunlap Institute for Astronomy and Astrophysics（邓普天文学与天体物理学研究所）
The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release II: dynamical and stellar population properties of z ~< 1 galaxies in the COSMOS field
A SPectroscopic survey of biased halos In the Reionization Era (ASPIRE): Spectroscopically Complete Census of Obscured Cosmic Star Formation Rate Density at $z=4-6$
Investigating the Observational Progenitor Mass Gap in the White Dwarf Initial-Final Mass Relation. I. Cluster Census and Characterization of the First White Dwarfs in the Gap
University of British Columbia（不列颠哥伦比亚大学）；University of Warwick（华威大学）
Skyfire: A Spectroscopic Census of Little Red Dots and Broad-Line AGN in the CEERS Field
Colby College（科尔比学院）；The University of Texas at Austin（德克萨斯大学奥斯汀分校）；Cosmic Frontier Center, The University of Texas at Austin（宇宙前沿中心，德克萨斯大学奥斯汀分校）；Kavli Institute for the Physics and Mathematics of the Universe (Kavli IPMU, WPI), The University of Tokyo（东京大学宇宙物理与数学研究所（Kavli IPMU，WPI））；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）；University of the Pacific（太平洋大学）；Peking University（北京大学）；Astrophysics Science Division, NASA Goddard Space Flight Center（美国宇航局戈达德太空飞行中心天体物理学部）；University of Connecticut（康涅狄格大学）；Space Telescope Science Institute（空间望远镜科学研究所）
Search for associations containing young stars (SACY) VIII. An updated census of spectroscopic binary systems showing hints of non-universal multiplicity among these associations
A Chemodynamical Census of the Milky Way's Ultra-Faint Compact Satellites. I. A First Population-Level Look at the Internal Kinematics and Metallicities of 19 Extremely-Low-Mass Halo Stellar Systems
Yale University（耶鲁大学）；University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics（邓普勒天文学与天体物理学研究所）；University of Virginia（弗吉尼亚大学）；Carnegie Institution for Science（卡内基科学机构）；University of Chicago（芝加哥大学）；Kavli Institute for Cosmological Physics（卡弗里宇宙物理学研究所）；Fermi National Accelerator Laboratory（费米国家加速器实验室）
The R136 star cluster dissected with Hubble Space Telescope/STIS. I. Far-ultraviolet spectroscopic census and the origin of HeII 1640 in young star clusters
A Census of Compact Elliptical Galaxies in the Coma Cluster
Faculty of Space Research, M.V. Lomonosov Moscow State University（莫斯科国立大学空间研究学院）；Sternberg Astronomical Institute, M.V. Lomonosov Moscow State University（莫斯科国立大学斯登伯格天文研究所）；Universite Paris Cite, CNRS, Astroparticule et Cosmologie（巴黎 Cité 大学，法国国家科学研究中心，粒子与宇宙学）
A rotation-based census of blue lurker candidates in open clusters
Charles University（查理大学）；National Central University（中央大学）；Università di Firenze（佛罗伦萨大学）；INAF – Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切里天文台）
Medium-band Astrophysics with the Grism of NIRCam In Frontier fields (MAGNIF): Spectroscopic Census of H$α$ Luminosity Functions and Cosmic Star Formation at $z\sim 4.5$ and 6.3
Cosmic Pairs: A DESI Census of Dual and Offset AGN as Precursors to Massive Black Hole Binaries
Carnegie Mellon University（卡内基梅隆大学）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）；Institute for Advanced Study, Princeton（普林斯顿高等研究院）；Institute of Space Sciences, ICE-CSIC（空间科学研究所，西班牙国家科学研究委员会）；Institut d’Estudis Espacials de Catalunya (IEEC)（加泰罗尼亚太空研究学院）；Lawrence Berkeley National Laboratory（劳伦斯伯克利国家实验室）；Boston University（波士顿大学）
该研究基于 DESI DR1 光谱数据，构建了超大样本双与偏移 AGN，结合 ASTRID 模拟揭示其演化特征，为 LISA 可探测的大质量黑洞并合提供了前身星系群样本。
A Comprehensive JWST/NIRSpec Census of Broad-line Active Galactic Nuclei: Faint, Low-mass Accretors and a Population of Little Red Dots
New York University（纽约大学）；Menlo School（门洛学校）；Center for Interdisciplinary Exploration & Research in Astrophysics (CIERA)（天体物理跨学科探索与研究中心）；Northwestern University（西北大学）
An (in)complete NIRSpec census of Balmer absorption in Type 1 AGN -- radiation-driven outflows in little red dots, quasars and variable stars
University of Cambridge（剑桥大学）；Kavli Institute for Cosmology, University of Cambridge（剑桥大学卡弗里宇宙学研究所）；Cavendish Laboratory, University of Cambridge（剑桥大学卡文迪许实验室）；University College London（伦敦大学学院）
$χ^{1}$ Fornacis cluster DANCe. Census of stars, structure, and kinematics of the cluster with Gaia-EDR3
内容：$χ^{1}$天炉座星团（Alessi 13）是太阳附近为数不多的几个年龄和距离的疏散星团之一，应该得到更多的关注，因为它可以作为未来许多与恒星和行星形成有关的研究的基石。目的：我们利用盖亚太空任务第三次数据发布的早期安装，结合档案数据和我们自己的观察，扩大集群成员的普查，并重新审视集群的一些属性。研究方法：我们应用概率的方法来推断成员的概率超过1000度${^2}$的字段选择最有可能的集群成员，并得出的距离，空间速度和物理性质的恒星在这个样本。结果：我们确定了164个高概率的集群成员（包括61个新成员），涵盖了5.1至19.6等的G带星等范围。我们的集群成员的样本是完整的0.04 M $_{\odot}$。我们从贝叶斯推断中推导出了$108.4\pm0.3$ pc的距离，并证实了该星团与杜鹃座-时钟座、天鸽座和船底座年轻恒星协同运动。我们调查的运动学的集群从一个子样本的恒星测量径向速度，我们没有发现任何显着的膨胀或旋转的集群的影响。我们的研究结果表明，集群是有点年轻（约30万年）比以前认为的。基于光谱观测，我们认为，集群是质量分离和光谱类型的分布相比，其他年轻的恒星群显示出很小的变化。结论：在这项研究中，我们提供了最完整的集群成员普查，可以单独使用盖亚数据完成，我们使用这个新的样本来提供集群6D结构的更新图片。
