To investigate star formation and assembly processes of massive galaxies, we present here a spatially-resolved stellar populations analysis of a sample of 45 elliptical galaxies (Es) selected from the CALIFA survey. We find rather flat age and [Mg/Fe] radial gradients, weakly dependent on the effective velocity dispersion of the galaxy within half-light radius. However, our analysis shows that metallicity gradients become steeper with increasing galaxy velocity dispersion. In addition, we have homogeneously compared the stellar populations gradients of our sample of Es to a sample of nearby relic galaxies, i.e., local remnants of the high-z population of red nuggets. This comparison indicates that, first, the cores of present-day massive galaxies were likely formed in gas-rich, rapid star formation events at high redshift (z>2). This led to radial metallicity variations steeper than observed in the local Universe, and positive [Mg/Fe] gradients. Second, our analysis also suggests that a later sequence of minor dry mergers, populating the outskirts of early-type galaxies (ETGs), flattened the pristine [Mg/Fe] and metallicity gradients. Finally, we find a tight age-[Mg/Fe] relation, supporting that the duration of the star formation is the main driver of the [Mg/Fe] enhancement in massive ETGs. However, the star formation time-scale alone is not able to fully explain our [Mg/Fe] measurements. Interestingly, our results match the expected effect that a variable stellar initial mass function would have on the [Mg/Fe] ratio.
The spatially-resolved effect of mergers on the stellar mass assembly of MaNGA galaxies
Universidad de la Laguna（拉古纳大学）；SCIPP, University of California, Santa Cruz（加州大学圣克鲁兹分校 SCIPP）；Mila—Quebec Artificial Intelligence Institute（米拉魁北克人工智能研究所）；Center for Computational Astrophysics, Flatiron Institute（平顿研究所计算天体物理学中心）；Department of Astrophysics, University of Vienna（维也纳大学天体物理系）
Spatially resolved Halpha maps and sizes of 57 strongly star-forming galaxies at z~1 from 3D-HST: evidence for rapid inside-out assembly of disk galaxies
RIOJA. A Clumpy Galaxy Assembly at Redshift 6.81 Revealed by JWST
Waseda University（早稻田大学）；University of Tsukuba（筑波大学）；Flatiron Institute（平顿研究所）；The University of Tokyo（东京大学）；Nagoya University（名古屋大学）；Kyoto University（京都大学）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), UT Institute for Advanced Study, The University of Tokyo（东京大学宇宙起源研究核心（WPI）/ 基础宇宙物理学宇宙论前沿中心）；Chalmers University of Technology（查尔姆斯理工大学）；National Astronomical Observatory of Japan（日本国立天文台）；Chiba University（千叶大学）；Space Telescope Science Institute (STScI)（太空望远镜科学研究所）；Graduate University for Advanced Studies (SOKENDAI)（综合研究大学院大学）
KiDS J1447-0149: The first spatially resolved spectroscopy of a relic galaxy beyond the local universe. An old high-dispersion core embedded in a compact rotating stellar structure
Finnish Centre for Astronomy with ESO, (FINCA), University of Turku（图尔库大学芬兰ESO天文学中心）；Tuorla Observatory, Department of Physics and Astronomy, University of Turku（图尔库大学图奥拉天文台）；Turku Collegium for Science, Medicine and Technology (TCSMT), University of Turku（图尔库大学图尔库科学、医学与技术学院）；European Southern Observatory（欧洲南方天文台）；Sub-Department of Astrophysics, Department of Physics, University of Oxford（牛津大学物理系天体物理子部门）；INAF – Osservatorio Astronomico di Capodimonte（意大利国家天体物理研究所卡波迪蒙特天文台）；INAF – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Instituto de Astrofísica de Canarias（加那利群岛天体物理研究所）
Spatially Resolved Stellar Populations of $0.3<z<6.0$ Galaxies in WHL0137-08 and MACS0647+70 Clusters as Revealed by JWST: How do Galaxies Grow and Quench Over Cosmic Time?
The MAGPI survey: Stellar population radial trends and mass assembly in star-forming galaxies at z~0.3
University of Vienna（维也纳大学）；Universidade do Porto（波尔图大学）；Instituto de Astrofísica e Ciências do Espaço, Universidade do Porto（波尔图大学空间与天体物理研究所）；University of Strasbourg（斯特拉斯堡大学）；SISSA- International School for Advanced Studies（国际高等研究院）；UWC- University of the Western Cape（西开普大学）；IFPU- Institute for Fundamental Physics of the Universe（宇宙基础物理研究所）；INFN-Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Durham University（杜伦大学）
Galaxy And Mass Assembly (GAMA): the signatures of galaxy interactions as viewed from small scale galaxy clustering
星系-星系相互作用的统计研究经常利用祖先物理性质的净变化作为其核之间的分离的函数来追踪其相互作用的强度和可观察的时间尺度。在这项研究中，我们使用两点自动，交叉和标记关联函数调查在何种程度上的小尺度成团性质的恒星形成的星系可以用来获得物理洞察星系星系之间的相互作用的相似的光学亮度和恒星质量。从高度空间完整的星系和质量组装（GAMA）调查中得出的Halalpha恒星形成者显示，在小的分离上集群增加。此外，成团强度与光学亮度和恒星质量有很强的相关性，其中（1）在给定的距离下，光学较亮的星系成团幅度大于光学较暗的星系，（2）小尺度成团特性（例如强度，恒星形成星系的信号相对于基准幂律平台（fiducial power law plateaus）的尺度似乎随着星系光学亮度的增加而不同。根据交叉和标记相关分析，前一个结果在很大程度上是由光学明亮的恒星形成星系中增加的尘埃含量驱动的。后者可以被解释为相互作用尺度和星系光学亮度之间的相关性的证据，其中光学明亮的恒星形成者之间的相互作用的物理证据，可能托管在相对大质量的晕中，比光学暗淡的恒星形成者之间的分离更大。
MAGAZ3NE: Spatially Resolved Ages and Chemical Abundances of Ultra-Massive Quiescent Galaxies at z $\sim$ 3.5 using JWST/NIRSpec IFU
York University（约克大学）；University of Toronto（多伦多大学）；Dunlap Institute for Astronomy & Astrophysics, University of Toronto（多伦多大学邓普勒天文学与天体物理研究所）；University of Massachusetts, Amherst（马萨诸塞大学阿默斯特分校）；University of California Davis（加州大学戴维斯分校）；University of Wisconsin-Madison（威斯康星大学麦迪逊分校）；Observatories of the Carnegie Institution for Science（卡内基科学机构天文台）；Princeton University（普林斯顿大学）
Spatially resolved star formation history of Sextans dSph
Instituto Interdisciplinario de Ciencias Básicas (ICB), CONICET-UNCuyo（基础科学跨研究所 (ICB)，CONICET-UNCuyo）；Consejo Nacional de Investigaciones Científicas y Técnicas (CONICET)（国家科学研究委员会 (CONICET)）
Disentangling the assembly of the central and diffuse stellar components in galaxy clusters through dynamical friction and tidal stripping
University of Nottingham（诺丁汉大学）；École Polytechnique Fédérale de Lausanne (EPFL)（洛桑联邦理工学院）；Universidad de La Laguna（拉帕尔马大学）；Instituto de Astrofísica de Canarias（加那利天体物理研究所）；Universidad Autónoma de Madrid（马德里自治大学）
Pre-perihelion Emergence of the CN Gas Coma in 3I/ATLAS Temporally and Spatially Resolved by the 7-Dimensional Telescope
Institute for Astronomy, University of Hawai‘i（夏威夷大学天体物理研究所）；Astronomy Program, Department of Physics and Astronomy, Seoul National University（首尔大学物理与天文学系天文项目）；SNU Astronomy Research Center, Seoul National University（首尔大学天文研究中心）；Korea Astronomy and Space Science Institute (KASI)（韩国天体宇宙科学研究所）
