The bar pattern speed of the LMC has been measured using Gaia data, suggesting the presence of a slow pattern, perhaps not rotating at all. Numerical simulations of interacting LMC-SMC systems were able to reproduce a bar stoppage. Here, we report on the first measurement of the bar pattern speed of the LMC as a function of the evolutionary phase of its stellar populations. Astrometric and photometric data of 11 million LMC stars from Gaia DR3 were used to build five evolutionary phases, from less to more evolved stars. The Dehnen method, a new procedure to derive bar pattern speeds from kinematics of particles in N-body simulations, is applied to the LMC stellar populations. We observe a modulation of the bar pattern speed with the evolutionary phase, meaning that different LMC stellar populations exhibit different pattern speeds, ranging from -0.9 to 6.6 km/s/kpc. Moreover, less evolved stars have a lower pattern speed while the bar of more evolved phases tends to rotate faster. The LMC bar is thus extremely slow, ruling out the presence of bar corotation within the disc, in agreement with a previous claim, but this time observed with various stellar populations. It is the first time that a pattern speed is measured separately for different stellar populations in any galaxy. The LMC pattern speed cannot be simply resumed to a singular value, but instead is an overlay of different patterns depending on the evolutionary phase of the stars. Future Gaia releases will be crucial to investigate more deeply the relations of the pattern speed with important astrophysical parameters of stars, like their age and metallicity, which will be helpful to constrain the chemo-dynamical evolution of the LMC bar.
Down-the-barrel and transverse observations of the Large Magellanic Cloud: evidence for a symmetrical galactic wind on the near and far sides of the galaxy
A comprehensive kinematic model of the LMC disk from star clusters and field stars using Gaia DR3: Tracing the disk characteristics, rotation, bar, and the outliers
Disentangling the Morphology of Palomar~5: Effects of the Bar, Spiral Arms, LMC, and Halo Flattening
School of Physics and Astronomy, Sun Yat-sen University（中山大学物理学院）；CSST Science Center for the Guangdong-Hong Kong-Macau Greater Bay Area（中国空间站科学中心粤港澳大湾区分中心）；School of Astronomy and Space Science, University of Chinese Academy of Sciences（中国科学院大学天文与空间科学学院）；National Astronomical Observatories, Chinese Academy of Sciences（中国科学院国家天文台）；University of Surrey（萨里大学）
MAGellanic Outflow and chemistry Survey (MAGOS): Hot cores in the LMC
Institute of Science and Technology, Niigata University（新潟大学科学技术研究院）；Institute of Science Tokyo（东京科学研究所）；School of Physics and Astronomy, Shanghai Jiao Tong University（上海交通大学物理与天文学院）；State Key Laboratory of Dark Matter Physics（暗物质物理全国重点实验室）；Key Laboratory for Particle Astrophysics and Cosmology (MOE)（粒子天体物理与宇宙学教育部重点实验室）；Shanghai Key Laboratory for Particle Physics and Cosmology（上海粒子物理与宇宙学重点实验室）；RIKEN Pioneering Research Institute（理化学研究所前沿研究中心）
Kinematic analysis of the Large Magellanic Cloud using Gaia DR3
内容：盖亚任务的高质量数据允许以前所未有的细节研究大麦云（LMC）的内部运动学，提供对其盘的非轴对称结构的见解。目的：定义和验证一种改进的选择策略，以区分LMC恒星从银河系前景。为了检查可能的偏差，假设的参数或来自银河系的样品污染可以引入在使用盖亚数据的LMC的内部运动学分析。方法：我们的选择是基于监督神经网络分类器，使用尽可能多的Gaia DR 3数据。我们选择了三个具有不同完整性和纯度的候选LMC恒星样本;我们使用不同的测试样本对其进行验证，并将其与盖亚合作论文样本进行比较。我们分析由此产生的速度分布和地图，我们检查这些结果如何变化时，也使用视线速度，可用于恒星的一个子集。结果如下：银河系恒星样本中的污染基本上影响了大麦哲伦星系外围的结果，而视线速度的缺乏不会使内盘运动学的结果产生偏差。对于第一次，我们进行了运动学分析的LMC使用样本与全三维速度信息从盖亚DR 3。结论：内盘的动力学主要是棒控制的，旋臂超密度的运动学似乎是由向内的运动和旋臂中与棒相连的部分的自转速度控制的，MW星的污染似乎控制着盘的外部，主要影响旧的演化阶段;在某些情况下，LMC的假设盘形态参数和视线速度的不确定性可能具有显著的影响。[删节]
Kinematic Signatures in the Stellar Halo from Cosmological Encounters between the Milky Way and its Clouds
University of Pennsylvania（宾夕法尼亚大学）；Institute for Astronomy, University of Hawai‘i（夏威夷大学天体物理研究所）；University of Washington（华盛顿大学）；Boston University（波士顿大学）；Carnegie Observatories（卡内基观测站）；California Institute of Technology（加州理工学院）
Hubble Space Telescope proper motions of Large Magellanic Cloud star clusters -- II. Kinematic structure of young and intermediate-age clusters
Leibniz-Institut für Astrophysik Potsdam（波茨坦阿佩尔天体物理研究所）；INAF – Osservatorio di Astrofisica e Scienza dello Spazio di Bologna（博洛尼亚天文物理学与空间科学国家研究院）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；IKERBASQUE, Basque Foundation for Science（伊克尔巴斯基克科学基金会）；Space Telescope Science Institute（太空望远镜科学研究所）；atlanTTic, Universidade de Vigo, Escola de Enxeñaría de Telecomunicación（维戈大学电信工程学院阿特兰提克）；Universidad de La Laguna（拉帕鲁纳大学）；INAF – Osservatorio Astronomico d’ Abruzzo（阿布鲁佐天文台国家研究院）；INFN – Sezione di Pisa, Universitá di Pisa（比萨大学意大利国家核物理研究所比萨分部）；Department of Physics, University of Surrey（萨里大学物理系）；INAF - Osservatorio Astronomico di Padova（帕多瓦天文台国家研究院）
The star formation history of the Magellanic Clouds derived from long-period variable star counts
首次利用长周期变星重建了大麦哲伦云和小麦哲伦云的恒星形成历史。这些冷演化的恒星在近红外波段达到最高光度，因此它们的K波段星等可以用来推算它们的出生质量和年龄，从而得到SFH。在大麦哲伦星云，我们发现了一个10光年的单恒星形成时期，其速率为$\sim1.5$ M $_\odot$/年$^{-1}$，随后是全球范围内相对连续的SFR $\sim0.2$ M $_\odot$/年$^{-1}$。在LMC的核心（LMC条），可以看到一个次级的、明显的事件，从3 Gyr前开始，持续到$\sim0.5$ Gyr前。在SMC中，可以看到两个形成时期，一个是以$\sim0.28$ M $_\odot$ yr $^{-1}$的速率的$\sim6$ Gyr ago，另一个是以$\sim0.3$ M $_\odot$ yr $^{-1}$的速率的仅$\sim0.7$ Gyr ago。后者在大麦哲伦星云中也是可辨别的，因此可能与麦哲伦星云和/或银河系之间的相互作用有关，而大麦哲伦星云棒的形成可能是一个无关的事件。恒星形成活动现在集中在麦哲伦云的中心部分，如果动力学弛豫引起的恒星迁移有效的话，可能一直都是如此。不同的初始形成时期表明，LMC和SMC没有形成为一对，但至少SMC形成孤立的。
METAL: The Metal Evolution, Transport, and Abundance in the Large Magellanic Cloud Hubble program. II. Variations of interstellar depletions and dust-to-gas ratio within the LMC
