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astro-ph.GA

363 篇论文

K-DRIFT Science Theme: New Theoretical Framework Using the Galaxy Replacement Technique for LSB studies

本文介绍了为配合 K-DRIFT 望远镜探测低表面亮度结构而开发的星系替换技术（GRT），该技术通过在 N 体宇宙学模拟中插入高分辨率星系模型，以较低计算成本实现了极高的质量和空间分辨率，从而为理解星系形成及解释观测数据提供了新的理论框架。

Kyungwon Chun, Jihye Shin, Rory Smith, Jongwan Ko, jaewon Yoo, So-Myoung Park, Woowon Byun, Sang-Hyun Chun, Sungryong Hong, Hyowon Kim, Jae-Woo Kim, Jaehyun Lee, Hong Soo Park, Jinsu Rhee, Kwang-Il Seon, Yongmin YoonTue, 10 Ma🔭 astro-ph

Measuring the evolution of stellar bars with the host galaxy's spin

该研究结合模拟观测与 SAMI 星系巡天数据，揭示了星系自旋参数（λR\lambda_R）受恒星棒形成及取向的影响而降低，并指出弱棒星系具有更年轻的恒星种群和更高的自旋参数，表明其处于快速形成阶段，而强棒星系则处于缓慢的长期演化过程中。

Robin Joshi, Scott M. Croom, Stefania Barsanti, Elizabeth J. Iles, Joss Bland-Hawthorn, Jesse van de SandeTue, 10 Ma🔭 astro-ph

Identifying Red Supergiants in the Local Group Using JWST Photometry. I. NGC 6822, Sextans A, NGC 300, WLM, and IC 1613

该研究利用 JWST/NIRCam 的高分辨率数据，通过构建适用于贫金属环境的最优颜色 - 颜色图，成功在 NGC 6822、Sextans A、NGC 300、WLM 和 IC 1613 这五个本星系群星系中识别出大量受前景恒星污染极少的红超巨星候选体，显著完善了本星系群红超巨星的样本库。

Zhiwen Li, Ming Yang, Biwei Jiang, Yi RenTue, 10 Ma🔭 astro-ph

Pre-Virialized Assembly at Cosmic Dawn: The Dynamics and Extreme Ionization of Compact Group CGG-z7 at z∼7.04z\sim7.04

该论文利用 JWST 数据发现了红移 z∼7.04z\sim7.04 处最致密的星系群 CGG-z7，其极低的动力学质量与高恒星质量比表明它处于非平衡的“前维里化”并合阶段，且中心星系极高的电离特征暗示了被遮蔽的活动星系核的存在。

Xiaoyang Wei, Zheng Cai, Fujiang Yu, Mingyu Li, Yunjing WuTue, 10 Ma🔭 astro-ph

Ashes of FIRE: Modeling Dust Grain Size Evolution in the Local Group with FIRE

本文通过将新的离散化尘埃粒径演化模型引入 GIZMO 代码并结合 FIRE-3 反馈机制，利用理想化星系模拟揭示了 Local Group 中尘埃丰度主要由尘埃生长与破坏决定，而消光曲线斜率受凝聚作用影响，并指出模型预测的双峰粒径分布及缺乏极小碳质尘埃的现象，暗示了从预存尘埃进行“自上而下”PAH 形成的必要性。

Caleb R. Choban, Samir Salim, Dušan Kereš, Julia Roman-Duval, Karin M. SandstromTue, 10 Ma🔭 astro-ph

Spatiotemporal Properties of Compressible Magnetohydrodynamic Turbulence from Space Plasma

该研究利用 Cluster 卫星数据及新型多航天器偏振模分解技术，首次定量揭示了地球磁鞘中可压缩磁流体湍流的时空特性，证实慢模存在从弱到强的非线性转变而快模保持弱湍流状态，从而完善了跨模态、跨尺度及强弱湍流机制的可压缩湍流观测特征。

Siqi Zhao, Huirong Yan, Terry Z. Liu, Chuanpeng Hou, Ka Ho YuenTue, 10 Ma🔭 astro-ph

LeMMINGs VII: 5 GHz, 50 mas e-MERLIN observations of a statistically complete sample of nearby AGN

本文利用 e-MERLIN 在 5 GHz 频率下对邻近活动星系核（AGN）统计完备样本进行了 50 毫角秒分辨率的成像观测，揭示了低光度活动星系核主要表现为早期型星系中的致密射电喷流或核心，并表明高达 30% 的本地星系群可能拥有射电活跃核，从而凸显了高分辨率、高灵敏度成像对于探测最低光度核辐射的重要性。

D. R. A. Williams-Baldwin (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), R. D. Baldi (INAF - Istituto di Radioastronomia, Via P. Gobetti 101, I-40129 Bologna, Italy), R. J. Beswick (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), I. M. McHardy (School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK), E. Carver (School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK), J. Clifford (School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK), B. T. Dullo (Department of Physical Sciences, Embry-Riddle Aeronautical University, Daytona Beach, FL 32114, USA), N. Kill (School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK), B. Krishnamoorthi (School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK), I. M. Mutie (Department of Astronomy and Space Science, Technical University of Kenya, P.O Box 52428 - 00200, Nairobi, Kenya, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), O. Woodcock (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), M. K. Argo (Jeremiah Horrocks Institute, School of Engineering and Computing, University of Lancashire, Preston PR1 2HE, UK), P. Boorman (Cahill Center for Astrophysics, California Institute of Technology, 1216 East California Boulevard, Pasadena, CA 91125, USA), E. Brinks (Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, AL10 9AB, UK), D. M. Fenech (SKAO, Jodrell Bank, Lower Withington, Macclesfield, SK11 9FT, UK), J. H. Knapen (Instituto de Astrofísica de Canarias, Vía Láctea S/N, E-38205 La Laguna, Spain, Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Spain), S. Mathur (Astronomy Department, The Ohio State University, Columbus, OH, 43210, USA, Center for Astronomy and Astro-particle Physics, The Ohio State University, Columbus, OH 43210, USA, Eureka Scientific, 2452 DELMER ST STE 100, Oakland, CA, 94602, USA), J. Moldon (Instituto de Astrofísica de Andalucía), T. W. B. Muxlow (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), M. Pahari (Department of Physics, Indian Institute of Technology, Hyderabad 502285, India), N. H. Wrigley (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), A. Alberdi (Instituto de Astrofísica de Andalucía), W. Baan (Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi 830011, China, Netherlands Institute for Radio Astronomy), A. Beri (Indian Institute of Science Education and Research, School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK, Indian Institute of Astrophysics, Koramangala II Block, Bangalore 560034, India), X. Cheng (Korea Astronomy and Space Science Institute, 776 Daedeok-daero, Yuseong-gu, Daejeon 34055, Korea), D. A. Green (Astrophysics Group, Cavendish Laboratory, J. J. Thomson Avenue, Cambridge CB3 0HE, UK), J. Healy (United Kingdom SKA Regional Centre, Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), P. Kharb (National Centre for Radio Astrophysics), E. Körding (Department of Astrophysics/IMAPP, Radboud University, P.O. Box 9010, 6500GL Nijmegen, The Netherlands), G. Lucatelli (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK), F. Panessa (INAF - Istituto di Astrofisica e Planetologia Spaziali, via Fosso del Cavaliere 100, I-00133 Roma, Italy), M. Puig-Subirà (Instituto de Astrofísica de Andalucía), C. Romero-Cañizales (Institute of Astronomy and Astrophysics, Academia Sinica, 11F of AS/NTU Astronomy-Mathematics Building, No.1, Sec. 4, Roosevelt Rd, Taipei 106319, Taiwan), D. J. Saikia (Fakultät für Physik, Universität Bielefeld, Postfach 100131, D-33501 Bielefeld, Germany, Assam Don Bosco University, Guwahati 781017, Assam, India), P. Saikia (Center for Astro, Particle and Planetary Physics, Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA), F. Shankar (School of Physics and Astronomy, University of Southampton, Southampton, SO17 1BJ, UK), S. Sharma (Department of Physics, Indian Institute of Technology, Hyderabad 502285, India), I. R. Stevens (School of Physics and Astronomy, University of Birmingham, Edgbaston, Birmingham B15 2TT, UK), E. Varenius (Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, M13 9PL, UK)Tue, 10 Ma🔭 astro-ph

An Alternate Pathway for H2_2 Formation in the Early Universe: A physical process to account for the presence and coevolution of the luminous galaxies and supermassive black holes at the high redshifts

该论文提出了一种基于 H3+_3^+ 的 Jahn-Teller 动力学耦合的新机制，通过绕过高红移下受抑制的标准中间态直接生成基态 H2_2和 HD，从而可能解释早期宇宙中星系的过早形成及其与超大质量黑洞的协同演化。

Amrendra Pandey, Olivier Dulieu, Nadia Bouloufa-MaafaTue, 10 Ma🔬 physics.atom-ph

Disentangling the galactic and intergalactic components in 313 observed Lyman-alpha line profiles between redshift 0 and 5

该研究利用 zELDA 软件分析了 313 个莱曼阿尔法谱线，成功解耦了星系与星系际介质的贡献，发现校正后星系内禀谱线在红移 0 至 6 间演化极小，并揭示了星系际介质在红移大于 5 时对莱曼阿尔法光子可观测性的主导作用。

Siddhartha Gurung-López, Chris Byrohl, Max Gronke, Daniele Spinoso, Alberto Torralba, Alberto Fernández-Soto, Pablo Arnalte-Mur, Vicent J. MartínezThu, 12 Ma🔭 astro-ph

Broken Expectations: The Effects of Modelling Assumptions on the Inferred Dark Matter Distribution in the Milky Way's Satellites

该研究通过模拟银河系卫星星系，发现尽管潮汐力未显著影响密度分布推断，但常用的球对称 Jeans 方程分析（pyGravSphere）因模型局限倾向于低估内禀密度和 J 因子，且 Wolf 质量估计器虽总体准确但对轨道状态敏感，其结果暗示模拟星系与ΛCDM 质量 - 浓度关系的吻合可能要求银河系质量较轻或潮汐作用有限，这与潮汐扰动起源假说存在潜在张力。

Kristian Tchiorniy, Anna GeninaThu, 12 Ma🔭 astro-ph

An Ultra-Faint, Chemically Primitive Galaxy Forming in the Reionization Era

该研究利用詹姆斯·韦伯太空望远镜的引力透镜放大观测，确认了红移 z=6.625 处的超暗星系 LAP1-B 是迄今发现化学组成最原始的恒星形成星系，其极低的金属丰度、异常硬的电离辐射场及主导的暗物质晕特征，为理解早期宇宙中原始星系的形成及本地宇宙超暗矮星系的起源提供了关键证据。

Kimihiko Nakajima, Masami Ouchi, Yuichi Harikane, Eros Vanzella, Yoshiaki Ono, Yuki Isobe, Moka Nishigaki, Takuji Tsujimoto, Fumitaka Nakamura, Yi Xu, Hiroya Umeda, Yechi ZhangThu, 12 Ma🔭 astro-ph

The BoRG-JWSTJWST Survey: Analogs at z∼8z\sim8 to the UV-luminous Galaxy Population at z≳10z\gtrsim10

该研究利用 BoRG-JWSTJWST巡天发现的红移z∼8z\sim8类星体，通过光谱分析证实这些与z≳10z\gtrsim10“蓝色怪物”亮度相当的星系具有低尘埃含量且恒星形成具有随机爆发特征，从而表明z≳10z\gtrsim10的极亮星系可由年龄小于 10000 万年的年轻恒星解释。

Sofía Rojas-Ruiz, Guido Roberts-Borsani, Takahiro Morishita, Antonello Calabrò, Micaela B. Bagley, Tommaso Treu, Steven L. Finkelstein, Massimo Stiavelli, Michele Trenti, L. Y. Aaron YungThu, 12 Ma🔭 astro-ph

Before its time: a remarkably evolved protocluster core at z=7.88

该研究利用JWST观测发现，在宇宙大爆炸后仅6.5亿年（红移z=7.88）的A2744-z7p9OD原星系团核心中，已存在一个由23个星系组成、总恒星质量超过$10^{10}$太阳质量且演化程度极高的极端系统，其核心星系呈现同步的尘埃遮蔽与质量增长特征，揭示了早期宇宙中局部环境与星系形成演化的极端相互作用。

Callum Witten, Pascal A. Oesch, William McClymont, Romain A. Meyer, Yoshinobu Fudamoto, Debora Sijacki, Nicolas Laporte, Jake S. Bennett, Charlotte Simmonds, Emma Giovinazzo, A. Lola Danhaive, Laure Ciesla, Cristian Carvajal-Bohorquez, Maxime TrebitschThu, 12 Ma🔭 astro-ph