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astro-ph.GA

365 篇论文

Weighing gas-rich starless halos: dark matter parameters inference from their gas distributions

该研究利用贝叶斯嵌套采样方法，通过分析无恒星气体云（RELHICs）的分布，证明了在将环境密度作为自由参数以打破质量 - 浓度简并后，能够高精度地推断出宿主暗物质晕的维里质量，从而为未来巡天中称量无恒星暗物质晕提供了可靠框架。

Francesco Turini (University of Milano-Bicocca), Alejandro Benitez-Llambay (University of Milano-Bicocca)Mon, 09 Ma🔭 astro-ph

The case of NGC 5824, a cluster possibly embedded in a dark matter halo

本研究利用深度测光与盖亚数据证实，球状星团 NGC 5824 具有延伸至约 20 角分的对称扩散包层，其外表面密度轮廓的幂律指数（γ∼−2.6\gamma \sim -2.6）与嵌入暗物质晕的预测相符，暗示该星团可能确实被暗物质晕所包裹。

Paula B. Díaz, Berenice Muruaga, Ricardo R. Muñoz, Julio A. Carballo-Bello, Pete B. Kuzma, Valentina SuárezMon, 09 Ma🔭 astro-ph

Multiwavelength quasi-periodic variability of the blazar Ton 599

本文基于1983至2025年的多波段观测数据，发现TeV耀变体Ton 599存在显著的准周期性光变，其多波段辐射的相关性及多种特征周期（1.4至7.5年）表明，该现象是由双超大质量黑洞系统的轨道运动与喷流进动等几何效应，以及喷流内部激波等随机过程共同调制所致。

Yu. V. Sotnikova (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), T. V. Mufakharov (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia, Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science-1 Street, Urumqi 830011, China), A. E. Volvach (Crimean Astrophysical Observatory of the Russian Academy of Sciences, 298409, Nauchny, Russia), V. V. Vlasyuk (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), M. L. Khabibullina (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), A. G. Mikhailov (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), T. An (State Key Laboratory of Radio Astronomy and Technology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, China, Guizhou Radio Astronomical Observatory, Guizhou University, 550000, Guiyang, China), D. O. Kudryavtsev (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), Yu. A. Kovalev (Lebedev Physical Institute of Russian Academy of Sciences, Leninsky prosp. 53, Moscow 119991, Russia, Institute for Nuclear Research, Russian Academy of Sciences, 60th October Anniversary Prospect 7a, Moscow 117312, Russia), Y. Y. Kovalev (Max Planck Institute for Radio Astronomy, Auf dem Hügel 69, Bonn 53121, Germany), A. V. Popkov (Moscow Institute of Physics and Technology, Institutsky per. 9, Dolgoprudny 141700, Russia, Lebedev Physical Institute of Russian Academy of Sciences, Leninsky prosp. 53, Moscow 119991, Russia), S. S. Savchenko (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia, Pulkovo Observatory, St. Petersburg, 196140, Russia), A. K. Erkenov (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), D. A. Morozova (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), T. A. Semenova (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), O. I. Spiridonova (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), M. A. Kharinov (Institute of Applied Astronomy of the Russian Academy of Sciences, Kutuzova Embankment 10, St. Petersburg 191187, Russia), I. A. Rakhimov (Institute of Applied Astronomy of the Russian Academy of Sciences, Kutuzova Embankment 10, St. Petersburg 191187, Russia), T. S. Andreeva (Institute of Applied Astronomy of the Russian Academy of Sciences, Kutuzova Embankment 10, St. Petersburg 191187, Russia), L. Cui (Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science-1 Street, Urumqi 830011, China), X. Wang (Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science-1 Street, Urumqi 830011, China), N. Chang (Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 150 Science-1 Street, Urumqi 830011, China), R. Yu. Udovitskiy (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), P. G. Zhekanis (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), G. A. Borman (Crimean Astrophysical Observatory of the Russian Academy of Sciences, 298409, Nauchny, Russia), T. S. Grishina (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), E. N. Kopatskaya (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), E. G. Larionova (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), I. S. Troitskiy (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), Yu. V. Troitskaya (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), A. A. Vasilyev (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), A. V. Zhovtan (Crimean Astrophysical Observatory of the Russian Academy of Sciences, 298409, Nauchny, Russia), D. V. Kratov (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia), L. N. Volvach (Crimean Astrophysical Observatory of the Russian Academy of Sciences, 298409, Nauchny, Russia), E. V. Shishkina (Saint Petersburg State University, 7/9 Universitetskaya nab., St. Petersburg, 199034, Russia), A. I. Dmytrotsa (Crimean Astrophysical Observatory of the Russian Academy of Sciences, 298409, Nauchny, Russia), V. I. Zharov (Special Astrophysical Observatory of the Russian Academy of Sciences, Nizhny Arkhyz, 369167, Russia)Mon, 09 Ma🔭 astro-ph

An updated model for the Perseus Spiral Arm from Trigonometric Parallax and 3D kinematic distances of distant young stars

该研究利用 VLBA 对四个脉泽源的三角视差测量结果，结合三维运动学距离，修正了银河系第一象限内英仙座旋臂的位置，发现其距离银河中心比此前认知远 0.5 至 1.0 千秒差距，并确定了其与人马座旋臂在银河系远侧的交汇点。

Lucas J. Hyland, Mark J. Reid, Simon P. Ellingsen, Andreas Brunthaler, Xing-Wu Zheng, Karl M. MentenMon, 09 Ma🔭 astro-ph

Confirmation and Refutation of Lyman Continuum Leakers at z∼3z\sim3 with JWST NIRSpec/IFU

该研究利用 JWST NIRSpec/IFU 观测证实，红移 z∼3z\sim3 处的候选体 LACES-104037 中的潮汐尾结构（LACES104037-LyC）是一个逃逸率高达 99% 的莱曼连续谱光子泄漏源，揭示了星系并合是驱动早期宇宙再电离的重要机制，同时排除了另一候选体 LACES-94460 因低红移前景天体污染而导致的误判。

Shengzhe Wang, Xin Wang, Hang Zhou, Yiming Yang, Zhiyuan Ji, Yuxuan Pang, Chao-Wei Tsai, Akio K. Inoue, Mengtao Tang, Themiya Nanayakkara, Karl Glazebrook, Hu Zhan, Pinjian ChenMon, 09 Ma🔭 astro-ph

Extremely Metal-Poor Galaxies in DESI DR1: Connections to Galaxies in the Early Universe

该研究利用 DESI DR1 数据发现了大量极低金属丰度星系（XMPGs），证实它们不仅具有低金属丰度，还展现出与高红移早期宇宙星系相似的特有恒星形成主序和丰度关系，从而确立了其作为研究早期星系形成过程本地实验室的重要价值。

Jipeng Sui, Hu Zou, Dirk Scholte, Amélie Saintonge, Mar Mezcua, Malgorzata Siudek, Wenxiong Li, Wei-Jian Guo, Shufei Liu, Yunao Xiao, Francisco Prada, Siwei Zou, Jessica Nicole Aguilar, Steven Ahlen, Carlos Allende Prieto, Davide Bianchi, David Brooks, Yu-Ling Chang, Todd Claybaugh, Andrei Cuceu, Axel de la Macorra, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, ChangHoon Hahn, Dick Joyce, Robert Kehoe, Martin Landriau, Laurent Le Guillou, Yifei Luo, Aaron Meisner, Ramon Miquel, Seshadri Nadathur, Nathalie Palanque-Delabrouille, Will Percival, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan WeaverMon, 09 Ma🔭 astro-ph

SwinYNet: A Transformer-based Multi-Task Model for Accurate and Efficient FRB Search

本文提出了名为 SwinYNet 的基于 Transformer 的多任务模型，该模型无需耗时的去色散预处理即可直接从时频数据中实现快速射电暴（FRB）的检测、分割及参数估计，在模拟与实测数据中均展现出超越传统工具及现有 AI 基线的卓越精度与实时处理能力。

Yunchuan Chen, Shulei Ni, Chan Li, Jianhua Fang, Dengke Zhou, Huaxi Chen, Yi Feng, Pei Wang, Chenwu Jin, Han Wang, Bijuan Huang, Xuerong Guo, Donghui Quan, Di LiMon, 09 Ma🔭 astro-ph

Untangling dust emission and CIB anisotropies with the Scattering Transform Statistics

该研究提出并验证了一种基于散射协方差统计的统计成分分离方法，通过构建宇宙红外背景（CIB）生成模型，成功从 Planck 353 GHz 观测数据中分离出银河系尘埃发射信号，从而克服了传统模板拟合法在复杂气体区域失效的局限，为绘制中高银纬星际消光图提供了新途径。

Srijita Sinha (National Institute of Science Education and Research, An OCC of Homi Bhabha National Institute, Bhubaneswar 752050, Odisha, India), Tuhin Ghosh (National Institute of Science Education and Research, An OCC of Homi Bhabha National Institute, Bhubaneswar 752050, Odisha, India), Erwan Allys (Laboratoire de Physique de l'École normale supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, F-75005 Paris, France and), François Boulanger (Laboratoire de Physique de l'École normale supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université Paris Cité, F-75005 Paris, France and), Jean-Marc Delouis (Laboratoire d'Océanographie Physique et Spatiale)Mon, 09 Ma🔭 astro-ph

Size measurements and characterization of the astrophysical properties of multiple-component radio-AGNs in the ROGUE I catalog

本文基于 ROGUE I 目录，对手动测量的 2002 个多分量射电活动星系核进行了尺寸测定与表征，揭示了其物理属性、形态分类（如 FR I/II、弯曲尾等）与星系团环境及喷流稳定性之间的关联。

Arti Goyal, Arpita Misra, Subhrata Dey, Unnikrishnan Sureshkumar, Marion Soida, Anna Wojtowicz, Grazyna Stasinska, Natalia Vale Asari, Syed NaqviMon, 09 Ma🔭 astro-ph

The contribution to Galactic Centre {\gamma}-ray excess from cluster-born millisecond pulsars. Constraints from direct N-body simulations

该研究利用高分辨率直接 N 体模拟追踪球状星团中诞生并注入银河系中心的毫秒脉冲星，发现其累积产生的伽马射线辐射能够很好地解释银河系中心伽马射线超出（GCE）现象，从而支持其天体物理起源而非暗物质湮灭的解释。

M. Kalambay, M. Ishchenko, D. Kuvatova, T. Panamarev, P. BerczikMon, 09 Ma🔭 astro-ph

The trigonometric parallax of IRAS 23385+6053 and physical properties of molecular clouds based on the VLBI astrometry

该研究利用日本 VERA 的甚长基线干涉测量技术，精确测定了 IRAS 23385+6053 区域的三角视差，发现其距离约为 2.17 千秒差距（仅为先前运动学距离的一半），并据此揭示了仙后座和仙王座区域英仙座旋臂分子云在视线方向上延伸约 2 千秒差距的物理结构。

Shota Hamada, Mikito Kohno, Toshihiro Omodaka, Nobuyuki Sakai, Riku Urago, Takumi Nagayama, Hideyuki Kobayashi, Yuji UenoMon, 09 Ma🔭 astro-ph

Implications for Type Ia Supernova Nucleosynthesis from an Experimentally Constrained 16^{16}O(p,α)13(p,\alpha)^{13}N Reaction Rate

该研究通过首次在天体物理能区直接测量16^{16}O(p,α)13(p,\alpha)^{13}N反应截面，确定了其反应率仅比标准值高约1.5倍，从而排除了此前认为高达七倍的增强假设，表明该反应无法单独解释Ia型超新星中钙硫比随前身星金属丰度的变化，未来需聚焦于其他关键氧燃烧反应的不确定性。

M. Alruwaili (University of York, UK, Northern Border University, Saudi Arabia), C. Fougeres (Argonne National Laboratory, USA), A. M. Laird (University of York, UK), H. Jayatissa (Argonne National Laboratory, USA), M. L. Avila (Argonne National Laboratory, USA), E. Bravo (Universidad de Granada, Spain), C. Angus (University of York, UK, TRIUMF, Canada), C. Badenes (University of Pittsburgh, USA), S. Chakraborty (University of York, UK), C. Diget (University of York, UK), N. de Sereville (Institut de Physique Nucleaire d'Orsay, France), A. Hall-Smith (University of York, UK), R. Longland (North Carolina State University, USA, Triangle Universities Nuclear Laboratory, USA), W. -J. Ong (Lawrence Livermore National Laboratory, USA), K. E. Rehm (Argonne National Laboratory, USA), D. Santiago-Gonzalez (Argonne National Laboratory, USA)Mon, 09 Ma🔭 astro-ph

Effects of Self-Interaction and of an Ideal Gas in Binary Mergers of Bosonic Dark Matter Cores

该研究通过三维数值模拟发现，玻色暗物质核心并合后的最终质量比受自相互作用性质（排斥或吸引）的调控，而与理想气体的相互作用仅改变引力背景却不影响玻色组分的内禀标度律，从而揭示了并合结果的非普适性及玻色核心在不同环境下的鲁棒性。

Carlos Tena-Contreras, Ivan Alvarez-Rios, Francisco S. Guzman, Jens NiemeyerMon, 09 Ma🔭 astro-ph

Molecular Clouds Resolved at the Onset of Cosmic Noon

该研究利用甚大阵列（VLA）在红移 z=3.4 的射电星系 B2 0902+34 中，通过 CO(0-1) 吸收特征首次解析出七个分子云，其物理性质与银河系分子云相似，为研究宇宙正午时期恒星形成的云团物理与化学过程开辟了新途径。

Bjorn Emonts (NRAO Charlottesville), Matthew Lehnert (Univ. Lyon/CNRS), Mingyu Li (Tsinghua Univ), Azia Robinson (Agnes Scott College, NRAO Charlottesville), Stephen Curran (Univ. Wellington), Montserrat Villar-Martin (CAB/CSIC-INTA), Chris Carilli (NRAO Socorro), Raffaella Morganti (ASTRON, Kapteyn Inst), Ilsang Yoon (NRAO Charlottesville), Pierre Guillard (IAP/CNRS), George Miley (Leiden Obs), Reinout van Weeren (Leiden Obs), Zheng Cai (Tsinghua Univ)Mon, 09 Ma🔭 astro-ph