CSST 暗物质粒子性质 2025

24 Oct 2025, 08:00 → 27 Oct 2025, 17:00 Asia/Shanghai

尊敬的各位同仁：

         暗物质研究是当代基础科学的核心议题。探索其本质并揭示其塑造宇宙结构的关键作用，将极大深化人类对物质起源、物理规律及宇宙演化的认知。自上世纪三十年代暗物质问题被提出以来，理解暗物质本质及其对宇宙结构演化和星系形成的决定性影响，已成为宇宙学最重要的前沿领域之一。我国自然科学基金委在“十四五”规划中，已将“研究暗物质本质”列为优先发展的重要方向。

 

        为了推动理论、数值模拟与观测的交叉研究，本次会议邀请了CSST第二批科学研究课题（CSST时代的暗物质宇宙测绘和暗物质性质研究）的科学家集中研讨空间望远镜时代的暗物质研究，并特邀了课题外的暗物质专家参与指导，共同探讨如何结合矮星系暗物质间接探测与宇宙学模拟，并进一步预言CSST的探测能力。

 

         会议定于 2025年10月24日至27日在江苏省淮安市盱眙县天泉湖金陵山庄召开，由紫金山天文台主办。会议主题将聚焦暗物质间接探测与暗物质晕寻找的交叉研究，并涵盖以下领域：CSST对暗物质宇宙学参数的限制、暗物质性质限制与检验的理论与观测研究、宇宙大尺度暗物质分布重构，以及多尺度多方法的暗物质联合检验。

 

会议基本信息：

会议时间：2025年10月24日-27日（24日报到，25-26日会议，27日离会）

会议注册：截止日期为2025年09月29日

注册费用：本次会议不收取注册费

食宿安排：本次会议统⼀安排住宿，会议期间交通费和⻝宿费⾃理。

会议组委会：

蔡岳霖 紫金山天文台

袁  强 紫金山天文台

黄晓渊 紫金山天文台

李  翔 紫金山天文台

杨大能 紫金山天文台

沈兆强 紫金山天文台

李然 北京师范大学

 

 

 

2025CSST暗物质粒子性质-会议手册-v3.pdf

盱眙CSST会议通知.pdf

Friday 24 October

14:00 → 20:00 注册

Saturday 25 October

08:50 → 09:00 开场

蔡岳霖

09:00 → 11:45 Session 1 （每个报告：30分钟个人报告+15分钟讨论）

时长说明: 30分钟报告+15分钟讨论

Convener: Prof. 国亮 李 (紫金山天文台)

09:00 孤立的暗物质缺失矮星系

在标准宇宙学中，暗物质推动了星系的结构形成，并构建了形成星系的势阱。在大质量星系团中，暗晕中的重子物质比例将将达到宇宙平均值（15.7%），重子物质比例随着系统质量的降低而迅速减少。在矮星系中暗物质的质量占主导地位，即使在其光半光半径内（re≈1 kpc）仍然是暗物质主导。然而，最近有研究发现并非所有的矮星系都是由暗物质主导的，我们也发现了19个暗物质缺失的矮星系（ dark-matter-deficient dwarf galaxies DMDGs），它们在远大于re范围内主要由重子物质组成，这与标准宇宙学预言的矮星系应为暗物质主导相悖。从流体力学模拟中对这种矮星系的研究表明，星系在高密度区域的相互作用以及环境剥离是形成重子物质主导矮星系的原因。然而要解释孤立环境中DMDG（14/19）的形成和演化更具有挑战性，因为其形成和演化不受环境影响，目前我们的标准宇宙学无法解释重子物质主导矮星系是如何形成的。这样的系统对目前的星系形成理论提出了挑战，也为暗物质的本质提供了新的线索（例如，温暗物质、模糊暗物质、自相互作用暗物质或MOND）。

Speaker: Prof. 慧杰 胡 (安庆师范大学)

胡慧杰_CSST.pdf

09:45 Dwarf galaxies as dark matter probes with CSST

Speaker: Prof. 珍 袁 (南京大学)

CSST_DarkMatter_ZYuan_Oct2025.pdf

10:30 茶歇

11:00 Dark matter annihilation signals from the possible faintest dwarf satellite galaxy

Speaker: Prof. 鹏飞 殷 (高能物理研究所)

251025 Dark matter annihilation signatures from the possible faintest dwarf satellite galaxy.pdf

11:45 → 13:15 午餐

13:15 → 15:30 Session2 （每个报告：30分钟个人报告+15分钟讨论）

时长说明: 30分钟报告+15分钟讨论

Convener: Prof. 欢源 陕

13:15 一个具有异常高聚集度暗物质晕的并合矮星系遗迹

Speaker: Dr 孚嘉 李 (中国科学技术大学)

盱眙_李孚嘉.pptx

14:00 The central regions of galaxies as the probe of dark matter: astrophysical uncertainties

Speaker: Prof. 辉 李 (清华大学)

2025.10.25_PMO.pdf

14:45 Detecting ultralight dark photon dark matter with precision stellar astrometry

Speaker: Prof. 强 袁 (紫金山天文台)

2025_CSST_YuanQ.pdf

15:30 → 16:00 茶歇

16:00 → 18:15 Session3 （每个报告：30分钟个人报告+15分钟讨论）

时长说明: 30分钟报告+15分钟讨论

Convener: Prof. 强 袁 (紫金山天文台)

16:00 Constraining the properties of dark matter by astronomical observations

Speaker: Prof. 效军 毕 (高能物理研究所)

2025CSST-DM.pdf

16:45 The Preliminary Investigation of Low- Acceleration Gravitational Anomaly in Wide Binaries

Speaker: Dr 豪然 陈 (杭州电子科技大学)

The Preliminary Investigation of Low-Acceleration Gravitational Anomaly in Wide Binaries.ppt

17:30 Beyond Collisionless Cold Dark Matter: Observational Clues to Self-Interacting Dark Matter

Cold dark matter (CDM) has been remarkably successful in describing the large-scale universe, yet tensions persist on smaller scales — from dwarf galaxy cores to the excess of galaxy–galaxy strong lensing (GGSL) anomalies in clusters. These discrepancies point to limitations in the collisionless CDM paradigm. In this talk, I will focus on self-interacting dark matter (SIDM), and in particular a two-component model with mass segregation, which offers a unified explanation for both dwarf-scale cores and GGSL anomalies. These observational clues underscore the power of lensing and other astrophysical probes in revealing the microphysics of the dark sector.

Speaker: Dr 思媛 侯 (紫金山天文台)

Siyuan2025CSST.pdf

18:20 → 19:50 晚宴

Sunday 26 October

09:00 → 12:00 Session 4（每个报告：30分钟个人报告+15分钟讨论）: （每个报告：30分钟个人报告+15分钟讨论）

时长说明: 30分钟报告+15分钟讨论

Convener: Prof. 效军 毕

09:00 Baryon-Dominated Dwarf Galaxy Enhanced by Weakened Gravitational Binding in Galaxy Collisions

Baryon-dominated dwarf galaxies (BDDGs) can emerge from high-velocity collisions between gas-rich ultra-diffuse galaxies. Using hydrodynamical simulations with progenitors of contrasting gravitational binding energies, we show that progenitor structure critically regulates BDDG formation. Specifically, collisions involving more weakly bound progenitors sustain star formation longer and yield more massive BDDGs, whereas tightly bound progenitors experience stronger tidal winds that preferentially produce multiple low-mass remnants. While both bursty stellar feedback and elastic self-interacting dark matter can generate cored halos, only feedback injects energy and boosts the BDDG formation. Our results position collisional BDDGs as a novel probe of feedback-regulated galaxy formation and dark matter physics. Upcoming wide-field imaging (CSST, LSST), HI surveys (FAST), and kinematic follow-up will be crucial for identifying candidates and testing these scenarios.

Speaker: Prof. 大能 杨 (紫金山天文台)

CSST.pdf

09:45 The dark matter content of Milky Way dwarf spheroidal galaxies: Draco, Sextans and Ursa Minor

The Milky Way Survey of the Dark Energy Spectroscopic Instrument (DESI) has so far observed three classical dwarf spheroidal galaxies (dSphs): Draco, Sextans and Ursa Minor. Based on the observed line-of-sight velocities and metallicities of their member stars, we apply the axisymmetric Jeans Anisotropic Multi-Gaussian Expansion modeling (JAM) approach to recover their inner dark matter distributions. In particular, both the traditional single-population Jeans model and the multiple population chemodynamical model are adopted. With the chemodynamical model, we divide member stars of each dSph into metal-rich and metal-poor populations. The metal-rich populations are more centrally concentrated and dynamically colder, featuring lower velocity dispersion profiles than the metal-poor populations. We find a diversity of the inner density slopes of dark matter halos, with the best constraints by single-population or chemodynamical models consistent with each other. The inner density slopes are 0.71, 0.26 and 0.33 for Draco, Sextans and Ursa Minor, respectively. We also present the measured astrophysical J and D factors of the three dSphs. Our results indicate that the study of the dark matter content of dSphs through stellar kinematics is still subject to uncertainties behind both the methodology and the observed data, through comparisons with previous measurements and data sets.

Speaker: Dr 皓 杨 (上海交通大学)

MWdwarf-杨皓.pdf

10:30 茶歇

11:00 Exploring the dark matter identity with strong strong lensing in CSST Era

Speaker: Prof. 然 李 (国家天文台)

LittleDarkDot_2025.pdf

11:45 closing remark

12:00 → 13:30 午餐

14:00 → 15:00 回程

从金陵山庄搭车前往紫台仙林园区