术语表与阅读清单Glossary and reading list
1. 术语表1. Glossary
| 术语Term | 解释Meaning |
|---|---|
| CGMCGM | 星系周介质：星系暗晕里、星系盘外的热气体，\(10^{6}\)–\(10^{7}\) K，软 X 射线发光。circumgalactic medium: the hot gas in a galaxy's halo, outside the disk, at \(10^{6}\)–\(10^{7}\) K, glowing in soft X-rays. |
| \(R_{500}\) | 暗晕半径，其内平均密度为宇宙临界密度的 500 倍；CGM 常用半径单位。the halo radius within which the mean density is 500\times the cosmic critical density; a common radius unit for the CGM. |
| PSF / HEWPSF / HEW | 点扩散函数 / 半能量宽度：望远镜把点源拍成光斑；HEW 是含一半光子圆的直径。point-spread function / half-energy width: the blob a telescope makes of a point source; HEW is the diameter of the circle holding half the photons. |
| EPIC MOS / pnEPIC MOS / pn | XMM-Newton 的三台 X 射线相机：两台 MOS CCD 与一台 pn CCD；所有目标都坐落在 MOS1 的 CCD1 上。XMM-Newton's three X-ray cameras: two MOS CCDs and one pn CCD; every target sits on MOS1's CCD1. |
| ACIS-I / ACIS-SACIS-I / ACIS-S | Chandra 的两种探测器排布：I 是 16.9′ 方场（S 芯片在中间），S 是 8.3′ 方场。Chandra's two detector layouts: I is a 16.9′ square (with the S chips in the middle), S is an 8.3′ square. |
| eRASS1 / eRASS:4eRASS1 / eRASS:4 | eROSITA 全天巡天的第一圈与第四圈；本项目的 eROSITA 数据来源。the first and fourth passes of the eROSITA all-sky survey; the eROSITA data source for this project. |
| QPBQPB | 静止粒子背景：高能粒子在 CCD 里的计数，用掩角事件谱（back.pi）建模，随时间漂移。quiescent particle background: counts from energetic particles hitting the CCD, modelled with the corner-events spectrum (back.pi), drifting with time. |
| SPSP | 软质子：被磁层聚焦的低能质子，幂律谱，有耀斑也有稳态残余。soft protons: low-energy protons focused by the magnetosphere, power-law spectrum, flaring with a steady residual. |
| CXBCXB | 宇宙 X 射线背景：未分辨河外源的集合计数，天空光谱的一个成分。cosmic X-ray background: the combined counts of unresolved extragalactic sources, a component of the sky spectrum. |
| null fieldnull field | 零信号场：目标在视场中心但没有延展发射的指向场；用来测仪器制造的"晕"。a pointing whose target is at the field centre but has no extended emission; used to measure the instrument-made "halo". |
| stackingstacking | 叠加：把 \(N\) 个源的同半径区域相加，信号按 \(N\)、噪声按 \(\sqrt{N}\) 增长。adding the same radial region of \(N\) sources; signal grows as \(N\), noise as \(\sqrt{N}\). |
| VrotVrot | 旋转速度：星系盘的旋转速度（km/s），与暗晕质量挂钩；本项目的新假设预测量。rotation velocity: the disk's rotation speed (km/s), tied to halo mass; the new hypothesis' predictor in this project. |
| \(M_*\) | 恒星质量：星系里恒星的总质量（\(M_\odot\)）；Zhang 标度用的预测量。stellar mass: the total mass in stars in a galaxy (\(M_\odot\)); the predictor used by Zhang's scaling. |
| Tully–FisherTully–Fisher | 塔利–费舍尔关系：旋涡星系的光度（或质量）与旋转速度的经验关系。the Tully–Fisher relation: the empirical relation between a spiral's luminosity (or mass) and its rotation velocity. |
| \(W_{50}\) | HI 谱线半峰全宽：中性氢 21 cm 谱的宽度，除以 \(2\sin i\) 得旋转速度。the HI line width at half maximum: the width of the neutral-hydrogen 21 cm line, divided by \(2\sin i\) it gives the rotation velocity. |
2. 阅读清单2. Reading list
| 文献Paper | 为什么重要Why it matters |
|---|---|
| Zhang et al. 2024（I/II，arXiv:2401.17308 / 2401.17309）Zhang et al. 2024（I/II，arXiv:2401.17308 / 2401.17309） | eROSITA SDSS 中央星系叠加：本项目矛盾的"叠加侧"；\(L_X \propto M_*^{2.4}\) 标度。the eROSITA SDSS-central stack: the "stack side" of this project's tension; the \(L_X \propto M_*^{2.4}\) scaling. |
| He & Li 2026（arXiv:2601.16499）He & Li 2026（arXiv:2601.16499） | eRASS1 474 颗 L* 星系的叠加与方位角检验；"更低更陡"的轮廓与盘光假设的削弱。the eRASS1 stack of 474 L* galaxies and its azimuthal test; the "lower and steeper" profile and the weakening of the disk-light hypothesis. |
| Li 2018 ADAP 提案proposal (XMMproposal2026/adap_reference/) | "XMM 档案里的热 CGM 遗产"：档案叠加的原始设想；本项目母表的来源。"hot CGM as a legacy of the XMM-Newton archive": the original archival-stack idea; the source of this project's parent list. |
| Li et al. 2018 / Li & Huang 2020（arXiv:2009.02596）Li et al. 2018 / Li & Huang 2020（arXiv:2009.02596） | CGM-MASS 叠加与勘误：\(L_X\) 不受勘误影响的说明，本项目引用其数值。the CGM-MASS stack and its erratum: the statement that \(L_X\) is unaffected, which this project relies on. |
| Laktionov, Sasaki & Wilms 2025（arXiv:2510.00868）Laktionov, Sasaki & Wilms 2025（arXiv:2510.00868） | NGC 5746 的独立 Chandra/XMM 分析：晕 kT 0.56、双极气泡；与 Edmund 上限的冲突。an independent Chandra/XMM analysis of NGC 5746: halo kT 0.56, biconical bubbles; in conflict with Edmund's upper limit. |
| Anderson & Bregman 2011（NGC 1961）Anderson & Bregman 2011（NGC 1961） | 单颗巨大旋涡的 Chandra 深测：\(V_{\rm rot}\) 最高、亮度最高的已测点，落在 Zhang 自相似线上。a deep Chandra measurement of one massive spiral: the highest-\(V_{\rm rot}\), brightest detected point, lying on the Zhang self-similar line. |
| Hodges-Kluck, Bregman & Li 2018（ApJ 866, 126）Hodges-Kluck, Bregman & Li 2018（ApJ 866, 126） | NGC 891 热气体的 kT 0.20 keV、Z = 0.14：单颗星系分辨测量的参照。NGC 891's hot gas at kT 0.20 keV, Z = 0.14: a reference for single-galaxy resolved measurements. |
| Zhang et al. 2025/2026（A&A 693, A197 / 706, A102）Zhang et al. 2025/2026（A&A 693, A197 / 706, A102） | eROSITA 后续：热气体质量 \(0.8\)–\(3.5 \times 10^{11} M_\odot\)（重子预算的关键数）。later eROSITA work: hot-gas mass \(0.8\)–\(3.5 \times 10^{11} M_\odot\) (the key number for the baryon budget). |
| Reyes et al. 2011（arXiv:1106.1650）Reyes et al. 2011（arXiv:1106.1650） | Tully–Fisher 的 Kroupa IMF 标定：\(V_{80}\) 与 \(M_*\) 的转换（条件性，不是测量值）。the Kroupa-IMF calibration of the Tully–Fisher relation: \(V_{80}\) to \(M_*\) conversion (conditional, not a measurement). |
来源：cognition-os/00_AI_BRIEFING.md；XMMproposal2026 cognition-os/insights/I010_literature_context.md（已核验引用清单）、I027、I028、I030；cognition-os/insights/I001、I004、I007。条目按项目记录出现顺序，未逐篇重读原文。Source: cognition-os/00_AI_BRIEFING.md; XMMproposal2026 cognition-os/insights/I010_literature_context.md (the verified citation list), I027, I028, I030; cognition-os/insights/I001, I004, I007. Entries follow the order of appearance in the project records; the original papers were not re-read one by one.