What this project asks本项目问什么
M31HotISM asks whether M31's diffuse 0.6–0.8 keV disk emission comes from old stars, star formation, or a diffuse hot halo / Galactic foreground — and whether anything remains beyond the unresolved-stellar floor.
M31HotISM 问的是：M31 弥散 0.6–0.8 keV 圆盘辐射是来自旧恒星、恒星形成，还是弥散热晕 / 银河前景；扣除未解析恒星底板后是否还有残余。
Today's answer: The halo fields 20–100′ from M31 do contain a 0.7 keV component (\(q = 34.8\), \(kT \le 0.80\) keV), but it is not identified as Milky Way or M31 gas, and the halo-field column preference is now Questioned (R126); the disk needs no diffuse M31 gas of its own — the \(3\sigma\) limit is \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s inside \(a = 56'\) and \(< 4.4\times10^{37}\) outside, and the emission is consistent with stars plus an extended foreground mixture (tag: Provisional).
今天的答案：距 M31 20–100′ 的晕场确实含有一个 0.7 keV 成分（\(q = 34.8\)，\(kT \le 0.80\) keV），但它未被识别为银河系气体还是 M31 气体，且晕场柱密度的偏好现在受质疑（R126）；圆盘本身不需要弥散的 M31 气体——\(3\sigma\) 上限为 \(a = 56'\) 以内 \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s、以外 \(< 4.4\times10^{37}\) erg/s，发射与恒星加上一个扩展的前景混合一致（标签：临时性）。
Group meeting — latest day组会 —— 最新一天
2026-11-05 (UTC). Full archive: Group meeting.
2026-11-05 (UTC)。 完整档案：组会。
Results成果
- The age-resolved emissivity is still not established, and the halo-field column preference is now Questioned. The certified response is band-independent and free per-file floors return the old-age emissivity to zero, but the physical gate still fails because the QPB/SP degeneracy is unresolved (R125); the soft QPB scale that broke the first attempt is the 1.4–2.0 keV Al K\(\alpha\) + Si K\(\alpha\) line band missing from the continuum template, not soft protons (R127). With the band below 0.5 keV removed, the refits prefer the frozen N_H 0.03 over 0.0585, so the preference most likely reflects sub-0.5 keV calibration or soft-sky modelling rather than the column (R126). Label: Questioned (the column), Provisional (the emissivity).按年龄分辨的发射率仍未确立，且晕场柱密度的偏好现在受质疑。已认证响应与波段无关，自由的逐文件底板把旧年龄发射率给回零，但物理门控仍失败，因为 QPB/SP 退化未解决（R125）；破坏首次尝试的软 QPB 尺度是连续谱模板中缺失的 1.4–2.0 keV Al K\(\alpha\) + Si K\(\alpha\) 线带，而非软质子（R127）。移除 0.5 keV 以下波段后，重拟合偏好冻结的 N_H 0.03 而非 0.0585，因此该偏好最可能反映 0.5 keV 以下的校准或软天空建模，而非柱密度本身（R126）。标签：受质疑（柱密度），临时性（发射率）。
- The halo fields 20–100′ from M31 do contain a 0.7 keV plasma component. The registered full-freedom null rejects it at \(q = 22.4\), and six warm restarts push that to \(q = 34.8\): the component sits at \(kT \le 0.80\) keV (90 %) with a norm of \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\). What the measurement does not say is whether it is Milky Way or M31 circumgalactic gas, because the registered set-up switches the Milky Way 0.7 keV term off. Label: Provisional (detection), Questioned (attribution).距 M31 20–100′ 的晕场确实含有一个 0.7 keV 等离子体成分。已注册的全自由度零假设以 \(q = 22.4\) 拒绝它，六次热重启把这一数字推到 \(q = 34.8\)：该成分位于 \(kT \le 0.80\) keV（90%），norm 为 \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\)。这项测量没有说明它是银河系气体还是 M31 星周气体，因为已注册的设置关闭了银河系 0.7 keV 项。标签：临时性（检出），受质疑（归因）。
- The disk needs no diffuse M31 gas of its own. With the stellar floor fitted rather than borrowed, only the HI-shaped gas term is separable (\(3.47 \pm 1.56\times10^{-17}\), \(2.2\sigma\)), so the \(3\sigma\) limit is \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s inside \(a = 56'\) and \(< 4.4\times10^{37}\) outside — about six times below the first estimate, and quoted as an envelope \(2.3\text{–}6.2\times10^{37}\) / \(2.7\text{–}7.1\times10^{37}\) erg/s because the term spans \(1.1\text{–}4.3\sigma\) across floor anchors. Label: Provisional, conditional.圆盘本身不需要弥散的 M31 气体。在拟合而非借用恒星底板的情况下，只有 HI 形状的气体项可分离（\(3.47 \pm 1.56\times10^{-17}\)，\(2.2\sigma\)），因此 \(3\sigma\) 上限为 \(a = 56'\) 以内 \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s、以外 \(< 4.4\times10^{37}\) erg/s——比最初的估计低约六倍，并因该项随底板锚点在 \(1.1\text{–}4.3\sigma\) 之间变动而以区间 \(2.3\text{–}6.2\times10^{37}\) / \(2.7\text{–}7.1\times10^{37}\) erg/s 引用。标签：临时性，有条件。
- The one-foreground story is no longer "one level". Two registered fits of the same halo data give \(9.66 \pm 1.16\times10^{-8}\) and \(5.0 [3.56, 7.43]\times10^{-8}\), \(2.3\text{–}2.7\sigma\) apart, so "one common level behind the halo fields, the disk floor and the stellar prediction" is a model-dependent coincidence. The working conclusion was weakened to "current fits do not require diffuse M31 gas; the emission is consistent with stellar-like emission plus an extended foreground mixture". Label: Questioned (one common level).单一前景的故事不再是“一个水平”。同一份晕场数据的两个已注册拟合给出 \(9.66 \pm 1.16\times10^{-8}\) 与 \(5.0 [3.56, 7.43]\times10^{-8}\)，相差 \(2.3\text{–}2.7\sigma\)，因此“晕场、圆盘底板与恒星预测背后有一个共同水平”是模型依赖的巧合。工作结论被减弱为“当前拟合不需要弥散的 M31 气体；发射与恒星状发射加上一个扩展的前景混合一致”。标签：受质疑（一个共同水平）。
Work工作
Six jobs in flight at 08 revision 49: two research jobs (D1d, the age-resolved emissivity regression at pixel-level support with an absolute corner→FOV QPB, resumed after its D30 input gate; V1b, the remaining nH profiles), two red teams (RT-36 on whether the nH preference is calibration or degeneracy; RT-39 on S1b’s live-time gate against the 3B maps), the S1b share-package patch on one GTI version (D30), and one literature task (L37, hot-ISM L_X per SFR).
08 修订版 49 时有六项工作在飞：两项研究工作（D1d，像素级支撑、绝对角区→视场 QPB 的按年龄分辨发射率回归，在 D30 输入门控后恢复；V1b，剩余的 nH 剖面），两个红队（RT-36 针对 nH 偏好是校准还是退化；RT-39 针对 S1b 的活时间门控与 3B 图），S1b 共享包按单一 GTI 版本修补（D30），以及一项文献任务（L37，热 ISM 的每 SFR L_X）。
Problems问题
- The age-resolved regression came back as a formal result whose physical calibration failed: the soft QPB scale was 2.70 against a prior of \(1 \pm 0.10\) (\(17\sigma\)) and the deviance/dof was 3.59, so no per-age emissivity is established. Its replacement carries a \(\pm 11\) % normalization systematic.按年龄分辨的回归给出了一个形式结果，但其物理校准失败：软 QPB 尺度为 2.70，而先前为 \(1 \pm 0.10\)（\(17\sigma\)），deviance/dof 为 3.59，因此按年龄发射率未被确立。它的替代版本带 \(\pm 11\) % 的归一化系统误差。
- The outer-rise test is power-limited: the halo-field scatter is 2–\(4 \times\) the whole detected halo range, so no per-annulus test at this precision can separate a Milky Way halo from a foreground. The pre-registered rule came back undecided.外层上升的检验受功效限制：晕场散度是整个已检出晕范围的 2–4 倍，因此在此精度下任何逐环带检验都无法区分银河系晕与前景。预注册规则的裁定为未决。
For the PI待 PI 决定
One item, answered on 2026-11-05: the S1 share package for the collaborator must be patched to one GTI version (rpc/2.filter / 3B.background, never 4.background / 2.1filter) before it is uploaded, because its masked exposure maps were built on the other GTI algorithm. S1b issues the new maps, the QPB products, the MANIFEST and a README note (D30); the upload and the sharing remain the PI’s.
一项，已于 2026-11-05 作答：给协作者的 S1 共享包必须在上传前修补为单一 GTI 版本（rpc/2.filter / 3B.background，绝不用 4.background / 2.1filter），因为它的掩蔽曝光图建立在另一种 GTI 算法上。S1b 发出新的图、QPB 产品、MANIFEST 与 README 说明（D30）；上传与共享仍由 PI 决定。
M31HotISM — hot ISM in M31's circumgalactic mediumM31HotISM —— M31 星周介质中的热星际介质
M31HotISM studies the physical origin of M31's diffuse 0.6–0.8 keV X-ray emission: does it trace old stars (stellar mass \(M_*\)), star formation (\(\Sigma_\mathrm{SFR}\)), or a diffuse hot halo / Galactic foreground, and is there a residual beyond the unresolved-stellar floor? It uses XMM-Newton EPIC MOS spectra in variable-\(W1\) elliptical annuli, an XSherpa fit template, and a template decomposition into old stellar, young, and constant components.
M31HotISM 研究 M31 弥散 0.6–0.8 keV X 射线辐射的物理起源：它是追踪旧恒星（恒星质量 \(M_*\)）、恒星形成（\(\Sigma_\mathrm{SFR}\)），还是弥散热晕 / 银河前景，并且是否存在超出未解析恒星底板的残余？项目使用 XMM-Newton EPIC MOS 谱，在变 \(W1\) 椭圆环带上，配合 XSherpa 模板拟合，并分解为旧恒星、年轻和常数三个分量。
Objectives目标
| ## | Question / criterion问题 / 标准 | Status状态 | Best current number目前最佳数字 | Source来源 | Trend趋势 |
|---|---|---|---|---|---|
| Q1 | Origin of 0.7 keV emission0.7 keV 发射起源 | Provisional / Questioned (I021)临时性 / 受质疑（I021） | kT 0.71–0.90; obs/pred 0.38→1.64, foreground-path dependent; the halo fields do contain a 0.7 keV component (q 34.8, kT \(\leq 0.80\) keV, norm 3.2–5.8e-8), but the level is estimator-dependent (\(9.66 \pm 1.16e-8\) vs 5.0 [3.56, 7.43]e-8, 2.3–\(2.7\sigma\) apart), so one common level is Questioned and a pure constant is rejected against the published near-disk levelskT 0.71–0.90；obs/pred 0.38→1.64，随前景而变；晕场确实含有一个 0.7 keV 成分（q 34.8，kT \(\leq 0.80\) keV，norm 3.2–5.8e-8），但该水平依赖于估计器（\(9.66 \pm 1.16e-8\) vs 5.0 [3.56, 7.43]e-8，相差 2.3–\(2.7\sigma\)），因此“一个共同水平”受质疑，且对照已发表的近盘水平纯常数被排除 | R007, R017, I021, R057, R071, R093R007，R017，I021，R057，R071，R093 | → |
| Q2 | Scales with \(\Sigma_*\), \(\Sigma_\mathrm{SFR}\), or \(R\)随 \(\Sigma_*\)、\(\Sigma_\mathrm{SFR}\) 或 \(R\) 变化 | Questioned受质疑 | W1 beats W4 by \(\Delta\chi^2=770\) (pedestal-laden); pedestal does not cause R006; the pilot finds old + FUV beats old + constant by \(\Delta\chi^2=-7.34\) with A_young/A_old = 0.32 (degenerate), so a young term is present but not identifiedW1 胜 W4，\(\Delta\chi^2=770\)（带底座）；底座不导致 R006；试点发现 old + FUV 胜过 old + constant，\(\Delta\chi^2=-7.34\)，A_young/A_old = 0.32（退化），因此年轻项存在但未被识别 | R013, B026, R022, R059R013，B026，R022，R059 | ↗ |
| Q3 | Azimuthal symmetry (both axes)两轴方位对称性 | Questioned受质疑 | NE \(-\) SW \(-6.3\sigma\) (conditional)NE \(-\) SW \(-6.3\sigma\)（条件性） | R011 R011 | ↘ |
| Q4 | Residual beyond stellar + foreground恒星 + 前景之外的残余 | Provisional (upper limit, no detection)临时性（上限，无检出） | with the stellar floor fitted, only the HI-shaped gas term is separable (\(3.47 \pm 1.56\times10^{-17}\), \(2.2\sigma\)): 3\(\sigma\) \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s for \(a \le 56'\), < \(4.4\times10^{37}\) erg/s for \(a \ge 56'\); quoted as the envelope 2.3–6.2e37 / 2.7–7.1e37 because the term spans 1.1–\(4.3\sigma\) across floor anchors; no diffuse M31 gas is required. The separate SFR-shaped gas term of D1b is now not detected: with the masked point-source count within 1′ as a covariate its amplitude drops from 1.3603 to 0.3673, the cluster-bootstrap interval [0, 0.97]e−16 includes zero, and at 90 % it is < 0.97e−16 \(\approx\) L < 1.1e37 erg/s over the footprint (R131)在拟合恒星底板的情况下，只有 HI 形状的气体项可分离（\(3.47 \pm 1.56\times10^{-17}\)，\(2.2\sigma\)\)：3\(\sigma\) \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s（\(a \le 56'\)），< \(4.4\times10^{37}\) erg/s（\(a \ge 56'\)）；因该项随底板锚点在 1.1–\(4.3\sigma\) 之间变动，以区间 2.3–6.2e37 / 2.7–7.1e37 引用；不需要弥散的 M31 气体。D1b 那个单独的 SFR 形状气体项现在未检出：把 1′ 内的被掩护点源计数作为协变量后，其幅度从 1.3603 降到 0.3673，簇自助法区间 [0, 0.97]e−16 包含零，90% 下 < 0.97e−16 \(\approx\) 在该足迹上 L < 1.1e37 erg/s（R131） | R064, R091, R098, R131R064，R091，R098，R131 | ↗ |
| Q5 | Unresolved-stellar fraction未解析恒星比例 | In progress进行中 | the faint-XRB share is measured (11–45 % of the inner hard excess after completeness weighting); the age-resolved emissivity priors are in hand (old population 6–10e27 erg s\(^{-}\)\(^{1}\) M☉\(^{-}\)\(^{1}\), falling about 3 dex from 10 Myr to 10 Gyr), but the age-resolved regression has failed its physical calibration three times over and is still running: D1b was formal only with the QPB/SP degeneracy unresolved (R125), D1c's support rule removed 605/622 regions and left 0/24 primary cases passing, so its full-sample row is formal too (old \(\epsilon\) 1.99 [1.72, 2.25]e27 per formed M☉, ratio 82, dev/dof 1.74, QPB pull 8.4), and D1d is running at pixel level with an absolute corner→FOV QPB after its D30 input gate (R129, R130)暗弱 XRB 份额已量出（做完备度加权后占内硬超额的 11–45 %）；按年龄分辨的发射率先验已在手中（旧种群 6–10e27 erg s\(^{-}\)\(^{1}\) M☉\(^{-}\)\(^{1}\)，从 10 Myr 到 10 Gyr 下降约 3 dex），但按年龄分辨的回归已三次未通过其物理校准，且仍在运行：D1b 只是形式结果、QPB/SP 退化未解决（R125），D1c 的支撑规则移除了 605/622 个区域、24 个主用例中 0 个通过，因此其全样本行同样只是形式结果（旧年龄 \(\epsilon\) 1.99 [1.72, 2.25]e27 每已形成 M☉、比值 82、dev/dof 1.74、QPB pull 8.4），而 D1d 在 D30 输入门控后正以像素级支撑与绝对的角区→视场 QPB 运行（R129、R130） | R068, R096, R121, R125, R129, R130, D29R068，R096，R121，R125，R129，R130，D29 | ↗ |
| N1 | Foreground absorber magnitude (T-NH)前景吸收体量级（T-NH） | Contradicted (magnitude); the 0.0585 preference is Questioned被否定（量级）；0.0585 的偏好受质疑 | MW-only \(N_\mathrm{H}\approx 0.054\)–\(0.067\times10^{22}\) cm\(^{-2}\), about twice the frozen 0.03; all 8 annuli preferred 0.0585 (\(\Delta\)\(\chi^2\) −27.8 to −218.6), but the preference is now Questioned: with E < 0.5 keV removed the reduced refits prefer 0.03 (\(\Delta\chi^2\) 3.79 and 16.73), so it most likely reflects sub-0.5 keV calibration or soft-sky modelling rather than the column; soft calibration is not excluded仅 MW \(N_\mathrm{H}\approx 0.054\)–\(0.067\times10^{22}\) cm\(^{-2}\)，约为冻结值 0.03 的两倍；全部 8 个环带曾偏好 0.0585（\(\Delta\)\(\chi^2\) −27.8 到 −218.6），但该偏好现在受质疑：移除 E < 0.5 keV 后约化重拟合偏好 0.03（\(\Delta\chi^2\) 3.79 与 16.73），因此它最可能反映 0.5 keV 以下的校准或软天空建模，而非柱密度本身；软波段校准并未被排除 | R016 (Lit L02), R116, R124, R126R016（Lit L02），R116，R124，R126 | → |
Secondary goals: G2 reusable XMM MOS extraction engine (esas_playground v1.6.1); G3 cross-project Pages directory upkeep. No science content.
次要目标：G2 可重用 XMM MOS 提取引擎（esas_playground v1.6.1）；G3 跨项目 Pages 目录维护。无科学内容。
Open problems开放问题
| Problem问题 | Why it matters为何重要 | Best hypothesis最佳假设 | Next test下一步检验 | Owner负责人 | Status状态 |
|---|---|---|---|---|---|
| 1. Is the outer-disk 0.7 keV rise foreground?1. 外盘 0.7 keV 上升是前景吗？ | Decides whether M31's disk has a hot-gas phase at all决定 M31 圆盘是否根本存在热气相 | the halo fields hold a detected 0.7 keV component (q 34.8, kT \(\leq 0.80\) keV, norm 3.2–5.8e-8), but its level is estimator-dependent (\(9.66 \pm 1.16e-8\) vs 5.0 [3.56, 7.43]e-8) and a pure constant is rejected against the published near-disk levels, so neither the level nor the origin is identified晕场存在一个已检出的 0.7 keV 成分（q 34.8，kT \(\leq 0.80\) keV，norm 3.2–5.8e-8），但其水平依赖于估计器（\(9.66 \pm 1.16e-8\) vs 5.0 [3.56, 7.43]e-8），且对照已发表的近盘水平纯常数被排除，因此水平与起源都未被识别 | the independent foreground field (FG1) and a joint fit with the foreground profiled across the halo fields and the outer annuli — a per-annulus test cannot split them at the current field scatter独立前景视场（FG1），以及在晕场与外环带上前景被 profile 的联合拟合——以当前视场散度，逐环带检验无法区分两者 | FG1, RT-36FG1，RT-36 | Undetermined: the rule came back undecided and the test is power-limited无法判定：规则裁定为未决，且该检验受功效限制 |
| 2. Stars or gas inside that foreground?2. 该前景内部是恒星还是气体？ | Sets whether the answer is a Milky Way stellar floor or a hot halo决定答案是银河系恒星底板还是热晕 | Unresolved Milky Way stars can supply \(0.5\text{--}1.0\times\) the bright-removed emissivity at our depth; the faint-end slope is the lever在我们的深度上，未解析的银河系恒星可提供亮源移除后发射率的 0.5–1.0 倍；暗端斜率是关键杠杆 | The faint-XRB share from the published X-ray luminosity functions; the age-resolved emissivity from the resolved star-formation history用已发表的 X 射线光度函数估计暗弱 XRB 份额；用已解析的恒星形成历史得到按年龄分辨的发射率 | XLF1, F1, B1, Lit L23XLF1，F1，B1，Lit L23 | Open; the mask depth is not recoverable, but the faint end is now computable开放；掩护深度无法恢复，但暗端现在可计算 |
| 3. Is the inner disk's hard excess real?3. 内圆盘的硬超额是真的吗？ | \(2\text{--}3\times\) too large for M32 stars plus faint LMXBs比 M32 恒星加暗弱 LMXB 大 2–3 倍 | the point-spread spill of masked sources was the candidate; it is now measured at \(0.70 [0.55, 0.85]\) of the King prediction, and subtracting it still leaves all 5 inner annuli hard-rich at 3.0–4.5\(\sigma\). Per K-band light the excess is 1.59 \(\pm\) ~0.2\(\times\) the Chandra M31 quiet disk, and the sources the masks miss contribute \(\leq\) ~¼ of it without the stellar-mass shape被掩护源的点扩散溢出曾是候选；现已测得为 King 预测的 \(0.70 [0.55, 0.85]\)，扣除它之后内圆盘全部 5 个环带仍硬质丰富（3.0–4.5\(\sigma\)）。按 K 光比光，超额是钱德拉 M31 安静圆盘的 1.59 \(\pm\) ~0.2 倍，而掩护漏掉的源贡献不超过其 ~¼ 且不具恒星质量形状 | the spill/zero-point convention, which the same-aperture XMM spectrum shows differs by 3.9–\(4.4 \times\) between the two conventions; the faint-XRB share is now measured (11–45 % of the excess)溢出/零点约定——同孔径的 XMM 谱显示两种约定在 H 中相差 3.9–4.4 倍；暗弱 XRB 份额现已量出（占超额的 11–45 %） | V22, RT-19, XLF2V22，RT-19，XLF2 | Provisional; survives R047's downgrade, which R048 withdrew临时性；R047 的降级被 R048 撤回 |
| 4. Halo-field 0.7 keV test4. 晕场 0.7 keV 检验 | Distinguishes M31 halo from MW foreground区分 M31 晕与 MW 前景 | a detected 0.7 keV component at \(q = 34.8\), \(kT \le 0.80\) keV (90 %), norm \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\); the level is estimator-dependent, so it is quoted as a range一个以 \(q = 34.8\) 检出的 0.7 keV 成分，\(kT \le 0.80\) keV（90%），norm \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\)；该水平依赖于估计器，因此以区间引用 | the independent foreground field (FG1) and a joint fit with the foreground profiled独立前景视场（FG1）与前景被 profile 的联合拟合 | FG1FG1 | Detected; attribution open已检出；归因开放 |
| 5. Template identifiability5. 模板可辨识性 | Old/young/constant decomposition may be degenerateold/young/constant 分解可能退化 | Old+FUV+constant identifiable (lower bound); the sky pedestal moves only the constant; the pilot finds old + FUV beats old + constant, but the red team weakened it: the gain rests on 2.08 effective spectra and A_young/A_old = \(0.325 \pm 0.346\) (\(0.94\sigma\))Old+FUV+constant 可辨识（下界）；天空底座只移动常数项；试点发现 old + FUV 胜过 old + constant，但红队将其减弱：增益仅来自 2.08 个有效谱，A_young/A_old = \(0.325 \pm 0.346\)（\(0.94\sigma\)） | the staged radial-lever fit on three annuli, with the identifiability rule and injections registered before the run在三个环带上的分阶段径向杠杆拟合，可辨识性规则与注入在运行前注册 | V6bV6b | Running; subset and rule designed运行中；子集与规则已设计 |
| 6. Azimuthal symmetry6. 方位对称性 | Sector fits were ObsID subsets, not same-area扇区拟合是 ObsID 子集，非同面积 | SE/NW difference follows MWhalo foregroundSE/NW 差异随 MWhalo 前景 | the major-axis NE/SW campaign on three matched annuli; the minor axis is untestable below ~86 % contrast, so it is dropped在三个匹配环带上的大轴 NE/SW 运动；小轴在 ~86 % 对比度以下不可测试，因此放弃 | V8bV8b | Running; campaign sized运行中；规模已估计 |
| 7. Foreground absorber magnitude7. 前景吸收体量级 | The disk fits freeze nH at 0.03e22, about half the Milky Way-only value圆盘拟合把 nH 冻结在 0.03e22，约为仅银河系值的一半 | MW-only 0.054–0.067e22; the bracket 0.048/0.0585/0.076 stands; measured in one annulus: at 0.0585e22 the disk plasma component rises 4.8 % in intrinsic surface brightness and the halo term rises 18 %仅银河系 0.054–0.067e22；区间 0.048/0.0585/0.076 保持；已在一个环带上量出：在 0.0585e22 处圆盘等离子体成分的本征表面亮度上升 4.8 %，晕项上升 18 % | V1b refits the other 8 annuli with the foreground free, reporting both componentsV1b 在前景放开的情况下重拟合其余 8 个环带，并报告两个成分 | V1bV1b | Running; one annulus measured运行中；已量出一个环带 |
| 8. Is the extraction tool trustworthy?8. 提取引擎可信吗？ | Every early extraction is made twice from now on (D23)今后每次早期提取都做两遍（D23） | the fast path reproduces the native per-channel counts exactly on identical inputs, but the particle background differs by up to 0.9 %, so the fast path replaces neither the object nor the background without qualification快速路径在相同输入上精确复现原生逐道计数，但粒子背景差异达 0.9 %，因此未经限定它既不能替代对象谱也不能替代背景 | the sector pilot as the second stage of the dual-path comparison以扇区试点作为双路径比较的第二阶段 | V8, V12V8，V12 | Stage A done; stage B queued阶段 A 已完成；阶段 B 排队中 |
| 9. Point-source mask depth (closed as unanswerable)9. 点源掩护深度（作为不可回答而关闭） | Sets the unresolved-star share of the foreground决定前景中未解析恒星的份额 | No certified selection function exists in the retained products保留产品中不存在认证的选择函数 | A matched completeness/injection test (new work, not scheduled)一次匹配的完整性/注入测试（新工作，尚未排期） | —— | Closed: BLOCKED with a justified challenge (R019)已关闭：BLOCKED，理由充分的质疑（R019） |
| 10. How much diffuse gas is allowed?10. 允许多少弥散气体？ | The upper limit is the publishable form of the answer (D27)上限是可发表形式的答案（D27） | no diffuse 0.7 keV gas in any annulus; 3\(\sigma\) \(L_X(0.5\text{–}2\,\mathrm{keV}) < 2.4\times10^{38}\) erg/s inside 56′ and < \(1.6\times10^{38}\) erg/s outside; a Mineo-level hot ISM is disfavoured at 2.2–3.2\(\sigma\)任何环带都没有弥散 0.7 keV 气体；3\(\sigma\) \(L_X(0.5\text{–}2\,\mathrm{keV}) < 2.4\times10^{38}\) erg/s（56′ 以内）以及 < \(1.6\times10^{38}\) erg/s（以外）；Mineo 级热 ISM 被否定 2.2–3.2\(\sigma\) | the stellar-floor normalisation must be fitted, not assumed; the age-resolved emissivity work supplies it恒星底板归一化必须拟合而非假定；按年龄分辨的发射率工作将提供它 | B1, F1, D1B1，F1，D1 | Provisional; the number waits on the fitted floor临时性；该数字等待拟合的底板 |
Where it stands现状
The run6 campaign is complete: 33 ObsIDs, 490 complete MOS task bundles (3,920 FITS) across 252 ObsID-region combinations. Nine retained 8' annuli give no-background SrcApec fits with \(kT = 0.71\)–\(0.90\) keV. The observed/predicted surface-brightness ratio rises from 0.38 at \(a=20'\) to 1.64 at \(a=84'\) (Provisional; crosses 1 at 60–68'). The 0.2 keV MWhalo residual is consistent with the M31CGM baseline everywhere (max \(|\sigma|=1.37\); only \(a=20'\) reaches \(\approx 2.26\sigma\) after a conservative nH correction). The halo-field 0.7 keV question now has a valid result: the component is detected (\(q = 34.8\), \(kT \le 0.80\) keV, norm \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\)), but its level is estimator-dependent and its origin is not identified, so "one common level" is Questioned. With the stellar floor fitted rather than borrowed, no diffuse M31 gas is required: the 3\(\sigma\) limit is \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s for \(a \le 56'\) and < \(4.4\times10^{37}\) erg/s for \(a \ge 56'\), quoted as an envelope because the term spans 1.1–\(4.3\sigma\) across floor anchors; a Mineo-level hot ISM is disfavoured at 2.2–\(3.2\sigma\); the separate SFR-shaped gas term of D1b is not detected either — with the masked point-source count within 1′ as a covariate its amplitude drops from 1.3603 to 0.3673 and the cluster-bootstrap interval [0, 0.97]e−16 includes zero, so at 90 % it is < 0.97e−16 ≈ L < 1.1e37 erg/s over the footprint (R131). The outer-disk rule came back undecided and power-limited, so the working conclusion is now "the emission is consistent with stellar-like emission plus an extended foreground mixture".
run6 运动已完成：33 个 ObsID，490 个完整 MOS 任务包（3,920 个 FITS），横跨 252 个 ObsID-区域组合。九个保留的 8' 环带给出无背景 SrcApec 拟合，\(kT = 0.71\)–\(0.90\) keV。观测/预测表面亮度比从 \(a=20'\) 处的 0.38 上升到 \(a=84'\) 处的 1.64（临时性；在 60–68' 处穿过 1）。0.2 keV MWhalo 残余在各处都与 M31CGM 基准一致（最大 \(|\sigma|=1.37\)；仅在 \(a=20'\) 处在保守 nH 修正后达到 \(\approx 2.26\sigma\)）。晕场 0.7 keV 问题现在有了有效结果：该成分被检出（\(q = 34.8\)，\(kT \le 0.80\) keV，norm \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\)），但其水平依赖于估计器、起源未被识别，因此“一个共同水平”受质疑。在拟合而非借用恒星底板的情况下，不需要弥散的 M31 气体：3\(\sigma\) 上限为 \(a \le 56'\) 时 \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s、\(a \ge 56'\) 时 < \(4.4\times10^{37}\) erg/s，并因该项随底板锚点在 1.1–\(4.3\sigma\) 之间变动而以区间引用；Mineo 级热 ISM 被否定 2.2–\(3.2\sigma\)；D1b 那个单独的 SFR 形状气体项也未检出——把 1′ 内的被掩护点源计数作为协变量后，其幅度从 1.3603 降到 0.3673，簇自助法区间 [0, 0.97]e−16 包含零，因此 90% 下 < 0.97e−16 \(\approx\) 在该足迹上 L < 1.1e37 erg/s（R131）。外圆盘规则的裁定为未决且受功效限制，因此工作结论现在是“发射与恒星状发射加上一个扩展的前景混合一致”。
What is unsolved未解决
Four open questions (Q1–Q4): (1) the origin of the 0.7 keV disk emission — old stars, star formation, or a diffuse halo/foreground; (2) whether it scales with \(\Sigma_*\), \(\Sigma_\mathrm{SFR}\), or projected radius \(R\); (3) whether it is smooth (halo), structured (ISM), or stellar-field-like (azimuthal symmetry); (4) whether a residual beyond stellar + foreground exists. Plus Q5 (fraction of diffuse soft X-ray in disk galaxies that is unresolved stellar) — not started.
四个开放问题（Q1–Q4）：（1）0.7 keV 圆盘发射的起源——旧恒星、恒星形成，还是弥散晕/前景；（2）它是否随 \(\Sigma_*\)、\(\Sigma_\mathrm{SFR}\) 或投影半径 \(R\) 变化；（3）它是平滑（晕）、结构化（ISM）还是恒星场状（方位对称性）；（4）是否存在恒星 + 前景之外的残余。还有 Q5（圆盘星系中弥散软 X 射线中未解析恒星的比例）——尚未开始。
What to do next下一步
The plan for the next 1–4 weeks follows 08 §3 and RESEARCH_PLAN: finish V1 (foreground-nH refit pilot, resumed with CORRECTION_04 after its evaluation gate failed at 955.007 vs 944.492), V2 (halo 0.7 keV kT profile), V6 (net old+FUV+constant template pilot), V7 (outer annuli foreground variants), V8 (clipped sector extraction pilot), V11 (point-source mask depth — reported STATUS: BLOCKED), RT-06/RT-07, Lit L03. Each running job decides one open question when it reports.
未来 1–4 周的计划遵循 08 §3 和 RESEARCH_PLAN：完成 V1（前景-nH 重拟合试点，评估门控在 955.007 vs 944.492 失败后以 CORRECTION_04 恢复）、V2（晕 0.7 keV kT 剖面）、V6（净 old+FUV+constant 模板试点）、V7（外环带前景变体）、V8（剪切扇区提取试点）、V11（点源掩护深度——报告 STATUS: BLOCKED）、RT-06/RT-07、Lit L03。每个运行中的任务在报告时决定一个开放问题。
Skeleton diagram骨架图
Data flow: XMM-Newton ObsIDs \(\rightarrow\) ESAS/SAS extraction on Virgo (run6, variable-\(W1\) annuli \(\times\) point-source masks) \(\rightarrow\) MOS spectra + RMF/ARF/QPB \(\rightarrow\) XSherpa fit template on LTD/lang2 (foreground LB+MWhalo+CXB + SrcApec + template) \(\rightarrow\) annulus profile \(\rightarrow\) template decomposition old/young/constant \(\rightarrow\) physical origin.
数据流：XMM-Newton ObsID \(\rightarrow\) Virgo 上的 ESAS/SAS 提取（run6，变 \(W1\) 环带 \(\times\) 点源掩护）\(\rightarrow\) MOS 谱 + RMF/ARF/QPB \(\rightarrow\) LTD/lang2 上的 XSherpa 拟合模板（前景 LB+MWhalo+CXB + SrcApec + 模板）\(\rightarrow\) 环带剖面 \(\rightarrow\) 模板分解 old/young/constant \(\rightarrow\) 物理起源。
Plan for the next 1–4 weeks未来 1–4 周计划
- FG1: an independent foreground field (Suzaku off-field, XMM mirror and matched-latitude fields, eRASS1 as a check), then a joint fit with the foreground profiled across the halo fields and the outer annuli — the per-annulus test is power-limited (R122).FG1：一个独立前景视场（Suzaku 离场、XMM 镜像与匹配纬度视场，eRASS1 作检查），然后在晕场与外环带上前景被 profile 的联合拟合——逐环带检验受功效限制（R122）。
- D1d: the age-resolved emissivity regression at pixel-level support with an absolute corner→FOV QPB, after D1c came back formal only — its support rule removed 605/622 regions and 0/24 primary cases passed, while the full-sample row gives old \(\epsilon\) 1.99 [1.72, 2.25]e27 per formed M☉, ratio 82, dev/dof 1.74 and QPB pull 8.4; the soft QPB scale must return to \(1 \pm 0.10\) and the deviance/dof to ~1, and the absolute emissivity carries a \(\pm 11\) % normalization systematic (R121, R123, R129, R130).D1d：像素级支撑、绝对角区→视场 QPB 的按年龄分辨发射率回归，承接 D1c 仅形式结果——其支撑规则移除了 605/622 个区域、24 个主用例中 0 个通过，而全样本行给出旧年龄 \(\epsilon\) 1.99 [1.72, 2.25]e27 每已形成 M☉、比值 82、dev/dof 1.74、QPB pull 8.4；软 QPB 尺度必须回到 \(1 \pm 0.10\)，deviance/dof 回到 ~1，且绝对发射率带 \(\pm 11\) % 的归一化系统误差（R121、R123、R129、R130）。
- V1b: the remaining nH profiles with the foreground free, giving the profile-likelihood error the conditional errors cannot provide; the first interval (a024_032) is 2.15–2.53e-7, \(2.45 \times\) the conditional error.V1b：前景放开时剩余的 nH 剖面，给出条件性误差无法提供的 profile-likelihood 误差；第一个区间（a024_032）为 2.15–2.53e-7，是条件性误差的 2.45 倍。
- RT-36: whether the 8-annuli preference for N_H = 0.0585e22 is a calibration effect or a fit degeneracy; a 2–3 % energy-dependent soft residual moves a fitted N_H by ~(0.9–2.5)e20 cm\(^{-2}\), so soft calibration is not excluded (R116, R124).RT-36：8 个环带对 N_H = 0.0585e22 的偏好是校准效应还是拟合退化；2–3 % 的能量依赖软残余会把拟合的 N_H 移动 ~(0.9–2.5)e20 cm\(^{-2}\)，因此软波段校准并未被排除（R116、R124）。
- RT-38 and RT-39: RT-38 is done — the D1b SFR-shaped soft gas term is not detected once the masked point-source count within 1′ is a covariate (amplitude 1.3603 → 0.3673, interval [0, 0.97]e−16 includes zero, so < 0.97e−16 ≈ L < 1.1e37 erg/s at 90 %); RT-39 recomputes one failing row’s map EXPOSURE against its event live time by hand, which sets the S1b rebuild scope (R127, R131).RT-38 与 RT-39：RT-38 已完成——把 1′ 内的被掩护点源计数作为协变量后，D1b 的 SFR 形状软气体项未检出（幅度 1.3603 → 0.3673，区间 [0, 0.97]e−16 包含零，因此 90% 下 < 0.97e−16 ≈ L < 1.1e37 erg/s）；RT-39 手工重算一行失败案例的图 EXPOSURE 与其事件活时间，据此确定 S1b 重建的范围（R127、R131）。
- V6b: the staged radial-lever fit on subset F (a032_040, a048_056, a080_096), with the identifiability rule and the injections registered before the run; the unit-flux conversion is fixed first.V6b：在子集 F（a032_040、a048_056、a080_096）上的分阶段径向杠杆拟合，可辨识性规则与注入在运行前注册；先修正单位通量换算。
- V8b: the major-axis NE/SW sector campaign on three matched annuli, re-gated at 457–1039 h one-worker; the fast-path twin waits for POLYGON support, so it is low priority behind the population work.V8b：在三个匹配环带上的大轴 NE/SW 扇区运动，重新门控为一工人 457–1039 h；快方孪生等待 POLYGON 支持，因此排在人口工作之后的低优先级。
- V23 / V22: the spill/zero-point convention, which the same-aperture XMM spectrum shows differs by 3.9–\(4.4 \times\) between the two conventions, and the faint-XRB share of the inner hard excess (11–45 % after completeness weighting).V23 / V22：溢出/零点约定——同孔径的 XMM 谱显示两种约定在 H 中相差 3.9–4.4 倍——以及暗弱 XRB 在内硬超额中的份额（做完备度加权后 11–45 %）。
- G1: the ~0.2–0.3 keV disk component — M31 gas or the Milky Way halo — read from V1b's corrected-N_H profiles with an M31-internal absorber, and DEM1: whether the 0.2–0.3 + 0.7 keV pair is one log-normal distribution (it is not, at the measured width).G1：~0.2–0.3 keV 圆盘成分——M31 气体还是银河晕——从 V1b 修正 N_H 的剖面读出，并带 M31 内部吸收体；以及 DEM1：0.2–0.3 + 0.7 keV 这一对是否为一个对数正态分布（在实测宽度下不是）。
- V5/E038: the RGS refit with the correct abundance table, kept at low priority behind the age-resolved line.V5/E038：用正确丰度表做的 RGS 重拟合，作为低优先级排在按年龄分辨的工作之后。
What's new本次更新
- 2026-11-05 (UTC): the age-resolved emissivity work is on its third generation, and the soft gas term it produced is gone. D1c fixed the QPB per file from the detector corners but its support rule removed 605/622 regions (13 regions and 2,926 counts left, 0/24 primary cases pass), so it is formal only: its full-sample row gives old \(\epsilon\) 1.99 [1.72, 2.25]e27 per formed M☉, ratio 82, dev/dof 1.74 and QPB pull 8.4, and D1d was launched for pixel-level support and an absolute corner→FOV QPB (R129). D1d’s D30 input audit then found 61 upstream mask/object images still on rpc/4.background (2.1filter) to be remade from 3B on Virgo, while the PHA GTI differences are \(\leq\) 1.4 % and the 25 response-gate failures are area, not time (R130). Separately, RT-38 removed the SFR-shaped soft gas term altogether: adding the masked point-source count within 1′ as a covariate cuts its amplitude 1.3603 → 0.3673 (−73 %), the cluster-bootstrap SD 0.456 is \(\approx\) 21\(\times\) the naive SE, and the interval [0, 0.97]e−16 includes zero, so at 90 % that term is < 0.97e−16 ≈ L < 1.1e37 erg/s over the footprint (R131). Label: Questioned (the term, not detected), Provisional (the emissivity).2026-11-05（UTC）：按年龄分辨发射率的工作已到第三代，而它产出的软气体项消失了。D1c 用探测器角区逐文件固定 QPB，但其支撑规则移除了 605/622 个区域（只剩 13 个区域、2,926 个计数，24 个主用例中 0 个通过），因此只是形式结果：其全样本行给出旧年龄 \(\epsilon\) 1.99 [1.72, 2.25]e27 每已形成 M☉、比值 82、dev/dof 1.74、QPB pull 8.4，于是启动 D1d 做像素级支撑与绝对的角区→视场 QPB（R129）。D1d 的 D30 输入审计随后发现 61 张上游掩护/目标图像仍在 rpc/4.background（2.1filter）上，需在 Virgo 上用 3B 重做，而 PHA 的 GTI 差异 \(\leq\) 1.4%，25 个响应门控失败是面积而非时间（R130）。另外，RT-38 完全去掉了 SFR 形状的软气体项：把 1′ 内的被掩护点源计数作为协变量加入后，其幅度从 1.3603 降到 0.3673（−73%），簇自助法的 SD 0.456 \(\approx\) 朴素 SE 的 21\(\times\)，区间 [0, 0.97]e−16 包含零，因此 90% 下该项 < 0.97e−16 ≈ 在该足迹上 L < 1.1e37 erg/s（R131）。标签：受质疑（该项，未检出），临时性（发射率）。
- 2026-11-05 (UTC): the S1 exposure-map mismatch has an explanation and a rule. The share package’s inventory preferred the rpc/4.background products, which are built from a different GTI algorithm (2.1filter) than the events it ships (2.filter), so most of its maps disagree with its own events. Every product now pairs with the 2.filter events, and the share package is patched before it is uploaded — the upload and the sharing remain the PI’s. Label: accepted (the rule), Provisional (the patch).2026-11-05（UTC）：S1 曝光图不匹配有了解释与规则。共享包的清单优先选了 rpc/4.background 产品，它们由与所发事件（2.filter）不同的 GTI 算法（2.1filter）构建，因此其大部分图与自己的事件不一致。现在每个产品都与 2.filter 事件配对，共享包在上传前修补——上传与共享仍由 PI 决定。标签：被接受（规则），临时性（修补）。
- 2026-11-05 (UTC): the age-resolved regression came back again, and the column question with it. The certified response is band-independent (no double vignetting) and free per-file floors return the old-age emissivity to zero, but the physical gate still fails because the QPB/SP degeneracy is unresolved (R125). The soft QPB scale that broke the first attempt is now identified: it is the 1.4–2.0 keV Al K\(\alpha\) + Si K\(\alpha\) line band missing from the continuum template, not soft protons (R127). And the halo-field column preference is now Questioned rather than established — with the band below 0.5 keV removed the refits prefer the frozen 0.03, so the 0.0585 value most likely reflects sub-0.5 keV calibration or soft-sky modelling rather than the column (R126). Label: Questioned (the column), Provisional (the emissivity).2026-11-05（UTC）：按年龄分辨的回归再次给出结果，柱密度问题也随之改变。已认证的响应与波段无关（无双重消光），自由的逐文件底板把旧年龄发射率给回零，但物理门控仍失败，因为 QPB/SP 退化未解决（R125）。破坏首次尝试的软 QPB 尺度现已被定位：它是连续谱模板中缺失的 1.4–2.0 keV Al K\(\alpha\) + Si K\(\alpha\) 线带，而非软质子（R127）。而晕场柱密度的偏好现在从“已确立”变为“受质疑”——移除 0.5 keV 以下波段后重拟合偏好冻结的 0.03，因此 0.0585 更可能反映 0.5 keV 以下的校准或软天空建模，而非柱密度本身（R126）。标签：受质疑（柱密度），临时性（发射率）。
- 2026-11-04 (UTC): the halo fields 20–100′ from M31 do contain a 0.7 keV plasma component. The registered full-freedom null rejects it at \(q = 22.4\), and six warm restarts push that to \(q = 34.8\): \(kT \le 0.80\) keV at 90 %, norm \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\). What the measurement does not say is whether the component is Milky Way or M31 gas, because the registered set-up switches the Milky Way 0.7 keV term off. Label: Provisional (detection), Questioned (attribution).2026-11-04（UTC）：距 M31 20–100′ 的晕场确实含有一个 0.7 keV 等离子体成分。已注册的全自由度零假设以 \(q = 22.4\) 拒绝它，六次热重启把这一数字推到 \(q = 34.8\)：90% 下 \(kT \le 0.80\) keV，norm \(3.2\text{–}5.8\times10^{-8}\) arcmin\(^{-2}\)。但这项测量没有说明该成分是银河系气体还是 M31 气体，因为已注册的设置关闭了银河系 0.7 keV 项。标签：临时性（检出），受质疑（归因）。
- The gas limit moved again, and it is now conditional rather than one number. With the stellar floor fitted instead of borrowed, only the HI-shaped gas term is separable (\(3.47 \pm 1.56\times10^{-17}\), \(2.2\sigma\)), so the \(3\sigma\) limit is \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s inside \(a = 56'\) and \(< 4.4\times10^{37}\) outside — about six times below the first estimate. Because the term spans 1.1–4.3\(\sigma\) across floor anchors, the page quotes the envelope 2.3–6.2e37 / 2.7–7.1e37 erg/s with its anchor named.气体上限又变了一次，现在是有条件的而非单一数字。在拟合而非借用恒星底板的情况下，只有 HI 形状的气体项可分离（\(3.47 \pm 1.56\times10^{-17}\)，\(2.2\sigma\)），因此 \(3\sigma\) 上限为 \(a = 56'\) 以内 \(L_X(0.5\text{–}2\,\mathrm{keV}) < 3.8\times10^{37}\) erg/s、以外 \(< 4.4\times10^{37}\) erg/s——比最初的估计低约六倍。因该项随底板锚点在 1.1–4.3\(\sigma\) 之间变动，本页以区间 2.3–6.2e37 / 2.7–7.1e37 erg/s 引用并注明锚点。
- "One common level" is now Questioned. Two registered fits of the same halo data give \(9.66 \pm 1.16\times10^{-8}\) and \(5.0 [3.56, 7.43]\times10^{-8}\), \(2.3\text{–}2.7\sigma\) apart, and the registered halo levels span \(\times\)11.8 across fits of the same data. The working conclusion was weakened to "current fits do not require diffuse M31 gas; the emission is consistent with stellar-like emission plus an extended foreground mixture".“一个共同水平”现在受质疑。同一份晕场数据的两个已注册拟合给出 \(9.66 \pm 1.16\times10^{-8}\) 与 \(5.0 [3.56, 7.43]\times10^{-8}\)，相差 \(2.3\text{–}2.7\sigma\)，而已注册的晕水平在同一数据的拟合间跨度为 \(\times\)11.8。工作结论被减弱为“当前拟合不需要弥散的 M31 气体；发射与恒星状发射加上一个扩展的前景混合一致”。
- The outer-disk rule came back undecided, and the red team showed why it cannot decide at this precision: the foreground increment that removes the outer rise is sky-flat, but the halo-field scatter is 2–\(4 \times\) the whole detected halo range, so no per-annulus test can separate a halo from a foreground. The independent foreground field (FG1) is the next step.外圆盘规则的裁定为未决，而红队说明了它为何在此精度下无法决定：移除外层上升所需的前景增量在天空上是平坦的，但晕场散度是整个已检出晕范围的 2–4 倍，因此任何逐环带检验都无法区分晕与前景。独立前景视场（FG1）是下一步。
- The age-resolved regression came back as a formal result whose physical calibration failed (soft QPB scale 2.70 against a prior of \(1 \pm 0.10,\) deviance/dof 3.59), so no per-age emissivity is established; its replacement carries a \(\pm 11\) % normalization systematic. The nH preference in all 8 annuli was later Questioned: with the band below 0.5 keV removed the reduced refits prefer the frozen 0.03 (R126), and soft calibration is not excluded as its cause.按年龄分辨的回归给出了一个形式结果，但其物理校准失败（软 QPB 尺度 2.70 而先前为 \(1 \pm 0.10\)，deviance/dof 3.59），因此按年龄发射率未被确立；其替代版本带 \(\pm 11\) % 的归一化系统误差。全部 8 个环带的 nH 偏好后来受质疑：移除 0.5 keV 以下波段后约化重拟合偏好冻结的 0.03（R126），且软波段校准并未被排除为其成因。
- Improved: the first phone screen now says what the project asks and today's one-line answer, in both languages, above the group-meeting card (element id
group-meeting-summary). New figure: the halo-field detection and the estimator-dependent level (assets/figures/fig_halo_detect.png).改进：首个手机屏现在在组会卡之上用两种语言说明本项目问什么以及今天的一句话答案（元素 idgroup-meeting-summary）。新图：晕场检出与依赖于估计器的水平（assets/figures/fig_halo_detect.png）。 - 2026-11-03 (UTC): the diffuse-gas question had its first number — no diffuse M31 0.7 keV gas in any of the nine annulus, a 3\(\sigma\) limit of \(2.4\times10^{38}\) / \(1.6\times10^{38}\) erg/s with a borrowed floor, and the run6 premise withdrawn (R064, R070). Both numbers were superseded on 2026-11-04.2026-11-03（UTC）：弥散气体问题有了第一个数字——九个环带中都没有弥散的 M31 0.7 keV 气体，借用底板时 3\(\sigma\) 上限为 \(2.4\times10^{38}\) / \(1.6\times10^{38}\) erg/s，同时 run6 前提被撤回（R064、R070）。两个数字都在 2026-11-04 被取代。
Data as of数据截至
Newest source read: cognition-os/08_RUNNING.md, revision 49, updated 2026-11-05 03:56 EST; trust table read 2026-11-05 03:15 EST; 07_REVISION_LOG.md rows R001–R131 and 04_DECISION_LOG.md D26–D30 read in full.
最新读取的来源：cognition-os/08_RUNNING.md，修订版 49，更新于 2026-11-05 03:56 EST；信任表读取于 2026-11-05 03:15 EST；07_REVISION_LOG.md 的 R001–R131 行与 04_DECISION_LOG.md 的 D26–D30 已全文读取。