仪器与数据

Instrument and data

XMM-Newton EPIC-MOS diffuse-background spectra；作者统一处理档案视线、剔除点源并显式拟合仪器与天体背景。

XMM-Newton EPIC-MOS diffuse-background spectra, with archival sightlines processed uniformly, point sources removed, and instrumental plus astrophysical backgrounds modeled explicitly.

观测视线与样本域

Sightlines and sample domain

主catalog包含110个高银纬结果行；87行为halo detections。Figure 3转换使用其中86个具有唯一LAB N_H的detections；合并视线Seq=103因没有唯一吸收柱而排除。M31约b=-21.6 deg，不在该高纬样本的目标域内。

The main catalog contains 110 high-latitude result rows, including 87 halo detections. The Figure 3 conversion uses 86 detections with a unique LAB N_H; combined sightline Seq=103 is excluded because it has no unique absorption column. M31, near b=-21.6 deg, is outside the sample domain.

原文测量量

Native measurement

原始量是每条视线拟合得到的intrinsic 0.5-2.0 keV one-temperature Galactic-halo surface brightness、temperature及LAB N_H。它不是absorbed M31-direction broadband flux。

The native quantities are the fitted intrinsic 0.5-2.0 keV one-temperature Galactic-halo surface brightness, temperature, and LAB N_H for each sightline. They are not absorbed broadband fluxes toward M31.

原文模型

Published model

相关spectral branch使用Raymond-Smith halo plasma，置于photoelectric absorption之后，并与local/unabsorbed foreground、extragalactic continuum、instrumental lines和soft-proton背景共同拟合。Figure 3转换保持每条视线自己的temperature和N_H。

The relevant spectral branch uses an absorbed Raymond-Smith halo plasma fitted together with local/unabsorbed foreground, extragalactic continuum, instrumental lines, and soft-proton background. The Figure 3 transfer preserves each sightline's own temperature and N_H.

原文结果

Published results

论文给出的intrinsic 0.5-2.0 keV halo brightness在不同视线间有宽分布；Figure 3不把这种population spread解释为M31方向测量误差。

The paper reports a broad sightline-to-sightline distribution of intrinsic 0.5-2.0 keV halo brightness. Figure 3 does not reinterpret that population spread as a measurement error toward M31.

如何进入M31 Figure 3

Transfer into M31 Figure 3

对86条可转换detections逐条计算XSraymond*XSphabs的absorbed/intrinsic 0.5-2.0 keV比例，使用published temperature、LAB N_H、angr abundance和bcmc cross-sections，再乘各自intrinsic brightness。最终取转换后population median=0.384610、IQR=0.273548-0.549082、p16-p84=0.246097-0.690362。此步骤产生的是非同向population comparator，不是M31 projection。

For each of 86 convertible detections, the absorbed-to-intrinsic 0.5-2.0 keV ratio is evaluated with XSraymond*XSphabs using the published temperature and LAB N_H plus angr abundances and bcmc cross-sections, then applied to its intrinsic brightness. The converted population has median 0.384610, IQR 0.273548-0.549082, and p16-p84 0.246097-0.690362. This is a non-local population comparator, not an M31 projection.

假设与解释边界

Assumptions and boundaries

样本不覆盖M31低纬方向，也没有可在M31足迹逐场求值的3D density posterior。population IQR/percentiles不能称为target-direction confidence interval。

The sample does not cover the lower-latitude M31 direction and supplies no 3D density posterior that can be evaluated over the M31 footprint. Population IQR/percentiles are not a target-direction confidence interval.

本论文对应的Figure 3数据点

Figure 3 points from this study

Primary-source证据地图

Primary-source evidence map

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