{
  "schema_version": 1,
  "figure_band": "absorbed 0.5-2.0 keV",
  "figure_unit": "1e-15 erg cm-2 s-1 arcmin-2",
  "value_semantics": {
    "figure_central": "Frozen ledger audit summary; normally the plotted marker, except when an explicit plotted_central is present.",
    "plotted_central": "Actual Figure 3 marker when it intentionally differs from figure_central; currently used by the Locatelli all-field estimator."
  },
  "studies": [
    {
      "study_id": "henley-shelton-2013",
      "kind": "mw-observation",
      "slug": "henley-shelton-2013",
      "evidence_class": "high-latitude population context",
      "citation": {
        "title": "An XMM-Newton Survey of the Soft X-Ray Background. III. The Galactic Halo X-Ray Emission",
        "authors": "David B. Henley and Robin L. Shelton",
        "year": 2013,
        "journal": "The Astrophysical Journal 773, 92",
        "doi": "10.1088/0004-637X/773/2/92",
        "arxiv": "1306.2312",
        "source_snapshot": {"version": "arXiv:1306.2312v1", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "a8f9dc5442d2a8b339f57655ddc03a041a89e724e87dd87dba7724cb49e3ac4d"},
        "primary_urls": {
          "publisher": "https://iopscience.iop.org/article/10.1088/0004-637X/773/2/92",
          "pdf": "https://iopscience.iop.org/article/10.1088/0004-637X/773/2/92/pdf",
          "arxiv": "https://arxiv.org/abs/1306.2312v1",
          "catalog": "https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJ/773/92"
        }
      },
      "overview": {
        "zh": "这是一项XMM-Newton高银纬软X射线背景视线样本研究。Figure 3使用它描述不同高纬视线上的Galactic-halo brightness population，而不是把其median当成M31方向的局部前景测量。",
        "en": "This is an XMM-Newton high-Galactic-latitude survey of soft-X-ray-background sightlines. Figure 3 uses it as a population distribution of Galactic-halo brightness, not as a local foreground measurement toward M31."
      },
      "instrument": {
        "zh": "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。",
        "en": "XMM-Newton EPIC-MOS diffuse-background spectra, with archival sightlines processed uniformly, point sources removed, and instrumental plus astrophysical backgrounds modeled explicitly."
      },
      "sightlines": {
        "zh": "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。",
        "en": "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."
      },
      "measurement": {
        "zh": "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。",
        "en": "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."
      },
      "model": {
        "zh": "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。",
        "en": "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."
      },
      "published_results": {
        "zh": "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。",
        "en": "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."
      },
      "transfer_to_m31": {
        "zh": "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。",
        "en": "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."
      },
      "limitations": {
        "zh": "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。",
        "en": "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."
      },
      "evidence": [
        {"location": "Abstract and sample definition", "url": "https://iopscience.iop.org/article/10.1088/0004-637X/773/2/92", "claim": "High-latitude XMM-Newton halo survey and sample scope."},
        {"location": "VizieR J/ApJ/773/92 main table", "url": "https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJ/773/92", "claim": "Per-sightline temperatures, brightnesses, flags, and N_H values."},
        {"location": "Methods and spectral model", "url": "https://arxiv.org/abs/1306.2312v1", "claim": "Raymond-Smith halo plus foreground/background model and intrinsic 0.5-2.0 keV convention."}
      ],
      "point_ids": ["henley_shelton2013_high_latitude_population"]
    },
    {
      "study_id": "ponti-efeds-2023",
      "kind": "mw-observation",
      "slug": "ponti-efeds-2023",
      "evidence_class": "distant-sky fixed-scenario comparator",
      "citation": {
        "title": "Abundance and temperature of the outer hot circumgalactic medium",
        "authors": "G. Ponti et al.",
        "year": 2023,
        "journal": "Astronomy & Astrophysics 674, A195",
        "doi": "10.1051/0004-6361/202243992",
        "arxiv": "2210.03133",
        "source_snapshot": {"version": "arXiv:2210.03133v1", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "a7d0a29bd8b54a24b0ba42063ffd8add4c3863d3a7d6347e62fee3594a5bc06b"},
        "primary_urls": {
          "publisher": "https://www.aanda.org/articles/aa/full_html/2023/06/aa43992-22/aa43992-22.html",
          "table4": "https://www.aanda.org/articles/aa/full_html/2023/06/aa43992-22/T4.html",
          "table2": "https://www.aanda.org/articles/aa/full_html/2023/06/aa43992-22/T2.html",
          "pdf": "https://www.aanda.org/articles/aa/pdf/2023/06/aa43992-22.pdf",
          "arxiv": "https://arxiv.org/abs/2210.03133v1"
        }
      },
      "overview": {
        "zh": "Ponti et al.利用eFEDS深场分解外层MW hot-CGM emission，并显式比较negligible与high-SWCX两种固定情景。Figure 3保留两个情景点，不构造central value。",
        "en": "Ponti et al. decompose outer Milky-Way hot-CGM emission in the eFEDS field and explicitly compare fixed negligible- and high-SWCX scenarios. Figure 3 retains both scenario points without inventing a central value."
      },
      "instrument": {
        "zh": "eROSITA/eFEDS X-ray survey spectroscopy over约107.5 deg2；分析利用不同survey epochs检查SWCX，并联合建模热前景、CGM、CXB和吸收。",
        "en": "eROSITA/eFEDS X-ray survey spectroscopy over about 107.5 deg2, using different survey epochs to diagnose SWCX and jointly modeling thermal foregrounds, CGM, CXB, and absorption."
      },
      "sightlines": {
        "zh": "eFEDS位于约l=220-235 deg、b=20-40 deg的西侧天空，离M31超过105 deg。它是一个远方sky comparator，不是M31足迹测量或可局部化到M31的空间模型。",
        "en": "eFEDS lies in the western sky near l=220-235 deg and b=20-40 deg, more than 105 deg from M31. It is a distant-sky comparator, not an M31-footprint measurement or a spatial model localizable to M31."
      },
      "measurement": {
        "zh": "Table 4给出best-fitting CGM component surface brightness：0.3-0.6、0.6-2.0和0.3-2.0 keV，单位1e-13 erg cm-2 s-1 deg-2。左右列分别是negligible/high SWCX固定模型。",
        "en": "Table 4 reports best-fitting CGM-component surface brightness in 0.3-0.6, 0.6-2.0, and 0.3-2.0 keV, in 1e-13 erg cm-2 s-1 deg-2. Left/right columns are fixed negligible/high SWCX models."
      },
      "model": {
        "zh": "模型包含unabsorbed Local Hot Bubble、吸收后的CGM thermal component、CXB和SWCX情景；neutral-column distribution用disnht。PDF/arXiv给出sigma=0.117，而publisher HTML Eq.1显示0.177；转换采用PDF/arXiv的0.117。",
        "en": "The model includes an unabsorbed Local Hot Bubble, absorbed CGM thermal component, CXB, and SWCX scenarios, with disnht for the neutral-column distribution. The PDF/arXiv give sigma=0.117 while publisher HTML Eq. 1 shows 0.177; the transfer follows the PDF/arXiv value 0.117."
      },
      "published_results": {
        "zh": "Table 4的CGM值为negligible/high SWCX：0.3-0.6 keV 24.1/15.6，0.6-2.0 keV 5.6/4.9。两列是系统情景，不是同一参数的置信区间。",
        "en": "Table 4 gives CGM values for negligible/high SWCX of 24.1/15.6 in 0.3-0.6 keV and 5.6/4.9 in 0.6-2.0 keV. The two columns are systematic scenarios, not a confidence interval on one parameter."
      },
      "transfer_to_m31": {
        "zh": "对每个SWCX情景，用published kT/Z的Lodders APEC和lognormal-N_H quadrature计算F(0.5-0.6)/F(0.3-0.6)，乘Table 4 soft-bin flux后与published 0.6-2.0 flux相加，再换算deg2到arcmin2。得到high/negligible SWCX=0.291208/0.406510。这里没有M31几何transfer，只有common-band重建。",
        "en": "For each SWCX scenario, a Lodders APEC model at the published kT/Z plus lognormal-N_H quadrature gives F(0.5-0.6)/F(0.3-0.6). That fraction of the Table 4 soft-bin flux is added to the published 0.6-2.0 flux and deg2 is converted to arcmin2, yielding high/negligible SWCX values of 0.291208/0.406510. This is a common-band reconstruction, not an M31 geometry transfer."
      },
      "limitations": {
        "zh": "eFEDS与M31不共线；两个点的连接线只表示固定SWCX情景范围。Table 4没有把该值定义为M31方向的absorbed prior。",
        "en": "eFEDS is not co-directional with M31. The connector between its two points only groups fixed SWCX scenarios. Table 4 does not define an absorbed prior toward M31."
      },
      "evidence": [
        {"location": "Table 4", "url": "https://www.aanda.org/articles/aa/full_html/2023/06/aa43992-22/T4.html", "claim": "Disjoint CGM component fluxes in the two SWCX scenarios."},
        {"location": "Table 2 and Sect. 5.4", "url": "https://www.aanda.org/articles/aa/full_html/2023/06/aa43992-22/T2.html", "claim": "Negligible/high SWCX scenario definitions and model components."},
        {"location": "Version-of-record PDF Eq. 1", "url": "https://www.aanda.org/articles/aa/pdf/2023/06/aa43992-22.pdf", "claim": "disnht width sigma=0.117 used by the executable reconstruction."}
      ],
      "point_ids": ["ponti2023_efeds_negligible_swcx", "ponti2023_efeds_high_swcx"]
    },
    {
      "study_id": "ueda-2022",
      "kind": "mw-observation",
      "slug": "ueda-2022",
      "evidence_class": "in-domain directional footprint model",
      "citation": {
        "title": "The soft X-ray background with Suzaku. I. Milky Way halo",
        "authors": "Masaki Ueda et al.",
        "year": 2022,
        "journal": "Publications of the Astronomical Society of Japan 74, 1396-1414",
        "doi": "10.1093/pasj/psac077",
        "arxiv": "2209.01698",
        "source_snapshot": {"version": "arXiv:2209.01698v1", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "dacbf81e477abc660781654a7781fbe035ba5027b0885556d8af0d3162e350a6"},
        "primary_urls": {
          "publisher": "https://academic.oup.com/pasj/article/74/6/1396/6761006",
          "table3": "https://academic.oup.com/view-large/431544714",
          "pdf": "https://academic.oup.com/pasj/article-pdf/74/6/1396/54646119/psac077.pdf",
          "arxiv": "https://arxiv.org/abs/2209.01698v1"
        }
      },
      "overview": {
        "zh": "Ueda et al.用Suzaku软X射线背景spectra拟合约0.22 keV Milky-Way-halo component，并给出可沿任意内部视线积分的指数disk density model。M31十四场位于采用fit row的角域内。",
        "en": "Ueda et al. use Suzaku soft-X-ray-background spectra to fit an approximately 0.22 keV Milky-Way-halo component and publish an exponential disk density model that can be integrated along internal sightlines. All fourteen M31 fields lie within the angular domain of the adopted fit row."
      },
      "instrument": {
        "zh": "Suzaku XIS archival diffuse-background observations，spectral fitting区分Local Bubble/SWCX、约0.22 keV MWH、约0.8 keV额外component和CXB。Figure 3只转移约0.22 keV MWH disk。",
        "en": "Archival Suzaku XIS diffuse-background observations, with spectral fits separating Local Bubble/SWCX, the approximately 0.22 keV MWH, an additional approximately 0.8 keV component, and CXB. Figure 3 transfers only the approximately 0.22 keV MWH disk."
      },
      "sightlines": {
        "zh": "130场parent sample覆盖75<l<285 deg、|b|>15 deg。25场|b|>35 deg high-latitude uniform subset是另一个selection。本文采用Table 3的2005-2009、|l|>105 deg、N=36 row；M31十四场l约119.5-122.3 deg且|b|约19.9-23.2 deg，位于该角域内但不在25场uniform subset。",
        "en": "The 130-field parent sample covers 75<l<285 deg and |b|>15 deg. The 25-field high-latitude uniform subset at |b|>35 deg is a separate selection. We adopt the Table 3 row for 2005-2009, |l|>105 deg, N=36; the fourteen M31 fields at l about 119.5-122.3 deg and |b| about 19.9-23.2 deg are inside that angular domain but not the 25-field uniform subset."
      },
      "measurement": {
        "zh": "native quantity是通过absorbed phabs thermal spectrum推断的MWH emission measure EM=integral n_e n_H ds，不是直接观测的broadband surface brightness。",
        "en": "The native quantity is MWH emission measure, EM=integral n_e n_H ds, inferred through an absorbed phabs thermal spectrum rather than a directly observed broadband surface brightness."
      },
      "model": {
        "zh": "Table 3 adopted row给n_e0=(3.4+/-0.1)e-3 cm-3，固定R0=7.0 kpc、z0=2.7 kpc；disk law写作n=n0 exp(-R/R0) exp(-z/z0)。该row的chi2/dof=36/35。本项目有意采用这个N=36 disk-only row，而不是同一selection下统计量略优的disk+spherical composite row。",
        "en": "The adopted Table 3 row gives n_e0=(3.4+/-0.1)e-3 cm-3 with fixed R0=7.0 kpc and z0=2.7 kpc; the disk law is printed as n=n0 exp(-R/R0) exp(-z/z0). This row has chi2/dof=36/35. The project intentionally selects this N=36 disk-only row rather than the slightly better-fitting disk-plus-spherical composite row for the same selection."
      },
      "published_results": {
        "zh": "论文高纬uniform subset给出约kT=0.22 keV、EM约2e-3 cm-6 pc；Figure 3采用的空间normalization来自不同的Table 3 N=36 disk fit，不能把两项selection混写。",
        "en": "The high-latitude uniform subset yields approximately kT=0.22 keV and EM around 2e-3 cm-6 pc. The spatial normalization used in Figure 3 instead comes from the separate Table 3 N=36 disk fit; the two selections must not be conflated."
      },
      "transfer_to_m31": {
        "zh": "本项目补充midplane symmetry |z|、n_e/n_H=1.2、R_sun=8.2 kpc和内部observer LOS transform；逐场积分n_e n_H到M31十四场，再用Lodders APEC(kT=0.22,Z=1)*phabs(HI4PI)转换为absorbed 0.5-2.0。按观测total相同weights得到0.311904，footprint 0.289468-0.320667；只变化n0边际误差给0.272690-0.339807。",
        "en": "The project adds midplane symmetry |z|, n_e/n_H=1.2, R_sun=8.2 kpc, and an internal-observer LOS transform; it integrates n_e n_H through each of fourteen M31 fields and converts with Lodders APEC(kT=0.22,Z=1)*phabs(HI4PI) to absorbed 0.5-2.0. Using the same weights as the observed total gives 0.311904 with footprint 0.289468-0.320667; varying only the marginal n0 error gives 0.272690-0.339807."
      },
      "limitations": {
        "zh": "|z|、composition ratio、Solar radius和observer transform是本项目augmentations；footprint与n0 sensitivity不是joint posterior。约0.8 keV component未进入Figure 3。",
        "en": "The |z| symmetry, composition ratio, Solar radius, and observer transform are project augmentations. Footprint spread and n0 sensitivity are not a joint posterior. The approximately 0.8 keV component is omitted from Figure 3."
      },
      "evidence": [
        {"location": "Abstract and sample selection", "url": "https://academic.oup.com/pasj/article/74/6/1396/6761006", "claim": "Parent and high-latitude sample definitions plus thermal-component results."},
        {"location": "Table 3", "url": "https://academic.oup.com/view-large/431544714", "claim": "Adopted N=36 disk normalization, fixed scale lengths, and fit statistic."},
        {"location": "Equation 1 and adjacent text", "url": "https://arxiv.org/abs/2209.01698v1", "claim": "Published exponential disk law and EM definition."}
      ],
      "point_ids": ["ueda2022_suzaku_disk_m31_footprint"]
    },
    {
      "study_id": "kaaret-halosat-2020",
      "kind": "mw-observation",
      "slug": "kaaret-halosat-2020",
      "evidence_class": "out-of-domain directional extrapolation",
      "citation": {
        "title": "A disk-dominated and clumpy circumgalactic medium of the Milky Way seen in X-ray emission",
        "authors": "P. Kaaret et al.",
        "year": 2020,
        "journal": "Nature Astronomy 4, 1072-1077",
        "doi": "10.1038/s41550-020-01215-w",
        "arxiv": "2011.00126",
        "source_snapshot": {"version": "arXiv:2011.00126v1", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "f77e50a0d25cb168af70ef000219ac488fca3a881e0a0613ffc610077b1ead7e"},
        "primary_urls": {
          "publisher": "https://www.nature.com/articles/s41550-020-01215-w",
          "pdf": "https://www.nature.com/articles/s41550-020-01215-w.pdf",
          "arxiv": "https://arxiv.org/abs/2011.00126v1",
          "catalog": "https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/other/NatAs/4.1072"
        }
      },
      "overview": {
        "zh": "Kaaret et al.用HaloSat南天高纬EM分布比较disk与halo morphology，得到disk-dominated且需要patchiness的结论。Figure 3把最终empirical-disk+adiabatic-halo model域外外推到M31。",
        "en": "Kaaret et al. compare disk and halo morphologies using southern high-latitude HaloSat emission measures, finding disk-dominated emission with patchiness. Figure 3 extrapolates the final empirical-disk-plus-adiabatic-halo model outside its fitted domain to M31."
      },
      "instrument": {
        "zh": "HaloSat非成像软X射线CubeSat，采用silicon-drift detectors和宽视场；published morphology fit使用高纬场的单温APEC emission measures。",
        "en": "HaloSat is a non-imaging soft-X-ray CubeSat using silicon-drift detectors and a wide field of view; the published morphology fit uses one-temperature APEC emission measures from high-latitude fields."
      },
      "sightlines": {
        "zh": "density morphology只用73个b<-30 deg南天场。M31约b=-21.6 deg，十四场全部在domain外；最近fit field center距M31 17.70 deg，超过HaloSat约7 deg零响应半径。",
        "en": "The density morphology uses 73 southern fields at b<-30 deg. M31 near b=-21.6 deg places all fourteen fields outside the domain; the nearest fitted field center is 17.70 deg away, beyond HaloSat's approximately 7 deg zero-response radius."
      },
      "measurement": {
        "zh": "native data是每场单温APEC的EM与temperature，而不是M31方向flux。模型的published-fit convention通过catalog closure确定为integral(n_disk+n_halo)^2 ds。",
        "en": "The native data are per-field one-temperature APEC emission measures and temperatures, not M31-direction fluxes. Catalog closure identifies the published-fit convention as integral(n_disk+n_halo)^2 ds."
      },
      "model": {
        "zh": "empirical disk使用n0=0.0081 cm-3、z0=1.60 kpc及piecewise Sigma(R)；adiabatic halo是在NFW势中的Fang et al. polytrope，rho_V=4.8e-5 cm-3、R_s=21.7 kpc、C_V=12。composite fit chi2约71.7/70，patchiness sigma_p=3.4e-3 cm-6 pc。",
        "en": "The empirical disk uses n0=0.0081 cm-3, z0=1.60 kpc, and piecewise Sigma(R). The adiabatic halo is the Fang et al. polytrope in an NFW potential with rho_V=4.8e-5 cm-3, R_s=21.7 kpc, and C_V=12. The composite fit has chi2 about 71.7/70 and patchiness sigma_p=3.4e-3 cm-6 pc."
      },
      "published_results": {
        "zh": "论文主结论是soft X-ray emitting CGM在该南天样本中disk-dominated并且clumpy；composite final model用于patchiness与Figure 3 transfer。",
        "en": "The main conclusion is that the soft-X-ray-emitting CGM is disk dominated and clumpy in the southern sample; the composite final model is used for patchiness and the Figure 3 transfer."
      },
      "transfer_to_m31": {
        "zh": "本项目采用R_sun=8.0 kpc、|z|、0-260 kpc内部LOS，并按catalog-closed convention保留disk-halo cross term；因模型不预测M31方向temperature，补充sample median kT=0.225 keV、Z=0.3、Wilms/Verner TBabs及逐场HI4PI。得到all-field 0.565386、footprint 0.526442-0.577710、converted patchiness +/-0.165165；去cross term的structural check为0.438683。",
        "en": "The project adopts R_sun=8.0 kpc, |z|, and internal LOS integration from 0 to 260 kpc, retaining the disk-halo cross term under the catalog-closed convention. Because the model does not predict M31-direction temperature, it adds sample-median kT=0.225 keV, Z=0.3, Wilms/Verner TBabs, and field-specific HI4PI. The result is all-field 0.565386, footprint 0.526442-0.577710, and converted patchiness +/-0.165165; removing the cross term gives structural check 0.438683."
      },
      "limitations": {
        "zh": "这是低纬域外外推，不是HaloSat在M31方向的直接预测。论文没有说明fitted n的particle identity，因此不能额外乘n_e/n_H。M31附近archive target会混入M31弥散辐射，不能作为独立MW prior。",
        "en": "This is a lower-latitude out-of-domain extrapolation, not a direct HaloSat prediction toward M31. The paper does not identify the particle meaning of fitted n, so no extra n_e/n_H factor is justified. A nearby archive target would include M31 diffuse emission and is not an independent MW prior."
      },
      "evidence": [
        {"location": "Main text and Extended Data Fig. 4", "url": "https://www.nature.com/articles/s41550-020-01215-w", "claim": "Model inventory, fitted parameters, disk-dominated interpretation, and patchiness."},
        {"location": "CDS J/other/NatAs/4.1072", "url": "https://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/other/NatAs/4.1072", "claim": "The 73-field catalog used for fit-statistic and cross-term closure."},
        {"location": "Author arXiv source", "url": "https://arxiv.org/abs/2011.00126v1", "claim": "Southern-domain selection, geometry implementation clues, and source equations."}
      ],
      "point_ids": ["kaaret2020_halosat_disk_halo_m31_extrapolation"]
    },
    {
      "study_id": "locatelli-2024",
      "kind": "mw-observation",
      "slug": "locatelli-2024",
      "evidence_class": "western-half O VIII model extrapolated to the M31 footprint",
      "citation": {
        "title": "The warm-hot circumgalactic medium of the Milky Way as seen by eROSITA",
        "authors": "N. Locatelli et al.",
        "year": 2024,
        "journal": "Astronomy & Astrophysics 681, A78",
        "doi": "10.1051/0004-6361/202347061",
        "arxiv": "2310.10715",
        "source_snapshot": {"version": "arXiv:2310.10715v1", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "4a9220468bfabcf9eeeb464c7f93d9b87bf8f647798efc42a0fd4a5007537a6f"},
        "primary_urls": {
          "publisher": "https://www.aanda.org/articles/aa/full_html/2024/01/aa47061-23/aa47061-23.html",
          "table1": "https://www.aanda.org/articles/aa/full_html/2024/01/aa47061-23/T1.html",
          "pdf": "https://www.aanda.org/articles/aa/pdf/2024/01/aa47061-23.pdf",
          "arxiv": "https://arxiv.org/abs/2310.10715v1"
        }
      },
      "overview": {
        "zh": "Locatelli et al.用eROSITA O VIII line map拟合Milky-Way warm-hot CGM的spherical-halo与exponential-disk几何。Figure 3的橙线不是论文表中的broadband flux，而是把named reference Combined beta=0.5 geometry转移到十四条M31视线。",
        "en": "Locatelli et al. fit spherical-halo and exponential-disk geometries to an eROSITA O VIII line map of the Milky-Way warm-hot CGM. The orange Figure 3 line is not a tabulated broadband flux; it transfers the named reference Combined beta=0.5 geometry through fourteen M31 sightlines."
      },
      "instrument": {
        "zh": "eROSITA eRASS1的eROSITA_DE western Galactic half O VIII narrow-band map；相关原始observable是0.614-0.694 keV line-band photon intensity，80 eV窗口近似eROSITA能量分辨率。",
        "en": "An O VIII narrow-band map of the eROSITA_DE western Galactic half from eROSITA eRASS1. The native observable is photon intensity in 0.614-0.694 keV; the 80 eV window approximates the eROSITA energy resolution."
      },
      "sightlines": {
        "zh": "论文拟合western half（约180<l<360 deg）的mid/high-|b| MW line map，并mask eROSITA bubbles及明亮extended structures；M31位于l约121、b约-21.6 deg，明确在native map域外。本项目从太阳内部位置把reference geometry外推到十四个M31 XMM pointing centers。",
        "en": "The paper fits the mid/high-|b| Milky-Way line map in the western half (roughly 180<l<360 deg), masking the eROSITA bubbles and bright extended structures. M31 at about l=121, b=-21.6 deg is explicitly outside that native map domain. This project extrapolates the reference geometry from the internal Solar position through fourteen M31 XMM pointing centers."
      },
      "measurement": {
        "zh": "native fit约束O VIII line intensity及其空间形态，不直接测量absorbed 0.5-2.0 keV energy surface brightness。",
        "en": "The native fit constrains O VIII line intensity and its spatial morphology, not absorbed 0.5-2.0 keV energy surface brightness."
      },
      "model": {
        "zh": "Figure 3采用论文指定的reference Combined beta=0.5：spherical n_h=C r^(-3 beta)加exponential n_d=n0 exp(-R/Rh) exp(-|z|/zh)，参数beta=0.5、C=0.046、n0=0.032 cm-3、Rh=6.2 kpc、zh=1.1 kpc、kT=0.15 keV、Z=0.1。发射实现为n_h^2+n_d^2，没有cross term。论文Eq. (7)的交叉项漏印path-length s而量纲不成立；项目按Miller & Bregman上游公式保留s。",
        "en": "Figure 3 uses the paper-designated reference Combined beta=0.5 model: spherical n_h=C r^(-3 beta) plus exponential n_d=n0 exp(-R/Rh) exp(-|z|/zh), with beta=0.5, C=0.046, n0=0.032 cm-3, Rh=6.2 kpc, zh=1.1 kpc, kT=0.15 keV, and Z=0.1. The emission implementation is n_h^2+n_d^2 without a cross term. The cross term printed in Eq. (7) omits the path-length s and is dimensionally invalid; the project retains s following the upstream Miller & Bregman formula."
      },
      "published_results": {
        "zh": "paper result是O VIII-constrained geometry及Table 1参数族。Table 1的single spherical fit给beta=0.26+/-0.01，而Sect. 4.3正文写beta=0.23；两种正式来源保留这一内部不一致，本registry采用Table 1值并明确记录冲突。论文没有发表M31方向absorbed broadband值，也没有发表足以构造joint posterior的参数covariance。",
        "en": "The paper result is an O VIII-constrained geometry and the Table 1 parameter family. Table 1 gives beta=0.26+/-0.01 for the single spherical fit, whereas Sect. 4.3 states beta=0.23; both formal sources retain this internal discrepancy, so the registry adopts the Table 1 value while recording the conflict. The paper does not publish absorbed broadband values toward M31 or the parameter covariance required for a joint posterior."
      },
      "transfer_to_m31": {
        "zh": "先积分n_h^2+n_d^2得到十四场EM和intrinsic O VIII 4.14-4.56 L.U.；用80 eV FWHM Gaussian匹配原map line-band emissivity；固定该O VIII normalization并转换到Z=0.3 target APEC，再用每场HI4PI full-screen phabs得到absorbed 0.5-2.0。与observed all-field相同weights给1.290382，footprint 1.157655-1.341463，North/South 1.295557/1.213445。",
        "en": "Integrating n_h^2+n_d^2 first gives fourteen-field EMs and intrinsic O VIII intensities of 4.14-4.56 L.U. An 80 eV FWHM Gaussian matches the map's line-band emissivity treatment. Holding that O VIII normalization fixed, the transfer uses a Z=0.3 target APEC model and field-specific HI4PI full-screen phabs to obtain absorbed 0.5-2.0. Using the same weights as the observed all-field total gives 1.290382, footprint 1.157655-1.341463, and North/South 1.295557/1.213445."
      },
      "limitations": {
        "zh": "M31方向处于western-half training map域外；line-to-broadband、target abundance、full-screen absorption和field weighting也均是本项目transfer。0.934302-1.574700只由published marginal errors作diagonal sensitivity propagation，不是credible interval。1.290超过observed total 0.965约0.326，表示named model+conversion tension，不是负M31 emission。",
        "en": "The M31 direction lies outside the western-half training map. The line-to-broadband bridge, target abundance, full-screen absorption, and field weighting are also project transfers. The 0.934302-1.574700 range is diagonal sensitivity propagation from published marginal errors, not a credible interval. The 1.290 value exceeds the observed total 0.965 by about 0.326, indicating named model-plus-conversion tension rather than negative M31 emission."
      },
      "evidence": [
        {"location": "Table 1", "url": "https://www.aanda.org/articles/aa/full_html/2024/01/aa47061-23/T1.html", "claim": "Reference Combined beta=0.5 parameters and marginal errors."},
        {"location": "Model and emissivity sections", "url": "https://www.aanda.org/articles/aa/full_html/2024/01/aa47061-23/aa47061-23.html", "claim": "O VIII line-map observable, density geometries, temperature/abundance, and reference-model identity."},
        {"location": "Version-of-record PDF", "url": "https://www.aanda.org/articles/aa/pdf/2024/01/aa47061-23.pdf", "claim": "Figure/table identity and O VIII map processing used by the response-matched transfer."}
      ],
      "point_ids": ["locatelli2024_reference_beta0p5_m31_footprint"]
    },
    {
      "study_id": "zhang-2024",
      "kind": "external-galaxy-stack",
      "slug": "zhang-2024",
      "evidence_class": "external-galaxy population-stack template",
      "citation": {
        "title": "The hot circumgalactic medium in the eROSITA All-Sky Survey. I. X-ray surface brightness profiles",
        "authors": "Yi Zhang et al.",
        "year": 2024,
        "journal": "Astronomy & Astrophysics 690, A267",
        "doi": "10.1051/0004-6361/202449412",
        "arxiv": "2401.17308",
        "source_snapshot": {"version": "arXiv:2401.17308v3", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "4f96964adc92f9558da6acd9771fc0f612005f3b9eb3712d8e9c6ac89ca39b7c"},
        "primary_urls": {
          "publisher": "https://www.aanda.org/articles/aa/full_html/2024/10/aa49412-24/aa49412-24.html",
          "pdf": "https://www.aanda.org/articles/aa/pdf/2024/10/aa49412-24.pdf",
          "arxiv": "https://arxiv.org/abs/2401.17308v3"
        }
      },
      "overview": {
        "zh": "Zhang et al.把大量central galaxies的eROSITA photons按stellar-mass bins堆叠，统计分离hot-CGM、unresolved AGN/XRB/satellites与PSF。Figure 3使用M31-mass bin的population profile作为条件模板，不是M31本身的观测。",
        "en": "Zhang et al. stack eROSITA photons around large samples of central galaxies in stellar-mass bins, statistically separating hot CGM, unresolved AGN/XRB/satellites, and the PSF. Figure 3 uses the M31-mass-bin population profile as a conditional template, not an observation of M31 itself."
      },
      "instrument": {
        "zh": "eROSITA eRASS:4 stacking，使用rest-frame、absorption-corrected 0.5-2.0 keV luminosity surface-density profiles，并对redshift-dependent PSF和detected sources进行处理。",
        "en": "eROSITA eRASS:4 stacking of rest-frame, absorption-corrected 0.5-2.0 keV luminosity-surface-density profiles, including redshift-dependent PSF treatment and detected-source masking."
      },
      "sightlines": {
        "zh": "不是一条MW内部LOS，而是约26099个11.0<log(M*/Msun)<11.25 central galaxies的外部observer projected stacks；median z约0.12、median M*约1.3e11 Msun、median log M200m约12.7。M31-mass只按stellar mass命名，不保证morphology、SFR或halo mass完全等同M31。",
        "en": "This is not an internal-Milky-Way LOS but an external-observer projected stack of about 26,099 central galaxies with 11.0<log(M*/Msun)<11.25, median z about 0.12, median M* about 1.3e11 Msun, and median log M200m about 12.7. The label M31-mass is based on stellar mass alone and does not guarantee matched morphology, SFR, or halo mass."
      },
      "measurement": {
        "zh": "native profile是erg s-1 kpc-2的intrinsic/rest-frame 0.5-2.0 keV luminosity surface density；hot-CGM residual来自多component statistical decomposition。",
        "en": "The native profile is intrinsic/rest-frame 0.5-2.0 keV luminosity surface density in erg s-1 kpc-2; the hot-CGM residual comes from a multi-component statistical decomposition."
      },
      "model": {
        "zh": "hot-CGM radial profile用projected beta law S_X(R)=S_X0[1+(R/r_c)^2]^(-3 beta+1/2)。M31-mass median参数为log S_X0=37.1、r_c=4 kpc、beta=0.37；Figure 3采用一个nominal median profile，不把S_X0、r_c、beta的独立marginal ranges伪装成M31 prior。",
        "en": "The hot-CGM radial profile uses the projected beta law S_X(R)=S_X0[1+(R/r_c)^2]^(-3 beta+1/2). The M31-mass median parameters are log S_X0=37.1, r_c=4 kpc, and beta=0.37. Figure 3 uses one nominal median profile and does not turn independent marginal ranges of S_X0, r_c, and beta into an M31 prior."
      },
      "published_results": {
        "zh": "M31-mass bin的hot-CGM residual在Rvir内约3.9 sigma；paper给出shallow beta约0.37并说明population profile。Figure 3选取20 kpc characteristic value。",
        "en": "The M31-mass bin hot-CGM residual is detected at about 3.9 sigma within Rvir. The paper reports a shallow beta near 0.37 and a population profile; Figure 3 samples a characteristic value at 20 kpc."
      },
      "transfer_to_m31": {
        "zh": "先在20 kpc读取/计算nominal luminosity surface density 1.725299e36 erg s-1 kpc-2；对resolved surface brightness，distance因angular area与flux的D^-2相消。再用v19 thermal template将intrinsic luminosity-density convention转为M31视线的absorbed angular surface brightness，得到Figure 3的0.828454。",
        "en": "The nominal luminosity surface density at 20 kpc is first evaluated as 1.725299e36 erg s-1 kpc-2. For resolved surface brightness, distance cancels between angular area and flux D^-2. A v19 thermal template then converts the intrinsic luminosity-density convention to absorbed angular surface brightness along the M31 sightline, giving Figure 3 value 0.828454."
      },
      "limitations": {
        "zh": "population stack不是M31 measurement；mass label只匹配stellar-mass bin。转换使用单一v19 APEC spectrum而不是stack的完整multiphase distribution；beta参数covariance不可用。",
        "en": "The population stack is not an M31 measurement, and the mass label only matches a stellar-mass bin. The transfer uses one v19 APEC spectrum rather than a full multiphase distribution, and beta-parameter covariance is unavailable."
      },
      "evidence": [
        {"location": "Sample table and selection", "url": "https://www.aanda.org/articles/aa/full_html/2024/10/aa49412-24/aa49412-24.html", "claim": "M31-mass stellar bin, sample size, redshift, and halo-mass distribution."},
        {"location": "Surface-brightness and component-model methods", "url": "https://arxiv.org/abs/2401.17308v3", "claim": "eRASS:4 stacking, band/frame, PSF, source decomposition, and beta profile."},
        {"location": "M31-mass profile figure and fit table", "url": "https://www.aanda.org/articles/aa/pdf/2024/10/aa49412-24.pdf", "claim": "Profile normalization, beta-fit result, and hot-CGM significance."}
      ],
      "point_ids": ["zhang2024_m31_mass_nominal_20kpc"]
    },
    {
      "study_id": "grayson-2025",
      "kind": "simulation",
      "slug": "grayson-2025",
      "evidence_class": "simulation profile comparison",
      "citation": {
        "title": "The Hot Circumgalactic Medium in Stacked X-Rays: Observations versus Simulations",
        "authors": "Skylar Grayson et al.",
        "year": 2025,
        "journal": "The Astrophysical Journal 994, 89",
        "doi": "10.3847/1538-4357/ae100f",
        "arxiv": "2506.09123",
        "source_snapshot": {"version": "arXiv:2506.09123v2", "retrieved_utc": "2026-07-15T10:49:33Z", "sha256": "2b8c4d0a075581e9d9203e7c4d548c62bd7ce7e0859e38f899823392a1e4c470"},
        "primary_urls": {
          "publisher": "https://iopscience.iop.org/article/10.3847/1538-4357/ae100f",
          "pdf": "https://iopscience.iop.org/article/10.3847/1538-4357/ae100f/pdf",
          "arxiv": "https://arxiv.org/abs/2506.09123v2"
        }
      },
      "overview": {
        "zh": "Grayson et al.把eROSITA stacked profiles与EAGLE和SIMBA的synthetic X-ray profiles比较，包含标准、强AGN heating及NoAGN variants。Figure 3把M31-mass stellar bin的10-30 kpc simulation bands逐个作为条件模板。",
        "en": "Grayson et al. compare eROSITA stacked profiles with synthetic X-ray profiles from EAGLE and SIMBA, including standard, stronger-AGN-heating, and NoAGN variants. Figure 3 uses each 10-30 kpc simulation band in the M31-mass stellar bin as a separate conditional template."
      },
      "instrument": {
        "zh": "simulation结果不是望远镜直接观测。pyXSIM按gas temperature/metallicity/density以CIE APEC Monte Carlo生成2 Mpc内photons与LOS Doppler shifts；SOXS再用SIXTE提供的PSF/ARF/RMF分别模拟eROSITA七个mirror assemblies并stack。使用z=0.1 simulation snapshots，每个synthetic observation从对应observed sample随机赋redshift并采用1000 ks；因比较对象已cleaned/background-subtracted，不加foreground/background。",
        "en": "The simulation results are not direct telescope observations. pyXSIM Monte Carlo samples CIE APEC photons within 2 Mpc from gas temperature, metallicity, and density and applies line-of-sight Doppler shifts. SOXS then uses SIXTE PSF/ARF/RMF files to simulate and stack the seven eROSITA mirror assemblies. The analysis uses z=0.1 simulation snapshots, assigns each synthetic observation a redshift drawn from the corresponding observed sample, and adopts 1000 ks; no foreground/background is added because the comparator is already cleaned and background-subtracted."
      },
      "sightlines": {
        "zh": "每个simulation galaxy沿x、y、z三方向生成external-observer LOS projections后再stack，不是一条真实M31 LOS。Figure 3采用11<log(M*/Msun)<11.25 bin和projected physical 10-30 kpc annulus；论文没有把这些synthetic LOS重新放到M31 sky coordinates或穿过MW absorption。",
        "en": "Each simulated galaxy is projected along the x, y, and z directions and stacked as external-observer sightlines; none is a real M31 sightline. Figure 3 adopts the 11<log(M*/Msun)<11.25 bin and projected physical 10-30 kpc annulus. The paper does not place these synthetic sightlines at M31 sky coordinates or pass them through Milky-Way absorption."
      },
      "measurement": {
        "zh": "native plotted quantity是simulation的intrinsic X-ray luminosity surface density，Figure 7给各model line与spread。Figure 7意图与Zhang的0.5-2.0 keV profile比较，邻近Figure 6也把soft X-ray定义为0.5-2.0 keV；但profile methods/caption没有显式闭合Figure 7的event-energy cut或frame。当前数值由author arXiv figure在校准log axes和RGB后digitize。",
        "en": "The native plotted quantity is simulated intrinsic X-ray luminosity surface density, with Figure 7 showing model lines and spreads. Figure 7 is intended to match the Zhang 0.5-2.0 keV profiles, and adjacent Figure 6 defines soft X-rays as 0.5-2.0 keV, but the profile methods/caption do not explicitly close the Figure 7 event-energy cut or frame. Current values are digitized from the author arXiv figure using calibrated log axes and exact RGB values."
      },
      "model": {
        "zh": "EAGLE Ref-L050N0752用single-mode thermal AGN feedback、DeltaT_AGN=10^8.5 K；EAGLE-AGNdT9提高到10^9 K并改变accretion parameterization；EAGLE-NoAGN关闭AGN feedback。SIMBA标准模型包含high-Eddington kinetic wind、low-Eddington jet及相关X-ray mode；SIMBA-NoAGN全部关闭。五者是不同subgrid physics predictions，不是同一measurement的statistical error models。",
        "en": "EAGLE Ref-L050N0752 uses single-mode thermal AGN feedback with DeltaT_AGN=10^8.5 K; EAGLE-AGNdT9 raises this to 10^9 K and modifies the accretion parameterization; EAGLE-NoAGN disables AGN feedback. Fiducial SIMBA includes a high-Eddington kinetic wind, a low-Eddington jet, and associated X-ray mode; SIMBA-NoAGN disables AGN feedback. These are distinct subgrid-physics predictions, not statistical-error models for one measurement."
      },
      "mass_radius_scaling": {
        "zh": "原文没有给一条可直接把任意galaxy mass连续缩放到M31的analytic S_X-M relation。Figure 7按stellar mass分bin后显示：NoAGN在各mass bins的inner profile通常更亮；log M*<11.25时inner CGM的SIMBA显著亮于EAGLE，而最高mass时两套fiducial profiles更接近。作者先在0.1 dex stellar-mass cells重采样simulation，使其匹配Zhang observed stellar-mass distribution；本项目随后直接选择11<log(M*/Msun)<11.25、同时限制12<log(M200c/Msun)<14的M31-mass panel。halo-mass distribution没有与观测强制匹配。radius也不做R/R200重标度：Figure 3读取原文physical 10-30 kpc bin。",
        "en": "The paper does not provide an analytic S_X-mass relation that continuously rescales an arbitrary galaxy to M31. Across the stellar-mass bins in Figure 7, NoAGN runs are generally brighter in the inner profile; below log M*=11.25, SIMBA is substantially brighter than EAGLE in the inner CGM, while the two fiducial profiles converge at the highest masses. The paper resamples each simulation in 0.1 dex stellar-mass cells to match the observed Zhang stellar-mass distribution; this project then directly selects the M31-mass panel, 11<log(M*/Msun)<11.25 with 12<log(M200c/Msun)<14. The halo-mass distribution is not forced to match the observations. Radius is not rescaled by R/R200 either: Figure 3 reads the published physical 10-30 kpc bin."
      },
      "published_results": {
        "zh": "Figure 7显示在M31-mass bin与10-30 kpc内，NoAGN尤其SIMBA-NoAGN显著提高soft-X-ray brightness；不同feedback prescriptions给出数量级差异。",
        "en": "Figure 7 shows that within the M31-mass bin and 10-30 kpc, NoAGN models, especially SIMBA-NoAGN, strongly increase soft-X-ray brightness; different feedback prescriptions span orders of magnitude."
      },
      "transfer_to_m31": {
        "zh": "每个model从Figure 7 digitize 10-30 kpc intrinsic luminosity-density central/spread；使用同一distance-cancel surface-brightness conversion和v19 APEC absorption bridge得到Figure 3 values。五个points保持离散，不插值成M31 radial curves。",
        "en": "For each model, the central value and spread of intrinsic luminosity density in 10-30 kpc are digitized from Figure 7. The same distance-cancel surface-brightness conversion and v19 APEC absorption bridge give the Figure 3 values. The five points remain discrete and are never interpolated into M31 radial curves."
      },
      "limitations": {
        "zh": "转换对所有simulation采用单一v19 APEC spectrum，而非各模拟自身multiphase spectra。Figure 7范围是non-resampled galaxies的digitized bootstrap envelope，但论文没有说明confidence level，不能称为95% confidence interval。synthetic profiles已在随机赋予的观测redshifts下经过eROSITA PSF/response；单位转换不会把它们变成M31/XMM空间响应。stellar-mass matching不保证M31 halo mass、SFR、morphology或environment完全匹配。论文明确指出两个NoAGN runs不能再现galaxy stellar-mass function或stellar-halo mass relation，因此只能用作feedback sensitivity experiments。",
        "en": "The transfer applies one v19 APEC spectrum to all simulations rather than each simulation's multiphase spectrum. The Figure 7 ranges are digitized bootstrap envelopes for the non-resampled galaxies, but the confidence level is not stated and they are not a 95% confidence interval. The synthetic profiles are already convolved with the eROSITA PSF/response at randomly assigned observed redshifts; a unit conversion does not turn them into an M31/XMM spatial response. Stellar-mass matching does not guarantee matched M31 halo mass, SFR, morphology, or environment. The paper explicitly notes that the two NoAGN runs fail to reproduce the galaxy stellar-mass function or stellar-to-halo mass relation, so they are feedback-sensitivity experiments rather than realistic universes."
      },
      "evidence": [
        {"location": "Figure 7", "url": "https://arxiv.org/abs/2506.09123v2", "claim": "M31-mass 10-30 kpc profiles for five simulation variants."},
        {"location": "Sections 3.1-3.2, Equations 5-6", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/ae100f", "claim": "EAGLE/SIMBA samples, pyXSIM/APEC emissivity, SOXS/SIXTE eROSITA response projection, mass bins, and stacking."},
        {"location": "Discussion and model comparison", "url": "https://iopscience.iop.org/article/10.3847/1538-4357/ae100f/pdf", "claim": "Mass/radius behavior and physical interpretation of feedback-dependent profiles."}
      ],
      "point_ids": ["grayson2025_eagle_agndt9", "grayson2025_eagle", "grayson2025_eagle_noagn", "grayson2025_simba", "grayson2025_simba_noagn"]
    }
  ],
  "points": [
    {
      "prior_id": "henley_shelton2013_high_latitude_population",
      "study_id": "henley-shelton-2013",
      "slug": "henley-shelton2013-high-latitude-population",
      "doi": "10.1088/0004-637X/773/2/92",
      "figure_label": "H&S13 population median",
      "figure_central": 0.38461005704507567,
      "figure_low": 0.27354775115143726,
      "figure_high": 0.5490818824107443,
      "native_input": {"zh": "86条有唯一LAB N_H的intrinsic 0.5-2.0 keV halo detections。", "en": "Eighty-six intrinsic 0.5-2.0 keV halo detections with unique LAB N_H."},
      "transfer_summary": {"zh": "逐视线Raymond-Smith temperature和N_H吸收转换后取median/IQR。", "en": "Apply a sightline-specific Raymond-Smith temperature and N_H absorption conversion, then take the median/IQR."},
      "transfer_steps": [
        {"zh": "从VizieR J/ApJ/773/92读取有halo detection且有唯一LAB N_H的86条视线；不使用原论文只作population headline的固定0.5--7范围。", "en": "Read the 86 detected-halo sightlines with unique LAB N_H from VizieR J/ApJ/773/92; do not use the paper's fixed 0.5--7 population headline as the plotted interval."},
        {"zh": "逐视线用published Raymond-Smith temperature、LAB N_H、angr abundance与bcmc cross-sections，将intrinsic 0.5--2 flux重算为absorbed 0.5--2。", "en": "For every sightline, use its published Raymond-Smith temperature, LAB N_H, angr abundances, and bcmc cross-sections to recompute absorbed 0.5--2 flux from the intrinsic value.", "formula": "S_abs,i = S_intr,i × T_0.5-2(kT_i, N_H,i)"},
        {"zh": "把deg^-2除以3600变成arcmin^-2；Figure 3画86个转换值的median与IQR，p16--p84只作context。", "en": "Divide deg^-2 by 3600 to obtain arcmin^-2; Figure 3 plots the median and IQR of the 86 converted values, with p16--p84 retained only as context.", "formula": "S_fig = S_abs / 3600 / 10^-15"}
      ],
      "interpretation": {"zh": "高纬population context；不是M31方向prior。", "en": "High-latitude population context, not a prior toward M31."},
      "assumptions": [{"zh": "使用angr abundance与bcmc cross-sections复现原spectral convention。", "en": "Use angr abundances and bcmc cross-sections to reproduce the native spectral convention."}]
    },
    {
      "prior_id": "ponti2023_efeds_negligible_swcx",
      "study_id": "ponti-efeds-2023",
      "slug": "ponti2023-efeds-negligible-swcx",
      "doi": "10.1051/0004-6361/202243992",
      "figure_label": "eFEDS negligible-SWCX scenario",
      "figure_central": 0.4065102008977918,
      "figure_low": 0.4065102008977918,
      "figure_high": 0.4065102008977918,
      "native_input": {"zh": "Table 4 negligible-SWCX CGM flux：24.1(0.3-0.6)+5.6(0.6-2.0)。", "en": "Table 4 negligible-SWCX CGM flux: 24.1 (0.3-0.6) plus 5.6 (0.6-2.0)."},
      "transfer_summary": {"zh": "用published kT/Z模型截取0.5-0.6 soft-bin fraction，再加0.6-2.0。", "en": "Use the published kT/Z model to retain the 0.5-0.6 fraction of the soft bin, then add 0.6-2.0."},
      "transfer_steps": [
        {"zh": "固定当前Table 4 SWCX scenario，读取该scenario的CGM 0.3--0.6与0.6--2.0 flux；两个scenario不合并。", "en": "Fix the relevant Table 4 SWCX scenario and read its CGM 0.3--0.6 and 0.6--2.0 fluxes; never combine the two scenarios."},
        {"zh": "用该scenario published kT/Z的Lodders APEC，并对disnht lognormal N_H distribution做quadrature，求0.5--0.6占published 0.3--0.6 flux的fraction。", "en": "Use the scenario's published kT/Z Lodders APEC model and quadrature over the disnht lognormal N_H distribution to obtain the 0.5--0.6 fraction of the published 0.3--0.6 flux.", "formula": "F_0.5-2 = F_0.6-2 + f_0.5-0.6|0.3-0.6 × F_0.3-0.6"},
        {"zh": "把Table 4的10^-13 erg cm^-2 s^-1 deg^-2结果除以3600并换成Figure 3的10^-15 arcmin^-2单位；保留为fixed point。", "en": "Divide the Table 4 result in 10^-13 erg cm^-2 s^-1 deg^-2 by 3600 and convert to the Figure 3 10^-15 arcmin^-2 unit; retain it as one fixed point.", "formula": "S_fig = F_0.5-2 × 100 / 3600"}
      ],
      "interpretation": {"zh": "固定SWCX scenario；不是central estimate或CI。", "en": "A fixed SWCX scenario, not a central estimate or confidence interval."},
      "assumptions": [{"zh": "disnht sigma采用PDF/arXiv的0.117。", "en": "Use disnht sigma=0.117 from the PDF/arXiv."}]
    },
    {
      "prior_id": "ponti2023_efeds_high_swcx",
      "study_id": "ponti-efeds-2023",
      "slug": "ponti2023-efeds-high-swcx",
      "doi": "10.1051/0004-6361/202243992",
      "figure_label": "eFEDS high-SWCX scenario",
      "figure_central": 0.2912081083611119,
      "figure_low": 0.2912081083611119,
      "figure_high": 0.2912081083611119,
      "native_input": {"zh": "Table 4 high-SWCX CGM flux：15.6(0.3-0.6)+4.9(0.6-2.0)。", "en": "Table 4 high-SWCX CGM flux: 15.6 (0.3-0.6) plus 4.9 (0.6-2.0)."},
      "transfer_summary": {"zh": "用published kT/Z模型截取0.5-0.6 soft-bin fraction，再加0.6-2.0。", "en": "Use the published kT/Z model to retain the 0.5-0.6 fraction of the soft bin, then add 0.6-2.0."},
      "transfer_steps": [
        {"zh": "固定当前Table 4 SWCX scenario，读取该scenario的CGM 0.3--0.6与0.6--2.0 flux；两个scenario不合并。", "en": "Fix the relevant Table 4 SWCX scenario and read its CGM 0.3--0.6 and 0.6--2.0 fluxes; never combine the two scenarios."},
        {"zh": "用该scenario published kT/Z的Lodders APEC，并对disnht lognormal N_H distribution做quadrature，求0.5--0.6占published 0.3--0.6 flux的fraction。", "en": "Use the scenario's published kT/Z Lodders APEC model and quadrature over the disnht lognormal N_H distribution to obtain the 0.5--0.6 fraction of the published 0.3--0.6 flux.", "formula": "F_0.5-2 = F_0.6-2 + f_0.5-0.6|0.3-0.6 × F_0.3-0.6"},
        {"zh": "把Table 4的10^-13 erg cm^-2 s^-1 deg^-2结果除以3600并换成Figure 3的10^-15 arcmin^-2单位；保留为fixed point。", "en": "Divide the Table 4 result in 10^-13 erg cm^-2 s^-1 deg^-2 by 3600 and convert to the Figure 3 10^-15 arcmin^-2 unit; retain it as one fixed point.", "formula": "S_fig = F_0.5-2 × 100 / 3600"}
      ],
      "interpretation": {"zh": "固定SWCX scenario；与另一点的connector不是error bar。", "en": "A fixed SWCX scenario; its connector to the other point is not an error bar."},
      "assumptions": [{"zh": "eFEDS与M31相距超过105 deg，因此只作distant-sky comparator。", "en": "eFEDS is more than 105 deg from M31 and is only a distant-sky comparator."}]
    },
    {
      "prior_id": "ueda2022_suzaku_disk_m31_footprint",
      "study_id": "ueda-2022",
      "slug": "ueda2022-suzaku-disk-m31-footprint",
      "doi": "10.1093/pasj/psac077",
      "figure_label": "Ueda+22 disk projected to M31",
      "figure_central": 0.311904286700407,
      "figure_low": 0.2894675687845744,
      "figure_high": 0.3206666288460409,
      "native_input": {"zh": "Table 3 N=36 disk row：n_e0=3.4e-3 cm-3，R0=7.0 kpc，z0=2.7 kpc。", "en": "Table 3 N=36 disk row: n_e0=3.4e-3 cm-3, R0=7.0 kpc, z0=2.7 kpc."},
      "transfer_summary": {"zh": "逐M31视线积分n_e n_H并用kT=0.22 keV APEC、HI4PI phabs和observed weights。", "en": "Integrate n_e n_H through each M31 sightline and use kT=0.22 keV APEC, HI4PI phabs, and the observed weights."},
      "transfer_steps": [
        {"zh": "采用Ueda Table 3的2005--2009、|l|>105 deg、N=36 exponential disk fit：n_e0=3.4e-3 cm^-3、R0=7.0 kpc、z0=2.7 kpc。", "en": "Adopt the Ueda Table 3 exponential-disk fit for 2005--2009, |l|>105 deg, N=36: n_e0=3.4e-3 cm^-3, R0=7.0 kpc, z0=2.7 kpc."},
        {"zh": "从太阳位置沿每条M31 field sightline积分published density geometry；本项目明确补充对称|z|和n_H=n_e/1.2。", "en": "Integrate the published density geometry from the Solar position along each M31-field sightline; this project explicitly adds symmetric |z| and n_H=n_e/1.2.", "formula": "EM(l,b) = ∫ n_e(R,z) n_H(R,z) ds"},
        {"zh": "用kT=0.22 keV、Lodders APEC与field-specific HI4PI phabs将EM转为absorbed 0.5--2 brightness；以实测CGMsum statistical weights求all-field mean，14-field min--max只表示footprint。", "en": "Convert EM to absorbed 0.5--2 brightness with kT=0.22 keV, Lodders APEC, and field-specific HI4PI phabs; use the measured CGMsum statistical weights for the all-field mean, while the 14-field min--max represents footprint variation only."}
      ],
      "interpretation": {"zh": "fit-domain内的directional conditional model；footprint不是uncertainty。", "en": "An in-domain directional conditional model; the footprint is not an uncertainty interval."},
      "assumptions": [{"zh": "本项目增加|z|、n_e/n_H=1.2、R_sun=8.2 kpc。", "en": "The project adds |z|, n_e/n_H=1.2, and R_sun=8.2 kpc."}]
    },
    {
      "prior_id": "kaaret2020_halosat_disk_halo_m31_extrapolation",
      "study_id": "kaaret-halosat-2020",
      "slug": "kaaret2020-halosat-disk-halo-m31-extrapolation",
      "doi": "10.1038/s41550-020-01215-w",
      "figure_label": "HaloSat disk+halo extrapolation",
      "figure_central": 0.5653859652455517,
      "figure_low": 0.5264420313803833,
      "figure_high": 0.5777098778341332,
      "native_input": {"zh": "73个b<-30 deg HaloSat EM拟合的empirical disk+adiabatic halo。", "en": "Empirical-disk-plus-adiabatic-halo fit to 73 HaloSat EM fields at b<-30 deg."},
      "transfer_summary": {"zh": "按catalog-closed integral(n_d+n_h)^2投影M31，补充median kT、HI4PI和TBabs。", "en": "Project to M31 with the catalog-closed integral(n_d+n_h)^2 convention, adding median kT, HI4PI, and TBabs."},
      "transfer_steps": [
        {"zh": "采用paper joint fit的exponential disk加Fang et al. adiabatic NFW-polytrope halo；parent constraints来自73个b<-30 deg HaloSat EM fields。", "en": "Adopt the paper's joint exponential-disk plus Fang et al. adiabatic NFW-polytrope halo fit, constrained by 73 HaloSat EM fields at b<-30 deg."},
        {"zh": "沿每个M31 field积分paper catalog所闭合的n^2 convention，并保留disk--halo cross term；因为fitted n的particle identity未定义，不再乘1.2。", "en": "Integrate the catalog-closed n^2 convention along each M31 field and retain the disk--halo cross term; because the particle identity of fitted n is undefined, do not add a factor of 1.2.", "formula": "EM = ∫(n_disk + n_halo)^2 ds"},
        {"zh": "paper未给M31方向temperature；本项目采用HaloSat median kT=0.225 keV，配APEC 3.0.9、TBabs和field-specific HI4PI转absorbed 0.5--2，并用observed weights汇总。", "en": "The paper gives no temperature toward M31; this project adopts the HaloSat median kT=0.225 keV, APEC 3.0.9, TBabs, and field-specific HI4PI to obtain absorbed 0.5--2 brightness and combines fields with the observed weights."}
      ],
      "interpretation": {"zh": "十四场全部域外；仅supplemental extrapolation。", "en": "All fourteen fields are out of domain; this is only a supplemental extrapolation."},
      "assumptions": [{"zh": "fitted n的particle identity未知，不增加1.2 composition factor。", "en": "The particle identity of fitted n is unspecified, so no extra 1.2 composition factor is applied."}]
    },
    {
      "prior_id": "locatelli2024_reference_beta0p5_m31_footprint",
      "study_id": "locatelli-2024",
      "slug": "locatelli2024-reference-beta0p5-m31-footprint",
      "doi": "10.1051/0004-6361/202347061",
      "figure_label": "Locatelli+24 reference beta=0.5",
      "figure_central": 1.2545006767028457,
      "plotted_central": 1.290382023305802,
      "figure_low": 1.157655282720218,
      "figure_high": 1.3414632160380544,
      "native_input": {"zh": "Table 1 Combined beta=0.5 density geometry和0.614-0.694 keV O VIII line emissivity。", "en": "Table 1 Combined beta=0.5 density geometry and 0.614-0.694 keV O VIII line emissivity."},
      "transfer_summary": {"zh": "逐场O VIII normalization经80 eV smoothing closure、Z=0.3 target APEC和HI4PI phabs转0.5-2.0。", "en": "Convert field-by-field O VIII normalization through 80 eV smoothing closure, a Z=0.3 target APEC model, and HI4PI phabs to 0.5-2.0."},
      "transfer_steps": [
        {"zh": "采用Locatelli Table 1 Combined beta=0.5 disk+halo density geometry，在每个M31 primary field方向积分原文O VIII-emitting model。", "en": "Adopt the Locatelli Table 1 Combined beta=0.5 disk-plus-halo density geometry and integrate the published O VIII-emitting model toward every M31 primary field."},
        {"zh": "用原文0.614--0.694 keV、80 eV window的O VIII normalization闭合projection；这是line-map模型，不直接等同broadband。", "en": "Close the projection against the published O VIII normalization in the 0.614--0.694 keV, 80 eV window; this is a line-map model, not a broadband measurement."},
        {"zh": "保持O VIII line normalization固定，采用Z=0.3 target APEC和field-specific HI4PI phabs转成absorbed 0.5--2；以side-balanced estimator给ledger central，footprint min--max与parameter sensitivity分开报告。", "en": "Hold the O VIII line normalization fixed and use a Z=0.3 target APEC plus field-specific HI4PI phabs to obtain absorbed 0.5--2; report the side-balanced ledger central, footprint min--max, and parameter sensitivity separately."}
      ],
      "interpretation": {"zh": "ledger row的figure_central是side-balanced 1.255；Figure 3与all-field total配对的实心线另采用all-field estimator 1.290。", "en": "The ledger row's figure_central is the side-balanced 1.255; the solid Figure 3 line paired with the all-field total instead uses the separate all-field estimator 1.290."},
      "assumptions": [
        {"zh": "M31 l约121 deg在eRASS1 western-half map域外；这是geometry extrapolation。", "en": "M31 at about l=121 deg is outside the eRASS1 western-half map; this is a geometry extrapolation."},
        {"zh": "parameter range 0.934-1.575只是diagonal sensitivity，不是posterior。", "en": "The 0.934-1.575 parameter range is diagonal sensitivity, not a posterior."}
      ]
    },
    {
      "prior_id": "zhang2024_m31_mass_nominal_20kpc",
      "study_id": "zhang-2024",
      "slug": "zhang2024-m31-mass-nominal-20kpc",
      "doi": "10.1051/0004-6361/202449412",
      "figure_label": "Zhang+24 M31-mass stack at 20 kpc",
      "figure_central": 0.8284536873547118,
      "figure_low": 0.8284536873547118,
      "figure_high": 0.8284536873547118,
      "native_input": {"zh": "M31-mass external-galaxy stack的20 kpc intrinsic 0.5-2.0 luminosity surface density。", "en": "Intrinsic 0.5-2.0 luminosity surface density at 20 kpc from the M31-mass external-galaxy stack."},
      "transfer_summary": {"zh": "选择M31-mass bin、在20 kpc评价published median beta profile，再做distance-cancel angular conversion和v19 APEC absorption bridge。", "en": "Select the M31-mass bin, evaluate the published median beta profile at 20 kpc, then apply the distance-cancel angular conversion and v19 APEC absorption bridge."},
      "transfer_steps": [
        {"zh": "不按连续mass relation缩放：直接选择原文11.0<log(M*/Msun)<11.25的M31-mass central-galaxy stack。", "en": "Do not apply a continuous mass scaling relation: directly select the paper's M31-mass central-galaxy stack at 11.0<log(M*/Msun)<11.25."},
        {"zh": "采用Table 4 M31-mass median log S_X0=37.1、r_c=4 kpc、beta=0.37，在physical R=20 kpc评价projected beta profile，得到1.7253e36 erg s^-1 kpc^-2。", "en": "Use the Table 4 M31-mass medians log S_X0=37.1, r_c=4 kpc, and beta=0.37 and evaluate the projected beta profile at physical R=20 kpc, giving 1.7253e36 erg s^-1 kpc^-2.", "formula": "S_X(20)=10^37.1[1+(20/4)^2]^(-3×0.37+1/2)"},
        {"zh": "利用surface-brightness distance cancellation，把luminosity surface density除以4pi kpc_cm^2并乘arcmin^2/sr，再乘v19 absorbed/intrinsic ratio 0.678988916，得到Figure 3值0.828454。", "en": "Use surface-brightness distance cancellation: divide luminosity surface density by 4pi kpc_cm^2, multiply by arcmin^2/sr, and apply the v19 absorbed/intrinsic ratio 0.678988916 to obtain the Figure 3 value 0.828454.", "formula": "S_fig=S_L×Ω_arcmin2/(4π kpc_cm²)×0.678988916/10^-15"}
      ],
      "interpretation": {"zh": "population template，不是M31本身测量或formal local prior。", "en": "A population template, not an M31 measurement or formal local prior."},
      "assumptions": [{"zh": "单一thermal template代替stack的温度/金属丰度分布。", "en": "One thermal template substitutes for the stack's temperature/metallicity distribution."}]
    },
    {
      "prior_id": "grayson2025_eagle_agndt9",
      "study_id": "grayson-2025",
      "slug": "grayson2025-eagle-agndt9",
      "doi": "10.3847/1538-4357/ae100f",
      "figure_label": "EAGLE-AGNdT9",
      "figure_central": 0.22589950379475332,
      "figure_low": 0.20091404601593,
      "figure_high": 0.2474617256679783,
      "native_input": {"zh": "Figure 7 M31-mass bin的10-30 kpc EAGLE-AGNdT9 luminosity-density band。", "en": "The Figure 7 10-30 kpc EAGLE-AGNdT9 luminosity-density band in the M31-mass bin."},
      "transfer_summary": {"zh": "直接选择匹配M31 mass/radius的published bin，digitization后用共同distance-cancel与v19 APEC bridge；不做连续mass/radius rescaling。", "en": "Directly select the published bin matching M31 in mass and radius, then apply the common distance-cancel and v19 APEC bridge after digitization; no continuous mass/radius rescaling is used."},
      "transfer_steps": [
        {"zh": "选择Figure 7中11<log(M*/Msun)<11.25、12<log(M200c/Msun)<14的middle panel。simulation在0.1 dex stellar-mass cells匹配Zhang sample，但未匹配observed halo-mass distribution。", "en": "Select the Figure 7 middle panel at 11<log(M*/Msun)<11.25 and 12<log(M200c/Msun)<14. Simulations are matched to the Zhang sample in 0.1 dex stellar-mass cells, but their halo-mass distributions are not matched to observations."},
        {"zh": "读取physical 10--30 kpc radial bin中当前model的line central和shaded bootstrap band；使用calibrated log axes与exact line/fill RGB。", "en": "Read the current model's line central and shaded bootstrap band in the physical 10--30 kpc radial bin using calibrated logarithmic axes and exact line/fill RGB values."},
        {"zh": "把digitized intrinsic 0.5--2 luminosity surface density乘共同distance-cancel factor和v19 absorbed/intrinsic APEC ratio 0.678988916；保持为单一10--30 kpc band，不插值成M31 radial curve。", "en": "Multiply the digitized intrinsic 0.5--2 luminosity surface density by the common distance-cancel factor and v19 absorbed/intrinsic APEC ratio 0.678988916; retain one 10--30 kpc band and do not interpolate it into an M31 radial curve.", "formula": "S_fig=S_L×Ω_arcmin2/(4π kpc_cm²)×0.678988916/10^-15"}
      ],
      "interpretation": {"zh": "EAGLE-AGNdT9把thermal AGN heating increment从10^8.5提高到10^9 K并改变accretion parameterization；这是更强/更burst-like AGN heating的conditional template。", "en": "EAGLE-AGNdT9 raises the thermal AGN heating increment from 10^8.5 to 10^9 K and modifies the accretion parameterization; this is the conditional template for stronger, more burst-like AGN heating."},
      "assumptions": [{"zh": "figure-derived spread不是本项目measurement error。", "en": "The figure-derived spread is not a measurement error from this project."}]
    },
    {
      "prior_id": "grayson2025_eagle",
      "study_id": "grayson-2025",
      "slug": "grayson2025-eagle",
      "doi": "10.3847/1538-4357/ae100f",
      "figure_label": "EAGLE",
      "figure_central": 0.45049402230892394,
      "figure_low": 0.3954831154107961,
      "figure_high": 0.4999630414896396,
      "native_input": {"zh": "Figure 7 M31-mass bin的10-30 kpc standard EAGLE luminosity-density band。", "en": "The Figure 7 10-30 kpc standard-EAGLE luminosity-density band in the M31-mass bin."},
      "transfer_summary": {"zh": "直接选择匹配M31 mass/radius的published bin，digitization后用共同distance-cancel与v19 APEC bridge；不做连续mass/radius rescaling。", "en": "Directly select the published bin matching M31 in mass and radius, then apply the common distance-cancel and v19 APEC bridge after digitization; no continuous mass/radius rescaling is used."},
      "transfer_steps": [
        {"zh": "选择Figure 7中11<log(M*/Msun)<11.25、12<log(M200c/Msun)<14的middle panel。simulation在0.1 dex stellar-mass cells匹配Zhang sample，但未匹配observed halo-mass distribution。", "en": "Select the Figure 7 middle panel at 11<log(M*/Msun)<11.25 and 12<log(M200c/Msun)<14. Simulations are matched to the Zhang sample in 0.1 dex stellar-mass cells, but their halo-mass distributions are not matched to observations."},
        {"zh": "读取physical 10--30 kpc radial bin中当前model的line central和shaded bootstrap band；使用calibrated log axes与exact line/fill RGB。", "en": "Read the current model's line central and shaded bootstrap band in the physical 10--30 kpc radial bin using calibrated logarithmic axes and exact line/fill RGB values."},
        {"zh": "把digitized intrinsic 0.5--2 luminosity surface density乘共同distance-cancel factor和v19 absorbed/intrinsic APEC ratio 0.678988916；保持为单一10--30 kpc band，不插值成M31 radial curve。", "en": "Multiply the digitized intrinsic 0.5--2 luminosity surface density by the common distance-cancel factor and v19 absorbed/intrinsic APEC ratio 0.678988916; retain one 10--30 kpc band and do not interpolate it into an M31 radial curve.", "formula": "S_fig=S_L×Ω_arcmin2/(4π kpc_cm²)×0.678988916/10^-15"}
      ],
      "interpretation": {"zh": "EAGLE Ref-L050N0752、single-mode thermal AGN feedback、DeltaT_AGN=10^8.5 K的fiducial conditional template。", "en": "The fiducial EAGLE Ref-L050N0752 conditional template with single-mode thermal AGN feedback and DeltaT_AGN=10^8.5 K."},
      "assumptions": [{"zh": "不插值为M31 radial curve。", "en": "It is not interpolated into an M31 radial curve."}]
    },
    {
      "prior_id": "grayson2025_eagle_noagn",
      "study_id": "grayson-2025",
      "slug": "grayson2025-eagle-noagn",
      "doi": "10.3847/1538-4357/ae100f",
      "figure_label": "EAGLE-NoAGN",
      "figure_central": 0.9464272204530075,
      "figure_low": 0.8094945319665527,
      "figure_high": 1.050354962006114,
      "native_input": {"zh": "Figure 7 M31-mass bin的10-30 kpc EAGLE-NoAGN luminosity-density band。", "en": "The Figure 7 10-30 kpc EAGLE-NoAGN luminosity-density band in the M31-mass bin."},
      "transfer_summary": {"zh": "直接选择匹配M31 mass/radius的published bin，digitization后用共同distance-cancel与v19 APEC bridge；不做连续mass/radius rescaling。", "en": "Directly select the published bin matching M31 in mass and radius, then apply the common distance-cancel and v19 APEC bridge after digitization; no continuous mass/radius rescaling is used."},
      "transfer_steps": [
        {"zh": "选择Figure 7中11<log(M*/Msun)<11.25、12<log(M200c/Msun)<14的middle panel。simulation在0.1 dex stellar-mass cells匹配Zhang sample，但未匹配observed halo-mass distribution。", "en": "Select the Figure 7 middle panel at 11<log(M*/Msun)<11.25 and 12<log(M200c/Msun)<14. Simulations are matched to the Zhang sample in 0.1 dex stellar-mass cells, but their halo-mass distributions are not matched to observations."},
        {"zh": "读取physical 10--30 kpc radial bin中当前model的line central和shaded bootstrap band；使用calibrated log axes与exact line/fill RGB。", "en": "Read the current model's line central and shaded bootstrap band in the physical 10--30 kpc radial bin using calibrated logarithmic axes and exact line/fill RGB values."},
        {"zh": "把digitized intrinsic 0.5--2 luminosity surface density乘共同distance-cancel factor和v19 absorbed/intrinsic APEC ratio 0.678988916；保持为单一10--30 kpc band，不插值成M31 radial curve。", "en": "Multiply the digitized intrinsic 0.5--2 luminosity surface density by the common distance-cancel factor and v19 absorbed/intrinsic APEC ratio 0.678988916; retain one 10--30 kpc band and do not interpolate it into an M31 radial curve.", "formula": "S_fig=S_L×Ω_arcmin2/(4π kpc_cm²)×0.678988916/10^-15"}
      ],
      "interpretation": {"zh": "EAGLE-NoAGN关闭AGN feedback；论文明确说它不能再现stellar-mass function或stellar-halo mass relation，因此这是physics sensitivity experiment。", "en": "EAGLE-NoAGN disables AGN feedback; the paper explicitly says it fails to reproduce the stellar-mass function or stellar-to-halo mass relation, so this is a physics-sensitivity experiment."},
      "assumptions": [{"zh": "NoAGN是不同physics model，不是standard EAGLE的error bar。", "en": "NoAGN is a different physics model, not an error bar on standard EAGLE."}]
    },
    {
      "prior_id": "grayson2025_simba",
      "study_id": "grayson-2025",
      "slug": "grayson2025-simba",
      "doi": "10.3847/1538-4357/ae100f",
      "figure_label": "SIMBA",
      "figure_central": 1.6354745251160299,
      "figure_low": 1.3628820240832311,
      "figure_high": 1.9121285540582837,
      "native_input": {"zh": "Figure 7 M31-mass bin的10-30 kpc standard SIMBA luminosity-density band。", "en": "The Figure 7 10-30 kpc standard-SIMBA luminosity-density band in the M31-mass bin."},
      "transfer_summary": {"zh": "直接选择匹配M31 mass/radius的published bin，digitization后用共同distance-cancel与v19 APEC bridge；不做连续mass/radius rescaling。", "en": "Directly select the published bin matching M31 in mass and radius, then apply the common distance-cancel and v19 APEC bridge after digitization; no continuous mass/radius rescaling is used."},
      "transfer_steps": [
        {"zh": "选择Figure 7中11<log(M*/Msun)<11.25、12<log(M200c/Msun)<14的middle panel。simulation在0.1 dex stellar-mass cells匹配Zhang sample，但未匹配observed halo-mass distribution。", "en": "Select the Figure 7 middle panel at 11<log(M*/Msun)<11.25 and 12<log(M200c/Msun)<14. Simulations are matched to the Zhang sample in 0.1 dex stellar-mass cells, but their halo-mass distributions are not matched to observations."},
        {"zh": "读取physical 10--30 kpc radial bin中当前model的line central和shaded bootstrap band；使用calibrated log axes与exact line/fill RGB。", "en": "Read the current model's line central and shaded bootstrap band in the physical 10--30 kpc radial bin using calibrated logarithmic axes and exact line/fill RGB values."},
        {"zh": "把digitized intrinsic 0.5--2 luminosity surface density乘共同distance-cancel factor和v19 absorbed/intrinsic APEC ratio 0.678988916；保持为单一10--30 kpc band，不插值成M31 radial curve。", "en": "Multiply the digitized intrinsic 0.5--2 luminosity surface density by the common distance-cancel factor and v19 absorbed/intrinsic APEC ratio 0.678988916; retain one 10--30 kpc band and do not interpolate it into an M31 radial curve.", "formula": "S_fig=S_L×Ω_arcmin2/(4π kpc_cm²)×0.678988916/10^-15"}
      ],
      "interpretation": {"zh": "standard SIMBA包含high-Eddington wind、low-Eddington kinetic jet和相关X-ray feedback mode；本点是全部AGN modes启用的conditional template。", "en": "Fiducial SIMBA includes a high-Eddington wind, a low-Eddington kinetic jet, and associated X-ray feedback mode; this point is the conditional template with all AGN modes enabled."},
      "assumptions": [{"zh": "使用单一v19 APEC，不是SIMBA gas particle逐温度response。", "en": "Uses one v19 APEC model rather than temperature-by-temperature response for SIMBA gas particles."}]
    },
    {
      "prior_id": "grayson2025_simba_noagn",
      "study_id": "grayson-2025",
      "slug": "grayson2025-simba-noagn",
      "doi": "10.3847/1538-4357/ae100f",
      "figure_label": "SIMBA-NoAGN",
      "figure_central": 10.668992792955066,
      "figure_low": 10.394681925200063,
      "figure_high": 11.239522373010312,
      "native_input": {"zh": "Figure 7 M31-mass bin的10-30 kpc SIMBA-NoAGN luminosity-density band。", "en": "The Figure 7 10-30 kpc SIMBA-NoAGN luminosity-density band in the M31-mass bin."},
      "transfer_summary": {"zh": "直接选择匹配M31 mass/radius的published bin，digitization后用共同distance-cancel与v19 APEC bridge；不做连续mass/radius rescaling。", "en": "Directly select the published bin matching M31 in mass and radius, then apply the common distance-cancel and v19 APEC bridge after digitization; no continuous mass/radius rescaling is used."},
      "transfer_steps": [
        {"zh": "选择Figure 7中11<log(M*/Msun)<11.25、12<log(M200c/Msun)<14的middle panel。simulation在0.1 dex stellar-mass cells匹配Zhang sample，但未匹配observed halo-mass distribution。", "en": "Select the Figure 7 middle panel at 11<log(M*/Msun)<11.25 and 12<log(M200c/Msun)<14. Simulations are matched to the Zhang sample in 0.1 dex stellar-mass cells, but their halo-mass distributions are not matched to observations."},
        {"zh": "读取physical 10--30 kpc radial bin中当前model的line central和shaded bootstrap band；使用calibrated log axes与exact line/fill RGB。", "en": "Read the current model's line central and shaded bootstrap band in the physical 10--30 kpc radial bin using calibrated logarithmic axes and exact line/fill RGB values."},
        {"zh": "把digitized intrinsic 0.5--2 luminosity surface density乘共同distance-cancel factor和v19 absorbed/intrinsic APEC ratio 0.678988916；保持为单一10--30 kpc band，不插值成M31 radial curve。", "en": "Multiply the digitized intrinsic 0.5--2 luminosity surface density by the common distance-cancel factor and v19 absorbed/intrinsic APEC ratio 0.678988916; retain one 10--30 kpc band and do not interpolate it into an M31 radial curve.", "formula": "S_fig=S_L×Ω_arcmin2/(4π kpc_cm²)×0.678988916/10^-15"}
      ],
      "interpretation": {"zh": "SIMBA-NoAGN关闭全部AGN feedback后极亮、在linear图中off-scale；它也不能再现stellar-mass function/stellar-halo relation，只能视作feedback sensitivity experiment。", "en": "SIMBA-NoAGN disables all AGN feedback and becomes extremely bright and off scale in the linear panel; it also fails to reproduce the stellar-mass function or stellar-to-halo relation and is only a feedback-sensitivity experiment."},
      "assumptions": [{"zh": "数量级差异是feedback-model结果，不是观测显著性。", "en": "The order-of-magnitude difference is a feedback-model outcome, not an observational significance."}]
    }
  ]
}