Static evidence audit · source read from shared/problems/P001.md…P006.md and shared/questions/Q*.md
The repository defines a problem DAG and question records with target/idea links. The extracted structure below shows only 2 typed P→P edges, 0 typed Q→Q edges, and a one-way cross-layer trace of 7 literal Q→P mentions. No edge in this page was inferred from topic, shared target, or prose similarity.
Solid arrows follow exactly the source field direction. Dotted arrows are P006’s three answerable_on target links; they are not P→P DAG arcs.
P DAG: 1 serves + 1 requires + 0 specialises = 2 typed P→P arcs. P→target answerable_on arcs: 3.
One dot per actual Q*.md file. They have no lines between them because the declared Q schema contains no typed Q→Q relation and thus supplies 0 Q→Q edges.
updated1 strict YAML record missing type1 file with no YAML frontmatterDeclared outbound fields, counted literally: 203 Q→target values and 225 Q→idea values. These do not connect Q nodes to each other.
The task-defined cross-layer test counts any literal P0XX/Q0XX identifier in a Q/P file’s full text. This produces seven Q→P pairs (six Q files) and zero P→Q pairs. The lines are not upgraded to typed DAG edges: they are literal mentions, shown only because the requested cross-layer audit explicitly defines them that way.
Q→P literal mention pairs: 7. P→Q literal mention pairs: 0. Together, this is not a bidirectionally maintained link layer.
Layer P: 6 nodes; 2 typed P→P arcs (1 serves, 1 requires, 0 specialises); 3 answerable_on P→target arcs. Layer Q: 122 Q files visualized as nodes; 0 typed Q→Q arcs; 203 Q→target values; 225 Q→idea values. Cross layer: 7 literal Q→P identifier pairs, 0 literal P→Q identifier pairs.
Data-quality qualifier: 117 Q files have complete strict YAML; 1 strict-YAML file lacks the required type field. In 3 frontmatters, only the updated line is syntactically invalid due to an unquoted colon; all other declared Q fields were parsed after excluding precisely that line, and the original updated text was retained. One Q file has no YAML frontmatter. It is shown as a red dot and its explicit Markdown Targets/Ideas values are included in the field-value totals. There are 121 distinct filename Q IDs because two Q files carry Q171.
Boundary: raw Q text contains 73 other-Q identifier co-mentions across 40 files. They are not counted or drawn as Q→Q edges because no frontmatter relation field types their meaning; treating them as graph edges would be an inference. Cross-layer P/Q identifiers are different: the requested audit expressly asks to count them anywhere in file text.
| id | file | status | kind | serves | requires | specialises | answerable_on | sources | sources_verified |
|---|---|---|---|---|---|---|---|---|---|
| P001 | shared/problems/P001.md | draft | grand_challenge | "none" | [] | "none" | [] | [] | False |
| P002 | shared/problems/P002.md | draft | grand_challenge | "none" | ["P001"] | "none" | [] | [] | False |
| P003 | shared/problems/P003.md | draft | grand_challenge | "none" | [] | "none" | [] | [] | False |
| P004 | shared/problems/P004.md | draft | grand_challenge | "none" | [] | "none" | [] | [] | False |
| P005 | shared/problems/P005.md | draft | grand_challenge | "none" | [] | "none" | [] | [] | False |
| P006 | shared/problems/P006.md | open | sub_problem | "P002" | [] | "none" | ["M101", "M51", "M83"] | ["2010ApJS..188...46K", "2024ApJ...961..217G", "2025ApJ...986..167L", "2021MNRAS.508.6155W"] | True |
| file id | file | parse quality | status | title / question | targets | ideas | tags | updated |
|---|---|---|---|---|---|---|---|---|
| Q001 | shared/questions/Q001_central-diffuse-thermal-complexity.md | strict-yaml | active | Do source-masked central diffuse X-ray spectra of edge-on star-forming galaxies require one or multiple thermal components, and does the answer depend on galaxy properties? | ["NGC3628", "NGC4945", "NGC4565", "NGC3556", "NGC5775", "NGC4666"] | ["I033", "I034", "I035", "I036", "I037", "I043"] | ["question", "diffuse", "central", "thermal-complexity", "edge-on", "archive"] | 2026-07-21 |
| Q002 | shared/questions/Q002_edge-on-halo-detection-above-10mpc.md | strict-yaml | active | Do edge-on spiral galaxies at distances >10 Mpc have detectable hot X-ray halos at 15–30′ minor-axis offsets, and does the detectability depend on galaxy properties? | ["NGC5907", "NGC4217", "NGC4013", "NGC4666", "NGC2820", "NGC2146", "NGC4594"] | ["I039", "I040", "I041", "I044", "I045", "I076", "I079", "I080", "I086", "I090", "I112", "I146", "I239"] | ["question", "diffuse", "halo", "edge-on", "offset", "new-obs", "detection", "scaling-relation", "sample-level", "starburst-superwind", "liner", "descriptive-contrast"] | 2026-08-27 |
| Q003 | shared/questions/Q003_sy2-diffuse-vs-starburst-thermal-complexity.md | strict-yaml | active | Do Seyfert 2 galaxies produce source-masked central diffuse X-ray spectra that differ from starburst galaxies in their thermal complexity — do Sy2 central diffuse spectra require one or multiple thermal components, and is the answer different from the starburst sample? | ["Circinus"] | ["I046"] | ["question", "diffuse", "central", "thermal-complexity", "seyfert", "agn", "archive", "sy2-vs-starburst"] | 2026-07-20 |
| Q004 | shared/questions/Q004_arm-dependence-of-diffuse-xray-fuv-coupling.md | strict-yaml | active | Does spiral-arm environment change the slope of the diffuse-X-ray-to-FUV coupling, or only its normalization? | ["[[M101]]", "[[M51]]", "[[M83]]", "[[M33]]"] | ["I020", "I256"] | ["question", "diffuse", "fuv-coupling", "arm-interarm", "spiral"] | 2026-07-27 |
| Q005 | shared/questions/Q005_wind-symmetry-vs-environment.md | strict-yaml | active | Is a starburst-driven galactic wind symmetric about the disk, or shaped by its halo environment? | ["[[NGC253]]"] | ["I002", "I053", "I235"] | ["question", "superwind", "CGM", "symmetry", "bipolar"] | 2026-08-25 |
| Q006 | shared/questions/Q006_projected-outer-atmosphere-asymmetry.md | strict-yaml | active | Is a single projected outer-atmosphere field representative of a face-on starburst disk? | ["[[NGC6946]]"] | ["I054", "I067"] | ["question", "projected-atmosphere", "asymmetry", "face-on", "feedback", "CGM"] | 2026-08-07 (R2 I067 fork of I054 — four-aperture harmonic decomposition) |
| Q082 | shared/questions/Q082_ngc3079-outer-wind-adiabatic-thermal-profile.md | strict-yaml | active | Does NGC 3079's outer X-ray wind remain conditionally compatible with adiabatic free expansion? | ["[[NGC3079]]"] | ["I009", "I058", "I068", "I069", "I075", "I077", "I238"] | ["question", "superwind", "thermal-profile", "CC85", "projection", "archive", "sensitivity-test", "parameter-shift", "response-folded", "recovery-qualified", "radial-decrement"] | 2026-08-28 |
| Q084 | shared/questions/Q084_ngc5253-xray-bright-hot-ejecta-fate.md | strict-yaml | active | Do NGC 5253's starburst superbubbles vent an X-ray-bright hot phase into the outer halo? | ["[[NGC5253]]"] | ["I059", "I066", "I084", "I085", "I203"] | ["question", "dwarf-starburst", "superbubble", "halo", "outflow", "feedback"] | 2026-08-15 |
| Q090 | shared/questions/Q090_m51-axis-corrected-tidal-diffuse-excess.md | strict-yaml | active | Does the M51–NGC 5195 tidal interaction produce a measurable soft diffuse X-ray excess along the actual inter-galaxy axis? | ["[[M51]]", "[[NGC5195]]"] | ["I060", "I081", "I082", "I091", "I097", "I114", "I208"] | ["question", "tidal-interaction", "bridge", "diffuse", "archive", "geometry"] | 2026-08-17 |
| Q091 | shared/questions/Q091_virgo-cluster-ram-pressure-diffuse-hot-gas.md | strict-yaml | open | Does ram-pressure stripping in the Virgo Cluster environment produce a detectable diffuse hot-gas component along the minor-axis halo interface, distinct from the stripped cold/warm tail? | ["[[NGC4569]]", "[[NGC4388]]", "[[NGC4634]]"] | ["I092", "I093", "I110"] | ["question"] | 2026-08-10 |
| Q120 | shared/questions/Q120_ngc253-nw-halo-cc85-vs-isothermal-fork.md | strict-yaml | active | At 12–30 arcmin (12.217–30.543 kpc) in NGC 253's NW outer halo/inner CGM, do fixed projected CC85 and isothermal templates differ in XMM 0723220101? | ["[[NGC253]]"] | ["I071", "I089", "I139"] | ["question", "fork", "projected-temperature", "two-template-conditional", "cc85-vs-isothermal", "outer-halo", "inner-cgm"] | 2026-08-12 |
| Q148 | shared/questions/Q148_gas-poor-s0-diffuse-halo-xmm-detectability.md | strict-yaml | active | Do gas-poor S0 lenticular galaxies host XMM-detectable diffuse hot-gas halos beyond the Chandra-detected compact core? | ["[[NGC5866]]"] | ["I094", "I113"] | ["question"] | 2026-08-11 |
| Q149 | shared/questions/Q149_ngc4258-anomalous-arms-thermal-vs-nonthermal.md | strict-yaml | active | Are the NGC 4258 anomalous-arms X-ray bubbles thermal or non-thermal, and does XMM detect the directional contrast? | ["[[NGC4258]]"] | ["I095", "I111"] | ["question"] | 2026-08-26 (R1 I111 archive recheck; eRASS1 main-table correction; PIA10204 product-scope check) |
| Q156 | shared/questions/Q156_m82-point-source-population-correlated-variability.md | strict-yaml | active | What is the pairwise correlation amplitude of long-term X-ray variability across M82's XMM-resolvable point-source population, and what upper bound constrains it? | ["[[M82]]"] | ["I004", "I008", "I096"] | ["question", "point-source", "timing", "population", "compact-sources"] | 2026-08-10 |
| Q157 | shared/questions/Q157_ngc7793-lowmass-sd-hot-ism-extent.md | strict-yaml | active | Does the hot ISM of a low-mass Sd spiral extend beyond its optical disk, and can it be detected with a ULX-driven XMM archive repurposed for diffuse science? | ["[[NGC7793]]"] | ["I098"] | ["question"] | 2026-08-10 |
| Q158 | shared/questions/Q158_ngc4449-dwarf-irregular-hot-halo-venting.md | strict-yaml | active | Do dwarf irregular starbursts vent a detectable hot X-ray halo beyond their optical bodies, or is the hot gas confined to inner superbubbles? | ["[[NGC4449]]"] | ["I099", "I152"] | ["question"] | 2026-08-12 |
| Q168 | shared/questions/Q168_massive-spiral-cgm-azimuthal-smoothness.md | strict-yaml | active | Is the hot CGM of a massive isolated spiral azimuthally smooth or structured at fixed radius? | ["[[NGC1961]]"] | ["I101"] | ["question", "CGM", "massive-spiral", "azimuthal", "temperature", "surface-brightness", "archive"] | 2026-08-26 |
| Q169 | shared/questions/Q169_massive-spiral-corona-hydrostatic-isotropy.md | strict-yaml | active | Is the hot X-ray corona of a massive spiral in hydrostatic equilibrium, or is the isotropy claim an artifact of azimuthal averaging? | ["[[NGC6753]]"] | ["I102", "I116"] | ["question", "CGM", "corona", "massive-spiral", "isotropy", "hydrostatic-equilibrium", "surface-brightness", "archive"] | 2026-08-11 |
| Q170 | shared/questions/Q170_ngc3627-tidal-interaction-hot-halo-vs-feedback.md | strict-yaml | active | Does tidal interaction in a group environment produce a detectable hot X-ray halo independently of star-formation feedback? | ["[[NGC3627]]"] | ["I105", "I137", "I156"] | ["question", "tidal-interaction", "group-environment", "diffuse-halo", "cgm"] | 2026-08-12 |
| Q171 | shared/questions/Q171_moderately-inclined-superwind-current-calibration.md | no-yaml | active | Can current-calibration SAS/ESAS reprocessing of moderately deep (~25 ks PN clean) XMM observations reliably detect and characterize extraplanar diffuse hot gas in moderately inclined (b/a ~0.28) starburst galaxies, bridging the edge-on and face-on extremes? | ["NGC6810"] | ["I104"] | [] | None |
| Q171 | shared/questions/Q171_ngc3221-L-star-cgm-temperature-gradient-virial-radius.md | strict-yaml | active | Does the warm-hot CGM temperature gradient of an L* spiral extend to the virial radius, or does it flatten or truncate beyond 200 kpc? | ["[[NGC3221]]"] | ["I106", "I117"] | ["question", "cgm", "temperature-gradient", "L-star", "virial-radius", "thermodynamics"] | 2026-08-11 |
| Q172 | shared/questions/Q172_ngc1482-intermediate-distance-starburst-halo-detectability.md | strict-yaml | active | Can an intermediate-distance edge-on starburst establish a local outer minor-axis diffuse X-ray interval before any global-halo inference? | ["[[NGC1482]]"] | ["I107", "I142"] | ["question"] | 2026-08-12 |
| Q173 | shared/questions/Q173_ngc2683-quiescent-edge-on-sab-hot-halo-archive-detectability.md | strict-yaml | active | Does the nearby quiescent edge-on Sab NGC 2683 (10 Mpc) have a detectable hot X-ray halo in existing XMM+Chandra archive data? | ["[[NGC2683]]"] | ["I108"] | ["question"] | 2026-08-10 |
| Q174 | shared/questions/Q174_ngc3044-intermediate-distance-edge-on-halo-detectability.md | strict-yaml | active | Do highly edge-on star-forming spirals at ~20 Mpc host detectable hot X-ray halos at 15–30′ minor-axis offsets, extending the detection sequence beyond the <10 Mpc regime? | ["[[NGC3044]]"] | ["I109", "I155", "I163", "I168"] | ["question"] | 2026-08-31 |
| Q191 | shared/questions/Q191_ngc7793-deprojected-outer-halo-continuation.md | missing-type | open | Does NGC 7793 retain a measurable thermal outer atmosphere at deprojected 6.5–8.5 kpc? | ["[[NGC7793]]"] | ["I098", "I115", "I154"] | ["question", "hot-ism", "cgm", "low-mass-spiral", "NGC7793", "outer-profile"] | 2026-08-28 |
| Q195 | shared/questions/Q195_ngc5746-quiescent-massive-spiral-halo-cgm-extent.md | strict-yaml | active | What selected-side outer soft-X-ray surface-brightness profile can be established for NGC 5746 beyond its central XMM mapping? | ["NGC5746"] | ["I119", "I125"] | ["question", "diffuse", "halo", "quiescent", "massive-spiral", "cgm", "profile", "new-obs", "edge-on"] | 2026-08-11 |
| Q196 | shared/questions/Q196_ngc2903-barred-spiral-feedback-halo-cgm-extent.md | strict-yaml | active | Does the feedback-driven hot halo of a moderate-SFR barred spiral reach the CGM (≥40 kpc), or is it confined to the inner few kpc? | ["NGC2903"] | ["I120", "I130", "I133"] | ["question", "diffuse", "halo", "barred", "star-forming", "fountain", "cgm", "new-obs", "feedback"] | 2026-08-11 |
| Q198 | shared/questions/Q198_ngc6764-agn-hot-gas-confirmation-and-spectral-characterization.md | recovered-invalid-updated | active | Can first-XMM data independently confirm and characterize NGC 6764's AGN-origin bubble gas without a unique-mechanism claim? | ["[[NGC6764]]"] | ["I103", "I118", "I201"] | ["question", "agn-feedback", "radio-bubbles", "thermal-hot-gas", "spectral-characterization", "xmm"] | 2026-08-31 (R5 D042 C05: I118 parent-geometry history qualified; no question or I201 gate-state change) |
| Q199 | shared/questions/Q199_ngc4214-dwarf-starburst-hot-phase-retention-and-escape.md | strict-yaml | active | Does NGC 4214 retain a measurable source-masked hot phase around its dwarf-starburst complexes? | ["NGC4214"] | ["I121"] | ["question", "dwarf", "starburst", "diffuse-hot-gas", "superbubble", "feedback"] | 2026-08-11 |
| Q200 | shared/questions/Q200_ngc4700-hot-phase-counterpart-to-extraplanar-outflow-tracers.md | strict-yaml | active | Does NGC 4700's extraplanar outflow environment contain a measurable hot X-ray phase? | ["NGC4700"] | ["I122", "I177"] | ["question", "edge-on", "starburst", "diffuse-halo", "outflow", "feedback"] | 2026-08-14 |
| Q201 | shared/questions/Q201_ngc2613-edge-on-hot-phase-vs-hi-outflow.md | strict-yaml | active | Can a selected NGC 2613 PA23 projected soft-X-ray profile be constrained beyond the central diffuse-ISM region without inferring H I co-extension or a global halo? | ["NGC2613"] | ["I126", "I132", "I158"] | ["question", "edge-on", "intermediate-distance", "diffuse-halo", "disk-halo-interface", "multi-phase"] | 2026-08-12 |
| Q202 | shared/questions/Q202_ic10-local-group-dwarf-wind-hot-phase-extent.md | strict-yaml | active | Does IC 10's hot galactic-wind phase extend beyond the inner starburst into the disk–halo interface, or is it confined to the central star-forming complex despite the Lai+2007 synchrotron superbubble? | ["IC10"] | ["I127"] | ["question", "dwarf-starburst", "local-group", "galactic-wind", "diffuse-halo", "disk-halo-interface"] | 2026-08-14 |
| Q205 | shared/questions/Q205_ngc4438-virgo-ram-pressure-fov-edge-suzaku-tail-archive.md | strict-yaml | open | Can the two current nominal-FOV XMM records and Suzaku tail observation characterize NGC 4438's own diffuse hot-gas component, despite no XMM central pointing? | ["[[NGC4438]]"] | ["I124"] | ["question"] | 2026-08-11 |
| Q206 | shared/questions/Q206_ngc2403-galactic-fountain-disk-halo-hot-gas-reach.md | strict-yaml | open | Does the source-masked diffuse hot gas of the nearby star-forming spiral NGC 2403 extend beyond the inner disk into the disk–halo interface along the minor axis, or is it confined to the inner few kpc? | ["[[NGC2403]]"] | ["I123", "I134", "I143"] | ["question"] | 2026-08-12 |
| Q207 | shared/questions/Q207_ngc1808-projected-outer-hot-phase-reach.md | strict-yaml | active | Does NGC 1808 have a measurable projected outer hot component along its minor axis beyond the central Sy2/starburst complex? | ["[[NGC1808]]"] | ["I128", "I145", "I147", "I169", "I170"] | ["question", "hot-phase", "minor-axis", "new-obs"] | 2026-08-31 |
| Q208 | shared/questions/Q208_ngc7793-p13-hardness-intensity-sequence.md | strict-yaml | active | Does NGC 7793 P13 follow one continuous XMM hardness–intensity sequence over its qualified monitoring epochs? | ["[[NGC7793]]"] | ["I129", "I184"] | ["question", "compact-sources", "ulx", "spectral-monitoring"] | 2026-08-14 |
| Q249 | shared/questions/Q249_ngc1511-projected-hot-phase-interaction-extent.md | strict-yaml | open | Does NGC 1511 retain a measurable projected hot component beyond its optical disk, and do defined opposite minor-axis sides differ in projected soft emission? | ["NGC1511"] | ["I150", "I151", "I153"] | ["question", "hot-phase", "projected", "minor-axis", "paired-offset", "archive", "new-obs"] | 2026-08-12 (I151 descriptive paired-contrast fork) |
| Q258 | shared/questions/Q258_ngc1569-source-masked-diffuse-wind-archive.md | strict-yaml | active | Can public XMM data measure or bound NGC 1569's source-masked diffuse soft component after EPIC background qualification? | ["[[NGC1569]]"] | ["I159"] | ["question", "archive", "diffuse", "dwarf-starburst", "wind"] | 2026-08-12 |
| Q259 | shared/questions/Q259_ngc625-source-masked-diffuse-outflow-archive.md | strict-yaml | active | Can public XMM data establish a source-masked diffuse soft component or bound for NGC 625 after EPIC background qualification? | ["[[NGC625]]"] | ["I160"] | ["question", "archive", "diffuse", "dwarf-starburst", "outflow"] | 2026-08-31 |
| Q272 | shared/questions/Q272_ngc3184-face-on-source-masked-diffuse-baseline.md | strict-yaml | open | Can a matched XMM+Chandra source-masked component analysis reproduce or revise Doane et al. (2004)'s NGC 3184 diffuse decomposition? | ["[[NGC3184]]"] | ["I161", "I165"] | ["question", "face-on", "ngc3184", "archive"] | 2026-08-13 |
| Q273 | shared/questions/Q273_ngc3184-face-on-minor-axis-halo-offset.md | strict-yaml | open | Can NGC 3184 support a recovery-qualified source-masked projected diffuse-soft radial profile at 15–30′? | ["[[NGC3184]]"] | ["I162", "I167"] | ["question", "face-on", "ngc3184", "new-obs", "projected-profile", "projection-firewall"] | 2026-08-13 |
| Q274 | shared/questions/Q274_ngc4438-centred-xmm-diffuse-hot-gas-icm-separation.md | strict-yaml | open | Can a centred XMM EPIC field separate an NGC 4438 galaxy-associated diffuse component from Virgo-ICM/M86 projection? | ["[[NGC4438]]"] | ["I171"] | ["question", "new-obs", "xmm", "virgo", "ram-pressure-stripping", "diffuse-hot-gas", "component-separation"] | 2026-08-31 |
| Q275 | shared/questions/Q275_ngc7090-source-masked-extraplanar-soft-component-archive.md | strict-yaml | open | Can the existing XMM archive constrain NGC 7090's source-masked projected extraplanar soft component after EPIC background qualification? | ["[[NGC7090]]"] | ["I172"] | ["question", "archive", "xmm", "ngc7090", "edge-on", "diffuse-hot-gas", "extraplanar", "source-masked"] | 2026-08-13 |
| Q276 | shared/questions/Q276_ngc4490-pair-source-masked-soft-component-archive.md | strict-yaml | open | Can the existing XMM archive establish a source-masked pair-scale projected soft component or bound for NGC 4490/4485 after EPIC background qualification? | ["[[NGC4490]]"] | ["I173"] | ["question", "archive", "xmm", "ngc4490", "ngc4485", "interacting-pair", "diffuse-hot-gas", "source-masked"] | 2026-08-13 |
| Q283 | shared/questions/Q283_exterior-soft-component-archive-prevalence.md | strict-yaml | open | Across a roster fixed before the outcomes were seen, what fraction of nearby star-forming galaxies shows a source-masked exterior soft X-ray component above a common floor in the existing XMM archive? | ["[[NGC1569]]", "[[NGC625]]", "[[NGC4449]]", "[[NGC7090]]", "[[NGC2403]]", "[[NGC7793]]"] | ["I174"] | ["question", "archive", "xmm", "cross-target", "prevalence", "exterior", "diffuse-hot-gas", "source-masked", "stratified"] | 2026-08-14 |
| Q284 | shared/questions/Q284_intermediate-distance-minor-axis-offset-prevalence.md | strict-yaml | open | Do dedicated XMM pointings at the cycle-obs9 new-observation seed locators recover a local outer soft component at a measurable rate across a heterogeneous-distance roster, or do they exclude a majority-detection population at a stated floor? | ["[[NGC3044]]", "[[NGC1511]]", "[[NGC3627]]", "[[NGC3184]]"] | ["I175", "I204"] | ["question", "new-obs", "xmm", "cross-target", "prevalence", "minor-axis", "offset", "diffuse-hot-gas", "source-masked", "descriptive", "heterogeneous-distance"] | 2026-08-18 |
| Q285 | shared/questions/Q285_ic10-exterior-absolute-soft-emission-measurability.md | strict-yaml | open | Is IC 10's diffuse soft X-ray emission measurable, in absolute terms, outside its optical body? | ["[[IC10]]"] | ["I176"] | ["question"] | 2026-08-14 |
| Q287 | shared/questions/Q287_ngc4634-absolute-hot-halo-presence-per-sector.md | strict-yaml | active | Does NGC 4634 retain a hot halo phase at all on either side of its minor axis, or is it bounded away — independent of any leading/trailing comparison? | ["[[NGC4634]]"] | ["I178"] | ["question"] | 2026-08-14 |
| Q288 | shared/questions/Q288_ngc3221-19yr-discrete-source-stationarity.md | strict-yaml | active | How much does the luminous discrete X-ray source content of a star-forming L* spiral change over 19 years — is a single-epoch source list a representative description? | ["[[NGC3221]]"] | ["I179"] | ["question"] | 2026-08-14 |
| Q289 | shared/questions/Q289_ngc300-x1-multi-epoch-spectral-state-evolution.md | strict-yaml | open | Does a confirmed-black-hole ULX (NGC 300 X-1) change its X-ray spectral state between the multi-instrument epochs already in the archive, or does it remain spectrally stable across the epoch baseline? | ["[[NGC300]]"] | ["I180", "I200"] | ["question"] | 2026-08-15 |
| Q299 | shared/questions/Q299_ngc4258-outer-anomalous-arm-projected-soft-diffuse.md | recovered-invalid-updated | open | Can a dedicated XMM EPIC field measure or bound a projected soft diffuse component in NGC 4258's outer anomalous arms, beyond the inner bipolar bubbles? | ["[[NGC4258]]"] | ["I182"] | ["question", "new-obs", "xmm", "ngc4258", "anomalous-arms", "jet-driven-outflow", "diffuse-hot-gas"] | 2026-08-14 (R1 I182: bounded non-pre-emption + source support; see [[I182_ngc4258-outer-anomalous-arm-newobs]]) |
| Q300 | shared/questions/Q300_ic342-outer-disk-halo-interface-projected-soft-diffuse.md | strict-yaml | open | Can a dedicated XMM EPIC halo-offset field or mosaic detect or bound a projected soft diffuse component in the outer disk-halo interface of the nearest face-on spiral IC 342? | ["[[IC 342]]"] | ["I183"] | ["question", "new-obs", "xmm", "ic342", "face-on-spiral", "disk-halo-interface", "halo-offset", "mosaic"] | 2026-08-18 |
| Q305 | shared/questions/Q305_massive-spiral-cgm-thermal-structure-prevalence.md | strict-yaml | active | Is the resolved hot CGM of massive spiral galaxies in a single, smoothly-cooling thermal state, or does it show temperature/structural heterogeneity across deep XMM archives? | ["[[NGC1961]]", "[[NGC6753]]", "[[NGC3221]]"] | ["I101", "I102", "I116", "I106", "I117", "I186"] | ["question"] | 2026-08-31 |
| Q307 | shared/questions/Q307_ngc2683_outer-hot-halo-detectability.md | strict-yaml | active | Does NGC 2683 host a measurable projected outer hot-gas component at a dedicated 15–30′ minor-axis field? | ["[[NGC2683]]"] | ["I188"] | ["question", "hot-halo", "disk-halo-interface", "new-obs"] | 2026-08-15 |
| Q311 | shared/questions/Q311_ngc4258-exterior-sector-projected-soft-component.md | strict-yaml | open | Does NGC 4258 show a measurable projected soft X-ray component in frozen sky sectors lying wholly outside its projected optical disk? | ["[[NGC4258]]"] | ["I192"] | ["question", "new-obs", "exterior-sector", "source-agnostic", "ngc4258"] | 2026-08-31 (R1 corrected Konami+2009 imaging scope; current archive replay) |
| Q312 | shared/questions/Q312_halo-brightness-sfr-vs-mass-partial-association.md | recovered-invalid-updated | active | Is the extraplanar hot-halo surface brightness of edge-on spirals associated with star-formation surface density independently of stellar mass — feedback rate, or potential depth? | ["[[NGC5907]]", "[[NGC4217]]", "[[NGC4013]]", "[[NGC4666]]", "[[NGC2820]]"] | ["I193"] | ["question", "new-obs", "xmm", "cross-target", "halo", "diffuse-hot-gas", "sigma-sfr", "M_star", "partial-association", "censored-likelihood", "common-radius"] | 2026-08-18 (R3 cycle-obs9 I193 — physical D25-area/common-distance covariate certificate complete and conditionally negative: nominal plane is non-collinear but propagated p95 joint area 1.4991 exceeds the predeclared 0.7854 target; I193-E1/E2/E3 remain OPEN and I193 routes to R4 critique) |
| Q313 | shared/questions/Q313_exterior-soft-brightness-sfr-vs-mass-archive-association.md | strict-yaml | active | In the existing XMM archive, does the exterior source-masked soft surface brightness of nearby star-forming galaxies track star-formation surface density independently of stellar mass? | ["[[NGC1569]]", "[[NGC625]]", "[[NGC4449]]", "[[NGC7090]]", "[[NGC2403]]", "[[NGC7793]]"] | ["I194", "I209"] | ["question", "archive", "xmm", "cross-target", "exterior", "diffuse-hot-gas", "source-masked", "sigma-sfr", "M_star", "partial-association", "likelihood-preserving-regression"] | 2026-08-31 |
| Q314 | shared/questions/Q314_low-mass-starburst-wind-ejecta-escape-prevalence.md | strict-yaml | active | Do low-mass starburst dwarfs vent an X-ray-bright hot phase beyond their star-forming bodies at sample level, or is the hot ejecta confined to inner superbubbles? | ["[[NGC5253]]", "[[NGC4449]]", "[[IC10]]"] | ["I198"] | ["question"] | 2026-08-15 |
| Q315 | shared/questions/Q315_ngc300-x1-hard-band-spectral-state-evolution.md | strict-yaml | open | Can a hard-band-restricted (2–7 keV) joint XMM+Chandra+NuSTAR response-folded ΔΓ spectral-state-evolution test, with explicit cross-calibration nuisance parameters, detect or bound a spectral-state change in NGC 300 X-1 between the Swift 2007, XMM+NuSTAR 2016, and Chandra 2020 epochs? | ["[[NGC300]]"] | ["I200", "I205"] | ["question"] | 2026-08-16 |
| Q316 | shared/questions/Q316_virgo-cluster-ram-pressure-hot-halo-prevalence.md | strict-yaml | open | Across a frozen Virgo Cluster roster, what fraction of admitted cells shows a source-masked minor-axis hot-halo component above a common floor, and does that fraction exclude the field-galaxy prevalence? | ["[[NGC4569]]", "[[NGC4388]]", "[[NGC4438]]", "[[NGC4634]]"] | ["I202"] | ["question", "new-obs", "xmm", "cross-target", "virgo-cluster", "ram-pressure", "hot-halo", "prevalence", "stratified", "mixed-track"] | 2026-08-15 |
| Q319 | shared/questions/Q319_ngc1800-dwarf-starburst-wind-projected-component.md | strict-yaml | active | Does NGC 1800 host a measurable projected soft thermal component beyond its inner star-forming body, detectable by a first XMM EPIC observation? | ["[[NGC1800]]"] | ["I206"] | ["question", "dwarf-starburst", "diffuse-wind", "hot-gas", "new-obs"] | 2026-08-16 |
| Q320 | shared/questions/Q320_ngc4254-inner-disc-stripped-tail-archive.md | strict-yaml | active | Does NGC 4254 (M 99) retain a measurable diffuse hot phase in its inner disc and/or stripped H I tail environment, separable from the central source and ULX contamination in the existing XMM archive? | ["[[NGC4254]]"] | ["I207"] | ["question", "virgo-cluster", "diffuse-hot-gas", "ram-pressure", "stripped-tail", "archive"] | 2026-08-16 |
| Q326 | shared/questions/Q326_azimuthal-em-residual-beyond-spiral-phase.md | strict-yaml | active | At fixed radius in a face-on spiral disk, is the soft-X-ray emission measure a function of spiral phase alone, or does an azimuthal residual survive an exactly phase-matched control? | ["[[M51]]"] | ["I208"] | ["question", "diffuse", "face-on", "spiral", "azimuthal", "arm-phase-control", "methodology"] | 2026-08-17 |
| Q328 | shared/questions/Q328_discrete-source-epoch-representativeness-cross-target.md | strict-yaml | active | Across galaxies with two well-separated deep XMM EPIC epochs, how large is the epoch-to-epoch dispersion of the luminous discrete-source content, and is it bounded below the scale at which single-epoch source lists stop being representative? | ["[[M82]]", "[[NGC3221]]", "[[M33]]", "[[NGC7793]]", "[[M51]]", "[[NGC4258]]", "[[IC342]]"] | ["I210", "I179", "I096"] | ["question", "compact-sources", "timing", "population", "cross-target"] | 2026-08-18 |
| Q329 | shared/questions/Q329_ngc4656-exterior-minor-axis-projected-soft-component.md | strict-yaml | active | Does NGC 4656 — a low-mass, tidally disturbed edge-on spiral at b=+84.7° — show a measurable projected soft X-ray component in a dedicated exterior minor-axis XMM field, or can it be bounded below the ROSAT-era limit? | ["[[NGC4656]]"] | ["I211"] | ["question", "diffuse", "halo", "edge-on", "interacting", "new-obs"] | 2026-08-18 |
| Q330 | shared/questions/Q330_ngc4656-source-masked-diffuse-hot-gas-archive.md | strict-yaml | active | Can the existing nucleus-centred XMM EPIC field (0891020101) measure or bound a source-masked projected diffuse soft X-ray component in the off-nuclear region of NGC 4656, after current-calibration re-analysis? | ["[[NGC4656]]"] | ["I213"] | ["question", "diffuse", "halo", "edge-on", "interacting", "archive"] | 2026-08-18 |
| Q338 | shared/questions/Q338_radius-conditioned-exterior-soft-component-archive-census.md | strict-yaml | active | Across individually qualified XMM archive cells, which nearby star-forming galaxies show, bound, or leave unresolved a source-masked projected exterior soft component when each physical-radius regime is retained? | ["[[NGC1569]]", "[[NGC625]]", "[[NGC4449]]", "[[NGC7090]]", "[[NGC2403]]", "[[NGC7793]]"] | ["I214"] | ["question", "archive", "xmm", "cross-target", "descriptive-census", "exterior", "diffuse-hot-gas", "source-masked", "radius-conditioned"] | 2026-08-31 |
| Q339 | shared/questions/Q339_ngc2403-residual-above-disk-model-archive-fork.md | strict-yaml | open | In the existing XMM EPIC archive of NGC 2403, can a source-masked projected minor-axis outer excess be measured as a residual above a fitted exponential-disk diffuse model, or is that residual bounded, mixed, or unmeasurable? | ["[[NGC2403]]"] | ["I215"] | ["question"] | 2026-08-19 |
| Q340 | shared/questions/Q340_ngc4501-mach-cone-extraplanar-hot-gas.md | strict-yaml | active | Does NGC 4501's Mach-cone extraplanar diffuse emission survive source-masked EPIC re-analysis? | ["[[NGC4501]]"] | ["I232"] | ["question", "virgo", "ram-pressure", "mach-cone", "diffuse-hot-gas"] | 2026-08-25 |
| Q456 | shared/questions/Q456_compact-group-igrm-vs-member-superposition.md | strict-yaml | active | In a spiral-rich compact group, is the reported soft diffuse X-ray emission a genuine intragroup medium or the superposition of active member galaxies? | ["[[HCG16]]"] | ["I244"] | ["question"] | 2026-09-02 |
| Q457 | shared/questions/Q457_nearby-group-core-azimuthal-relaxation.md | strict-yaml | active | Is the core atmosphere of a nearby early-type group azimuthally relaxed, or perturbed enough to bias its hydrostatic mass? | ["[[NGC1407]]"] | ["I245"] | ["question"] | 2026-09-02 |
| Q458 | shared/questions/Q458_low-mass-disk-diffuse-hot-ism-in-ulx-led-archive.md | strict-yaml | active | Does a low-mass, late-type barred disk sustain a diffuse hot ISM at the amplitude an SFR-scaled relation predicts, when measured at the deepest depth the archive can offer? | ["[[NGC1313]]"] | ["I246"] | ["question"] | 2026-09-02 |
| Q459 | shared/questions/Q459_bar-fed-ring-feedback-outer-disk-coupling.md | strict-yaml | active | Is a bar-fed circumnuclear starburst ring a spatially self-contained feedback site, or does its hot gas reach the outer disk? | ["[[NGC1672]]"] | ["I247"] | ["question"] | 2026-09-02 |
| Q460 | shared/questions/Q460_group-member-one-sided-x-ray-edge-mechanism.md | strict-yaml | active | In a disturbed spiral falling through a poor group, is there a measurable one-sided diffuse X-ray asymmetry at all — and how large a one can the archive still hide? | ["[[NGC2276]]"] | ["I248"] | ["question"] | 2026-09-02 |
| Q461 | shared/questions/Q461_edge-on-halo-nondetection-depth-limited-or-physical.md | strict-yaml | active | Is a published edge-on-spiral X-ray halo non-detection a physical absence or an artefact of exposure depth? | ["[[NGC3877]]"] | ["I249"] | ["question"] | 2026-09-02 |
| Q462 | shared/questions/Q462_ngc1316-central-atmosphere-radial-thermal-structure.md | strict-yaml | active | Does NGC 1316's central hot atmosphere show a measurable radial thermal/abundance structure beyond the inner kiloparsec, and is it consistent with a cooling core perturbed by the Fornax A radio lobes? | ["[[NGC1316]]"] | ["I250"] | ["question"] | 2026-09-02 |
| Q463 | shared/questions/Q463_ngc7331-extraplanar-hot-gas-beyond-central-archive.md | strict-yaml | active | Does NGC 7331 retain a measurable extraplanar hot component beyond its central 0.54′-clustered XMM archive, or is its hot ISM confined to the inner disk? | ["[[NGC7331]]"] | ["I251"] | ["question"] | 2026-09-02 |
| Q464 | shared/questions/Q464_epic-pn-mos-diffuse-temperature-interchangeability.md | strict-yaml | active | Are XMM EPIC PN and MOS diffuse temperatures interchangeable, and does any offset depend on surface brightness? | ["[[NGC253]]"] | ["I252"] | ["question", "calibration", "epic", "methods"] | 2026-09-02 |
| Q465 | shared/questions/Q465_epic-acis-extended-lowsb-flux-scale.md | strict-yaml | active | For extended low-surface-brightness soft emission, is the EPIC/ACIS flux ratio independent of surface brightness? | [] | ["I254"] | ["question", "cross-calibration", "epic", "acis", "methods"] | 2026-09-02 |
| Q466 | shared/questions/Q466_soft-proton-systematic-generality-and-exposure-saturation.md | strict-yaml | active | Is the conservative soft-proton systematic generally an overestimate for faint extended EPIC spectra, and does the error budget saturate before the requested exposure? | [] | ["I255"] | ["question", "background", "soft-proton", "esas", "error-budget", "methods"] | 2026-09-02 |
| Q467 | shared/questions/Q467_edge-on-halo-luminosity-distribution-bimodality.md | strict-yaml | active | Is the extraplanar hot-gas luminosity distribution of edge-on spirals bimodal at controlled sensitivity, or is the observed split an artefact of survey depth? | [] | ["I253"] | ["question", "halo", "edge-on", "population", "censored-data", "occurrence"] | 2026-09-02 |
| Q468 | shared/questions/Q468_arm-contrast-separability-from-arm-definition.md | strict-yaml | active | Is an arm/interarm coupling contrast separable from the choice of arm definition? | ["[[M101]]"] | ["I256"] | ["question", "arm-interarm", "identifiability", "mask-construction", "precondition"] | 2026-09-02 |
| Q469 | shared/questions/Q469_m31-bulge-disc-same-pipeline-temperature.md | strict-yaml | active | Do the bulge and the star-forming disc of the nearest large spiral hold hot gas at different temperatures, or does the published difference come from the pipelines? | ["[[M31]]"] | ["I257"] | ["question", "m31", "thermal-structure", "methods"] | 2026-09-02 |
| Q470 | shared/questions/Q470_undisturbed-control-region-existence-census.md | strict-yaml | active | Does a control region that was not chosen by looking at the X-ray map exist in the galaxies where contrast measurements are proposed? | ["[[M51]]", "[[NGC6946]]", "[[NGC5253]]", "[[NGC1808]]", "[[NGC1961]]"] | ["I259"] | ["question", "identifiability", "methods", "census"] | 2026-09-02 |
| Q471 | shared/questions/Q471_wind-vs-corona-discrimination-reachability.md | strict-yaml | active | Can any XMM design separate a free wind from a quasi-hydrostatic corona in an edge-on spiral halo, or is the test out of reach? | ["[[NGC4631]]", "[[NGC3079]]", "[[NGC253]]", "[[NGC5775]]"] | ["I260", "I005"] | ["question", "halo", "wind", "power-analysis", "methods"] | 2026-09-02 |
| Q472 | shared/questions/Q472_materiality-threshold-availability-in-the-field.md | strict-yaml | active | Does this subfield publish outcome-independent materiality thresholds, or does it only publish significance? | [] | ["I261"] | ["question", "methods", "literature", "field-structure"] | 2026-09-02 |
| Q473 | shared/questions/Q473_outer-disk-sf-coupling-break-radius.md | strict-yaml | active | Does the outer-disk diffuse X-ray emission of a face-on spiral stay coupled to local star formation, or does a smoother component take over — and at what radius? | ["[[M101]]"] | ["I258", "I226", "I021"] | ["question", "m101", "outer-disk", "radial-profile", "pi-directed"] | 2026-09-02 |
| Q474 | shared/questions/Q474_ngc300-x1-phase-matched-state-comparison.md | strict-yaml | active | Between phase-matched, out-of-eclipse windows, does the confirmed-black-hole ULX NGC 300 X-1 occupy the same cell of a multi-observable black-hole-binary state classifier at epochs years apart? | ["[[NGC300]]"] | ["I262"] | ["question", "compact-source", "ulx", "spectral-timing", "archive"] | 2026-09-02 |
| Q475 | shared/questions/Q475_ngc3310-outer-diffuse-component.md | strict-yaml | active | Does NGC 3310, a starburst merger observed only on-axis, have diffuse hot gas beyond the region its three central archival EPIC fields reach? | ["[[NGC3310]]"] | ["I263"] | ["question", "new-obs", "starburst-merger", "diffuse"] | 2026-09-02 |
| Q476 | shared/questions/Q476_group-core-two-phase-instrument-independence.md | strict-yaml | active | Is the two-temperature preference in the NGC 5044 group core a property of the plasma or of the instrument that measured it? | ["[[NGC5044]]"] | ["I264"] | ["question", "archive", "group-scale", "multiphase", "methods"] | 2026-09-02 |
| Q477 | shared/questions/Q477_group-shock-two-observable-mach-consistency.md | strict-yaml | active | Do the density-jump and temperature-jump Mach numbers of a weak group-scale shock agree? | ["[[HCG62]]"] | ["I265"] | ["question", "group-scale", "shock", "thermalisation"] | 2026-09-02 |
| Q478 | shared/questions/Q478_group-wake-composition-stripped-vs-focused.md | strict-yaml | active | What fraction of a group-scale X-ray wake is stripped galaxy gas rather than compressed ambient medium? | ["[[NGC6872]]"] | ["I266"] | ["question", "group-scale", "wake", "abundance", "gas-removal"] | 2026-09-02 |
| Q479 | shared/questions/Q479_massive-spiral-hot-halo-detection-reproducibility.md | strict-yaml | active | Are the hot-halo detections around the most massive disk galaxies reproducible, or are they a function of the background model chosen? | ["[[UGC12591]]", "[[NGC5746]]"] | ["I267"] | ["question", "hot-halo", "massive-spiral", "reproducibility", "background-systematics"] | 2026-09-02 |
| Q480 | shared/questions/Q480_seyfert-galaxy-scale-photoionized-vs-collisional-transition.md | strict-yaml | active | At what radius does a Seyfert 2's soft X-ray emission stop being the AGN's photoionized cone and start being its host galaxy's hot gas? | ["[[NGC1068]]"] | ["I268"] | ["question", "seyfert", "agn-feedback", "photoionization", "hot-ism"] | 2026-09-02 |
| Q481 | shared/questions/Q481_merger-superwind-hot-phase-escape-radius.md | strict-yaml | active | Does the hot phase of a superwind in a major gas-rich merger escape the remnant, or terminate inside it? | ["[[NGC3256]]"] | ["I270"] | ["question", "superwind", "merger", "hot-ism", "feedback", "metal-transport"] | 2026-09-02 |
| Q482 | shared/questions/Q482_cavity-contrast-instrument-independence.md | strict-yaml | active | Is the measured contrast of X-ray cavities and cold fronts in a hot atmosphere a property of the gas, or of the instrument that measured it? | ["[[NGC4636]]"] | ["I271"] | ["question", "agn-feedback", "cavities", "group-atmosphere", "cross-instrument", "methods"] | 2026-09-02 |
| Q483 | shared/questions/Q483_epoch-multiplicity-exponent-faint-extended.md | strict-yaml | active | At fixed total exposure, does the achieved uncertainty on faint extended XMM emission fall with the number of independent epochs, and with what exponent? | ["[[M83]]", "[[NGC253]]", "[[M31]]"] | ["I273"] | ["question", "methods", "background", "error-budget", "observing-strategy", "xmm"] | 2026-09-02 |
| Q484 | shared/questions/Q484_arm-phase-temperature-vs-masking-completeness.md | strict-yaml | active | Is the arm/interarm hot-gas temperature contrast in spiral disks a property of the gas, or of how completely the discrete sources were removed? | ["[[M83]]"] | ["I269"] | ["question", "arm-interarm", "hot-ism", "source-masking", "methods", "spiral"] | 2026-09-02 |
| Q497 | shared/questions/Q497_second-thermal-phase-or-unresolved-binaries.md | strict-yaml | active | Is the second thermal component of a source-masked central spectrum a phase of hot gas, or the part of the X-ray binary luminosity function the mask left behind? | ["[[NGC3628]]", "[[NGC4945]]", "[[NGC4565]]", "[[NGC3556]]", "[[NGC5775]]"] | ["I292"] | ["question", "hot-ism", "central", "source-masking", "xlf", "methods", "cross-target"] | 2026-09-03 |
| Q498 | shared/questions/Q498_group-atmosphere-separability-against-projected-cluster.md | strict-yaml | active | How far out can a group's hot atmosphere be separated spectrally from a cluster projected behind it? | ["[[NGC4756]]"] | ["I293"] | ["question", "group", "early-type", "projection", "hot-gas", "methods"] | 2026-09-03 |
| Q499 | shared/questions/Q499_face-on-halo-geometric-identifiability.md | strict-yaml | active | In a nearly face-on spiral, is a hot "halo" a place, or only a label a spectral decomposition produced? | ["[[NGC628]]"] | ["I294"] | ["question", "face-on", "spiral", "halo", "geometry", "identifiability", "methods"] | 2026-09-03 |
| Q500 | shared/questions/Q500_population-sum-variance-versus-independence.md | strict-yaml | active | Does a galaxy's X-ray binary population vary as N independent sources, or does it carry a common mode? | ["[[M82]]", "[[M83]]"] | ["I295"] | ["question", "compact-sources", "timing", "population", "error-budget", "out-of-comfort-zone"] | 2026-09-03 |
| Q502 | shared/questions/Q502_hi-rich-massive-spiral-hot-halo-presence.md | strict-yaml | active | Does a massive spiral that kept its cold gas also keep a hot halo — and is a hot-halo claim made on 5 ks a claim at all? | ["[[NGC3968]]"] | ["I298"] | ["question", "massive-spiral", "hot-halo", "cgm", "hi-rich", "projection", "methods"] | 2026-09-03 |
| Q503 | shared/questions/Q503_hot-gas-per-unit-sfr-in-an-xuv-disk.md | strict-yaml | active | Does star formation make hot gas at a fixed rate, or only where it is clustered? | ["[[NGC3621]]"] | ["I299"] | ["question", "xuv-disk", "star-formation", "hot-ism", "lx-sfr", "scaling-relation", "methods"] | 2026-09-03 |
| Q504 | shared/questions/Q504_photoionized-fraction-predictability-from-nuclear-quantities.md | strict-yaml | active | Is the photoionized fraction of a Compton-thick host's extended soft emission predictable from the nucleus, or must every galaxy be measured? | ["[[Circinus]]", "[[NGC4945]]", "[[NGC1068]]"] | ["I300", "I046", "I034"] | ["question", "agn", "seyfert-2", "photoionization", "diffuse", "decomposition", "methods"] | 2026-09-03 |
| Q505 | shared/questions/Q505_entropy-profile-as-wind-versus-corona-discriminant.md | strict-yaml | active | Is the entropy profile the discriminant that the temperature profile could not be, for an edge-on spiral halo? | ["[[NGC4631]]"] | ["I297", "I005"] | ["question", "edge-on-spiral", "halo", "wind-vs-corona", "entropy", "discriminant", "methods"] | 2026-09-03 |
| Q506 | shared/questions/Q506_published-null-versus-soft-response-null.md | strict-yaml | active | When a massive quiescent spiral shows no extraplanar X-rays, is that the galaxy or the instrument's soft response? | ["[[NGC5170]]"] | ["I302"] | ["question", "edge-on-spiral", "quiescent", "halo", "published-null", "instrument-response"] | 2026-09-03 |
| Q507 | shared/questions/Q507_ccd-band-ratio-as-a-photoionisation-diagnostic.md | strict-yaml | active | Can a CCD band ratio actually measure a photoionised fraction, or has the field been assuming it can? | ["[[NGC1365]]"] | ["I303", "I300"] | ["question", "agn", "photoionisation", "extended-soft", "proxy-validation", "methods"] | 2026-09-03 |
| Q508 | shared/questions/Q508_source-mask-convention-as-a-load-bearing-systematic.md | strict-yaml | active | Is a source-masked diffuse X-ray measurement a property of the galaxy, or of the masking convention? | ["[[M83]]"] | ["I304", "I015"] | ["question", "methods", "source-mask", "systematics", "diffuse", "face-on-spiral"] | 2026-09-03 |
| Q509 | shared/questions/Q509_is-the-ulx-boundary-a-variability-discontinuity.md | strict-yaml | active | Does anything discontinuous happen to X-ray binary variability at the ULX luminosity boundary? | ["[[M83]]"] | ["I305", "I018"] | ["question", "compact-sources", "ulx", "timing", "population", "out-of-comfort-zone"] | 2026-09-03 |
| Q510 | shared/questions/Q510_does-merger-stage-order-the-diffuse-soft-residual.md | strict-yaml | active | Does the hot phase of a star-forming galaxy care about the merger? | ["[[NGC4038-4039]]", "[[NGC6240]]", "[[NGC7552]]", "[[NGC7771]]", "[[VV114]]", "[[NGC3256]]"] | ["I307"] | ["question", "hot-gas", "merger", "scaling-relation", "cross-target", "methods"] | 2026-09-03 |
| Q511 | shared/questions/Q511_is-a-hot-gas-abundance-a-property-of-the-gas-or-of-the-temperature-model.md | strict-yaml | active | Is a hot-gas abundance a property of the gas, or of the temperature model? | ["[[NGC4038-4039]]"] | ["I308"] | ["question", "hot-gas", "abundances", "model-degeneracy", "merger", "methods"] | 2026-09-03 |
| Q512 | shared/questions/Q512_is-there-any-exposure-at-which-a-single-galaxy-hot-cgm-non-detection-means-something.md | strict-yaml | active | Is there any XMM exposure at which a single-galaxy hot-CGM non-detection at 60–130 kpc means something? | ["[[NGC4013]]", "[[NGC5907]]", "[[NGC4217]]", "[[NGC4666]]", "[[NGC2820]]", "[[NGC300]]"] | ["I309", "I041", "I039", "I040", "I044", "I045", "I049"] | ["question", "halo", "cgm", "feasibility", "systematics", "edge-on", "methods"] | 2026-09-03 |
| Q513 | shared/questions/Q513_is-an-extraplanar-detection-a-measurement-of-the-halo-or-of-the-psf.md | strict-yaml | active | Is an extraplanar X-ray detection a measurement of the halo, or of the PSF? | [] | ["I310", "I113"] | ["question", "psf", "instrumental-systematics", "halo", "edge-on", "literature-screen", "methods"] | 2026-09-03 |
| Q514 | shared/questions/Q514_how-small-can-an-xmm-diffuse-aperture-be-before-one-agn-is-the-signal.md | strict-yaml | active | How small can an XMM diffuse aperture be before one unmasked AGN is the whole signal? | [] | ["I312"] | ["question"] | 2026-09-03 |
| Q515 | shared/questions/Q515_how-deep-has-the-xmm-archive-already-observed-the-outer-fields-it-is-asked-to-observe.md | strict-yaml | active | How deep has the XMM archive already observed off-axis the outer fields it is being asked to observe? | ["NGC4258", "NGC1672", "NGC7331", "NGC3310", "NGC3256", "NGC3968", "NGC3184"] | ["I313"] | ["question"] | 2026-09-03 |
| Q516 | shared/questions/Q516_is-the-90kpc-soft-emission-around-ngc6286-hot-gas.md | strict-yaml | active | Is the ~90 kpc soft X-ray emission around NGC 6286 hot gas, and at what temperature? | ["NGC6286"] | ["I314"] | ["question"] | 2026-09-03 |
| Q517 | shared/questions/Q517_is-the-hot-phase-of-a-dwarf-starburst-bound-to-it.md | strict-yaml | active | Is the hot phase of a dwarf starburst bound to its galaxy? | ["HENIZE2-10", "NGC4449"] | ["I315", "I316"] | ["question"] | 2026-09-03 |
| Q518 | shared/questions/Q518_does-a-tidal-interaction-change-how-efficiently-a-disk-turns-star-formation-into-hot-gas.md | strict-yaml | active | Does a tidal interaction change how efficiently a disk turns star formation into hot gas? | ["M51", "NGC5195"] | ["I317"] | ["question"] | 2026-09-03 |
| Q519 | shared/questions/Q519_is-a-compact-group-bridge-heated-gas-or-displaced-gas.md | strict-yaml | active | Is a compact-group intergalactic bridge heated gas, or displaced gas? | ["HCG57"] | ["I318"] | ["question"] | 2026-09-03 |
| Q520 | shared/questions/Q520_does-a-starburst-blowout-bubble-hold-a-phase-hotter-than-the-gas-we-measure.md | strict-yaml | active | Does a starburst blow-out bubble hold a phase hotter than the gas we measure? | ["NGC2782"] | ["I319"] | ["question"] | 2026-09-03 |
| Q540 | shared/questions/Q540_ngc520-merger-wind-age-vs-relic.md | strict-yaml | active | Is the hot gas of a mid-stage merger still being driven, or is it the relic of the burst? | ["NGC520"] | ["I337"] | ["question"] | 2026-09-04 |
| from Q file | literal P id | source locator |
|---|---|---|
| Q468 | P002 | shared/questions/Q468_arm-contrast-separability-from-arm-definition.md:26 |
| Q468 | P006 | shared/questions/Q468_arm-contrast-separability-from-arm-definition.md:21 |
| Q484 | P006 | shared/questions/Q484_arm-phase-temperature-vs-masking-completeness.md:53 |
| Q498 | P003 | shared/questions/Q498_group-atmosphere-separability-against-projected-cluster.md:35 |
| Q519 | P003 | shared/questions/Q519_is-a-compact-group-bridge-heated-gas-or-displaced-gas.md:18 |
| Q520 | P005 | shared/questions/Q520_does-a-starburst-blowout-bubble-hold-a-phase-hotter-than-the-gas-we-measure.md:18 |
| Q540 | P005 | shared/questions/Q540_ngc520-merger-wind-age-vs-relic.md:31 |