Datasets:

ulamai
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UnsolvedAstronomy

id string	problem_number string	slug string	title string	statement string	plain_statement string	precise_statement string	category string	category_number int64	category_name string	subcategory string	secondary_categories list	question_type string	object_classes list	object_scope string	population_scope string	scales list	epochs list	wavelengths_and_messengers list	facilities_or_surveys list	observables list	inferred_properties list	selection_effects list	systematic_uncertainties list	degeneracies list	status string	published bool	evidence_state string	consensus_state string	status_last_checked timestamp[s]	status_justification string	verification_mode string	verification_horizon string	falsifiability_or_discriminant string	current_best_bounds_or_constraints string	competing_models list	resolution_criteria list	why_it_matters string	background_needed string	difficulty_level int64	difficulty_rationale string	is_gold_seed bool	sources list	related_problem_ids list	duplicate_of null	cross_domain_links list	tags list	rejection_code string	curation_notes string	version string	created_at timestamp[s]	updated_at timestamp[s]
UAST-000001	UAST-000001	uast-000001-energy-scale-of-cosmic-inflation-and-primordial-tensor-to-scalar-ratio-r	Energy Scale of Cosmic Inflation and Primordial Tensor-to-Scalar Ratio r	Did cosmic inflation generate a detectable background of primordial tensor perturbations, and what is the value of the tensor-to-scalar ratio r and energy scale V^{1/4} encoded in degree-scale cosmic microwave background B-mode polarization?	Did the early universe undergo inflation at an energy scale high enough to leave a detectable gravitational-wave imprint in the polarization of the cosmic microwave background?	Across multipoles 2 <= ell <= 200 of the cosmic microwave background polarization field, what is the amplitude r = A_t / A_s of primordial tensor modes at pivot scale k_* = 0.05 Mpc^{-1} after separating Galactic thermal dust and synchrotron foregrounds and delensing late-time gravitational E-to-B conversion?	cosmology_early_universe	1	Cosmology and the Early Universe	inflation_and_primordial_initial_conditions	[]	value_or_bound	[ "cosmic_background", "early_universe", "large_scale_structure" ]	population_level	Astrophysical systems in inflation and primordial initial conditions	[ "cosmological_horizon", "gpc", "10_to_100_mpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "cmb_mm_submm", "optical", "near_ir", "radio_cm_m_lowfreq" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB BB angular power spectrum C_ell^{BB}", "multi-frequency polarized dust and synchrotron SED", "CMB lensing convergence kappa" ]	[ "tensor-to-scalar ratio r", "inflationary energy scale V^{1/4}", "inflaton field excursion Delta phi / M_Pl" ]	[ "sky-fraction mask exclusion of high-latitude Galactic dust filaments" ]	[ "spatially varying Galactic dust spectral index beta_d and temperature T_d", "instrumental beam polarization leakage and HWP systematics", "delensing residual variance" ]	[ "primordial tensor B-modes versus non-Gaussian polarized Galactic dust residuals and chiral axion-gauge field B-modes" ]	open	true	partial_observational_constraint	open_consensus	2026-10-16T00:00:00	BICEP/Keck and Planck observations constrain r < 0.036 (95% CL) without a detection, leaving open whether single-field Starobinsky/alpha-attractor models (r ~ 0.003-0.004) or low-scale inflation held in the early universe.	survey_statistical	decade_scale	Multi-frequency degree-scale and reionization-bump B-mode polarization measurements from Simons Observatory, LiteBIRD, and CMB-S4 reaching sigma(r) <= 5 x 10^{-4} with independent cross-frequency dust separation and >70% delensing.	Current observations from Planck, JWST, DESI constrain tensor-to-scalar ratio r, but systematic uncertainties in spatially varying Galactic dust spectral index beta_d and temperature prevent a definitive resolution.	[ "Baseline astrophysical mechanism in inflation and primordial initial conditions constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Energy Scale of Cosmic Inflation and Primordial Tensor-to-Scalar Ratio" ]	[ "High-significance multi-wavelength or dynamical measurement of CMB BB angular power spectrum C_ell^{BB} using Planck, JWST, DESI.", "Breaking the model degeneracy between primordial tensor B-modes versus non-Gaussian polarized Galactic dust residuals and chiral to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating tensor-to-scalar ratio r and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	BICEP/Keck and Planck observations constrain r < 0.036 (95% CL) without a detection, leaving open whether single-field Starobinsky/alpha-attractor models (r ~ 0.003-0.004) or low-scale inflation held in the early universe.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "New Messengers and New Physics: Windows on the Dynamic Universe, Priority Area: New Windows on the Dynamic Universe (Inflation)", "verbatim_quote_used": false }, { "source_id": "SRC-AST-002319", "citatio...	[ "UAST-000002", "UAST-000018", "UAST-000019", "UAST-000020", "UAST-000021", "UAST-000022", "UAST-000023", "UAST-000102", "UAST-000103", "UAST-000104", "UAST-000105", "UAST-000106", "UAST-000107", "UAST-000108", "UAST-000109", "UAST-005514", "UAST-005525", "UAST-005551" ]	null	[]	[ "cosmology_early_universe", "inflation_and_primordial_initial_conditions", "cosmic inflation", "primordial gravitational waves", "CMB B-mode polarization" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000002	UAST-000002	uast-000002-abundance-and-luminosity-function-of-unexpectedly-uv-bright-galaxies-at-redshifts-z-1	Abundance and Luminosity Function of Unexpectedly UV-Bright Galaxies at Redshifts z > 10 in JWST Surveys	What physical mechanism explains the high number density of ultraviolet-luminous galaxies observed by JWST at redshifts 10 <= z <= 14 compared with pre-JWST constant star-formation-efficiency LambdaCDM extrapolations?	Why has the James Webb Space Telescope found so many bright galaxies in the first 300 to 500 million years after the Big Bang compared with standard galaxy formation expectations?	In the rest-frame 1500 Angstrom UV luminosity function Phi(M_UV, z) at 10 <= z <= 14 measured by JWST NIRCam and NIRSpec, what combination of elevated feedback-free star formation efficiency epsilon_*, stochastic bursty star formation, top-heavy initial mass function, reduced dust attenuation, or early AGN contribution...	cosmology_early_universe	1	Cosmology and the Early Universe	inflation_and_primordial_initial_conditions	[]	mechanism	[ "cosmic_background", "early_universe", "large_scale_structure" ]	population_level	Astrophysical systems in inflation and primordial initial conditions	[ "cosmological_horizon", "gpc", "10_to_100_mpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "cmb_mm_submm", "optical", "near_ir", "radio_cm_m_lowfreq" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "rest-UV luminosity function Phi(M_UV, z)", "NIRSpec spectroscopic redshifts and Balmer/UV line ratios", "ALMA far-infrared dust continuum" ]	[ "halo-scale star formation efficiency epsilon_", "star formation burstiness amplitude sigma_UV", "stellar initial mass function slope", "stellar mass M_" ]	[ "Eddington bias boosting intrinsically faint stochastic starbursts above flux-limited NIRCam thresholds", "cosmic variance across small deep-field footprints" ]	[ "photometric redshift interloper contamination before NIRSpec confirmation", "stellar population synthesis mass-to-light ratio assumptions" ]	[ "high average star formation efficiency versus high short-timescale UV luminosity scatter versus top-heavy IMF" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Spectroscopically confirmed galaxies up to z ~ 14.32 (JADES-GS-z14-0) demonstrate that the bright-end UV excess is real, but current rest-UV/optical spectra do not uniquely separate bursty star-formation duty cycles from feedback-free high efficiency or IMF variations.	survey_statistical	near_term_1_to_5_years	Wide-area JWST + Roman spectroscopic surveys combined with ALMA dynamical mass and dust constraints and rest-optical H-alpha/continuum duty-cycle measurements across a representative sample of z > 10 galaxies.	Current observations from Planck, JWST, DESI constrain halo-scale star formation efficiency epsilon_*, but systematic uncertainties in photometric redshift interloper contamination before NIRSpec confirmat prevent a definitive resolution.	[ "Baseline astrophysical mechanism in inflation and primordial initial conditions constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Abundance and Luminosity Function of Unexpectedly UV-Bright Galaxies a" ]	[ "High-significance multi-wavelength or dynamical measurement of rest-UV luminosity function Phi(M_UV, z) using Planck, JWST, DESI.", "Breaking the model degeneracy between high average star formation efficiency versus high short-timescale UV luminosity scatter v to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating halo-scale star formation efficiency epsilon_* and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	3	Spectroscopically confirmed galaxies up to z ~ 14.32 (JADES-GS-z14-0) demonstrate that the bright-end UV excess is real, but current rest-UV/optical spectra do not uniquely separate bursty star-formation duty cycles from feedback-free high efficiency or IMF variations.	true	[ { "source_id": "SRC-AST-000020", "support_type": "direct_open_question", "locator": "Section 2: Early Galaxy Assembly and the UV Luminosity Function, Open Question 1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-013659", "citation": "Cueto et al. (2024, A&A 686, A138 (2024))"...	[ "UAST-000001", "UAST-015632", "UAST-006642", "UAST-011557" ]	null	[]	[ "cosmology_early_universe", "inflation_and_primordial_initial_conditions", "z > 10 UV-bright galaxies", "cosmic dawn star formation", "UV luminosity function" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000020).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000003	UAST-000003	uast-000003-physical-origin-of-the-hubble-constant-tension-between-early-universe-cmb-bao-inferen	Physical Origin of the Hubble Constant Tension Between Early-Universe CMB+BAO Inference and Local Distance Ladders	Does the discrepancy between the Hubble constant H_0 inferred from Planck CMB and BAO sound-horizon measurements under LambdaCDM and the local Cepheid-calibrated Type Ia supernova distance ladder (SH0ES) arise from beyond-LambdaCDM early-universe physics or from unmodeled distance-ladder systematics?	Why do measurements of the cosmic expansion rate from the early universe disagree with measurements from nearby stars and supernovae?	Between early-universe sound-horizon determinations (Planck + ACT + SPT + DESI BAO giving H_0 = 67.4-68.0 km s^{-1} Mpc^{-1}) and local distance-ladder calibrations of Type Ia supernovae (SH0ES Cepheids giving H_0 = 73.0 +- 1.0 km s^{-1} Mpc^{-1} versus CCHP TRGB/JAGB calibrations), what accounts for the offset in infe...	dark_matter_dark_energy_fundamental_cosmology	2	Dark Matter, Dark Energy, and Fundamental Cosmology	primordial_black_holes_and_exotic_relics	[]	tension_resolution	[ "dark_sector", "galaxy", "large_scale_structure" ]	population_level	Astrophysical systems in primordial black holes and exotic relics	[ "kpc", "mpc", "gpc" ]	[ { "name": "late_time_acceleration_and_halo_assembly", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "near_ir", "gravitational_wave", "x_ray" ]	[ "Vera C. Rubin Observatory LSST", "Euclid", "DESI", "Nancy Grace Roman Space Telescope", "HST" ]	[ "Cepheid period-luminosity relations", "TRGB and JAGB tip magnitudes in JWST NIRCam", "SNe Ia Hubble diagram", "CMB acoustic peak angular scale theta_*" ]	[ "present-day Hubble constant H_0", "comoving sound horizon r_d", "absolute SNe Ia magnitude M_B" ]	[ "host-galaxy selection and crowding in Cepheid vs TRGB/JAGB calibrator samples" ]	[ "Cepheid metallicity and dust-law slope R_V calibration", "TRGB tip-detection smoothing and zero-point anchoring", "peculiar velocity bulk-flow corrections" ]	[ "early dark energy reducing r_d versus local distance-scale zero-point shift Delta M_B" ]	open	true	partial_observational_constraint	open_consensus	2026-10-16T00:00:00	SH0ES HST+JWST Cepheid measurements maintain a ~5 sigma tension with Planck LambdaCDM, whereas CCHP JWST TRGB and JAGB analyses yield H_0 ~ 69.9 +- 1.7 km s^{-1} Mpc^{-1}, leaving the role of calibrator systematics versus early-universe physics unresolved.	multimessenger	decade_scale	Sub-percent distance-ladder-independent H_0 determinations from gravitational-wave standard sirens and strong-lensing time delays, alongside converged JWST Cepheid/TRGB/JAGB calibrations across >=40 SNe Ia hosts.	Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain present-day Hubble constant H_0, but systematic uncertainties in Cepheid metallicity and dust-law slope R_V calibration prevent a definitive resolution.	[ "Baseline astrophysical mechanism in primordial black holes and exotic relics constrained by Vera C. Rubin Observatory LSST, Euclid", "Alternative non-equilibrium, feedback, or multi-component physical model for Physical Origin of the Hubble Constant Tension Between Early-Universe " ]	[ "High-significance multi-wavelength or dynamical measurement of Cepheid period-luminosity relations using Vera C. Rubin Observatory LSST, Euclid, DESI.", "Breaking the model degeneracy between early dark energy reducing r_d versus local distance-scale zero-point shift Delta M_B to better than 3-5 sigma." ]	Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating present-day Hubble constant H_0 and testing fundamental astrophysical theory.	Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology.	4	SH0ES HST+JWST Cepheid measurements maintain a ~5 sigma tension with Planck LambdaCDM, whereas CCHP JWST TRGB and JAGB analyses yield H_0 ~ 69.9 +- 1.7 km s^{-1} Mpc^{-1}, leaving the role of calibrator systematics versus early-universe physics unresolved.	true	[ { "source_id": "SRC-AST-000014", "support_type": "direct_open_question", "locator": "Section 2: The Hubble Constant Tension, Tension 1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-001315", "citation": "Poulin et al. (2024, arXiv (astro-ph.CO))", "support_type": "explicit...	[ "UAST-000004", "UAST-000024", "UAST-000025", "UAST-000026", "UAST-000027", "UAST-000028", "UAST-000029", "UAST-000374", "UAST-000375", "UAST-000376", "UAST-000377", "UAST-000378", "UAST-000379", "UAST-000380", "UAST-000381", "UAST-004510", "UAST-004169", "UAST-004866" ]	null	[]	[ "dark_matter_dark_energy_fundamental_cosmology", "primordial_black_holes_and_exotic_relics", "Hubble constant H_0", "local distance ladder", "cosmic sound horizon r_d" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000014).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000004	UAST-000004	uast-000004-dynamical-evolution-of-dark-energy-equation-of-state-w-z-suggested-by-desi-bao-type-i	Dynamical Evolution of Dark Energy Equation of State w(z) Suggested by DESI BAO + Type Ia Supernova Combinations	Is cosmic acceleration driven by a time-independent cosmological constant (w = -1), or does dark energy evolve dynamically with redshift (w_0 > -1, w_a < 0) as hinted by joint DESI baryon acoustic oscillation, CMB, and Type Ia supernova analyses?	Is dark energy a fixed cosmological constant, or is its strength changing over cosmic time?	In the Chevallier-Polarski-Linder parameterization w(a) = w_0 + w_a(1 - a) fitted to transverse and radial BAO distances D_M(z)/r_d and D_H(z)/r_d across 0.1 < z < 2.5 together with CMB and SNe Ia (Pantheon+, Union3, DES-SN5YR), does the preference for w_0 > -1 and w_a < 0 reflect dynamical dark energy or supernova red...	dark_matter_dark_energy_fundamental_cosmology	2	Dark Matter, Dark Energy, and Fundamental Cosmology	primordial_black_holes_and_exotic_relics	[]	population_evolution	[ "dark_sector", "galaxy", "large_scale_structure" ]	population_level	Astrophysical systems in primordial black holes and exotic relics	[ "kpc", "mpc", "gpc" ]	[ { "name": "late_time_acceleration_and_halo_assembly", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "near_ir", "gravitational_wave", "x_ray" ]	[ "Vera C. Rubin Observatory LSST", "Euclid", "DESI", "Nancy Grace Roman Space Telescope", "HST" ]	[ "anisotropic BAO distance ratios D_M(z)/r_d and D_H(z)/r_d", "SNe Ia luminosity distance modulus mu(z)", "full-shape galaxy power spectrum P(k)" ]	[ "dark energy equation-of-state parameters (w_0, w_a)", "matter density parameter Omega_m" ]	[ "Malmquist and host-mass step selection biases in high-redshift photometric SNe Ia compilations" ]	[ "photometric calibration offsets between low-z anchor SNe and high-z rolling survey SNe", "prior volume effects in (w_0, w_a) parameterization" ]	[ "evolving dark energy w(z) versus spatial curvature Omega_k, neutrino mass sum m_nu, and SNe Ia progenitor evolution" ]	open	true	partial_observational_constraint	open_consensus	2026-10-16T00:00:00	DESI 2024 BAO + CMB + SNe Ia shows a 2.5-3.9 sigma preference for (w_0 > -1, w_a < 0) depending on the supernova compilation used (Pantheon+, Union3, DES-SN5YR), which has not yet reached the 5-sigma discovery threshold or excluded supernova calibration systematics.	multimessenger	decade_scale	Full 5-year DESI spectroscopic BAO + RSD dataset combined with Euclid, Roman, and Rubin LSST homogeneously calibrated SNe Ia and weak-lensing growth measurements.	Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain dark energy equation-of-state parameters (w_0, w_a), but systematic uncertainties in photometric calibration offsets between low-z anchor SNe and high-z ro prevent a definitive resolution.	[ "Baseline astrophysical mechanism in primordial black holes and exotic relics constrained by Vera C. Rubin Observatory LSST, Euclid", "Alternative non-equilibrium, feedback, or multi-component physical model for Dynamical Evolution of Dark Energy Equation of State w(z) Suggested by" ]	[ "High-significance multi-wavelength or dynamical measurement of anisotropic BAO distance ratios D_M(z)/r_d and D_H(z)/r_d using Vera C. Rubin Observatory LSST, Euclid, DESI.", "Breaking the model degeneracy between evolving dark energy w(z) versus spatial curvature Omega_k, neutrino mass sum m_nu, and SN to bette...	Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating dark energy equation-of-state parameters (w_0, w_a) and testing fundamental astrophysical theory.	Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology.	4	DESI 2024 BAO + CMB + SNe Ia shows a 2.5-3.9 sigma preference for (w_0 > -1, w_a < 0) depending on the supernova compilation used (Pantheon+, Union3, DES-SN5YR), which has not yet reached the 5-sigma discovery threshold or excluded supernova calibration systematics.	true	[ { "source_id": "SRC-AST-000019", "support_type": "direct_open_question", "locator": "Section 5: Dark Energy and Modified Gravity Constraints, Result w0-wa", "verbatim_quote_used": false }, { "source_id": "SRC-AST-000974", "citation": "Favale et al. (2025, Mon Not R Astron Soc (2026))", ...	[ "UAST-000003", "UAST-004169", "UAST-004275", "UAST-003852" ]	null	[]	[ "dark_matter_dark_energy_fundamental_cosmology", "primordial_black_holes_and_exotic_relics", "dark energy equation of state w(z)", "baryon acoustic oscillations", "cosmic expansion history" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000019).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000005	UAST-000005	uast-000005-spatial-distribution-and-baryon-partition-of-the-warm-hot-intergalactic-medium-across	Spatial Distribution and Baryon Partition of the Warm-Hot Intergalactic Medium Across Cosmic Web Filaments	How are the low-redshift 'missing baryons' partitioned in temperature, density, and metallicity between the diffuse warm-hot intergalactic medium (WHIM, 10^5-10^7 K) in cosmic web filaments and the outer circumgalactic halos of galaxies?	Where exactly does normal matter reside between galaxies in the modern universe, and how much of it is in cosmic web filaments versus extended galaxy halos?	At redshifts z < 1, what fraction of the cosmic baryon budget Omega_b resides in unvirialized cosmic-web filaments versus virialized halo gas as a function of overdensity delta_b and temperature T, and how do AGN and supernova outflows heat and enrich this gas?	large_scale_structure_igm_cosmic_web	3	Large-Scale Structure, Intergalactic Medium, and Cosmic Web	intergalactic_medium_and_lya_forest	[]	object_nature	[ "large_scale_structure", "intergalactic_medium", "circumgalactic_medium", "galaxy_cluster" ]	population_level	Astrophysical systems in intergalactic medium and lya forest	[ "kpc", "mpc", "10_to_100_mpc" ]	[ { "name": "cosmic_noon_to_present", "redshift_min": 0, "redshift_max": 5, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 12.6 } ]	[ "uv", "optical", "x_ray", "cmb_mm_submm", "radio_cm_m_lowfreq" ]	[ "DESI", "XRISM", "eROSITA", "ACT", "SPT-3G" ]	[ "fast radio burst dispersion measure DM(z)", "O VII and O VIII X-ray absorption/emission lines", "thermal and kinematic Sunyaev-Zel'dovich profiles" ]	[ "baryon mass fraction f_WHIM", "electron density profile n_e(r)", "IGM metallicity Z_IGM and temperature T_WHIM" ]	[ "sightline bias toward overdense galaxy groups in stacked tSZ/X-ray filament analyses" ]	[ "host-galaxy and Milky Way halo DM subtraction in localized FRB samples", "non-equilibrium ionization and clumping factor C = <n_e^2>/<n_e>^2" ]	[ "electron column density versus gas metallicity in X-ray O VII/O VIII absorption" ]	partially_solved	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Localized fast radio bursts (Macquart relation) and stacked tSZ/X-ray filaments confirm that the total cosmic baryon density Omega_b is present at low redshift, but the radial partition between extended circumgalactic halos and diffuse intergalactic filaments remains model-dependent.	survey_statistical	near_term_1_to_5_years	Joint tomography using >=1,000 host-localized FRBs (DSA-2000, CHIME Outriggers, SKA), high-resolution X-ray microcalorimeter absorption spectra (XRISM, NewAthena, Arcus), and CMB-S4/Simons Observatory kSZ profiling.	Current observations from DESI, XRISM, eROSITA constrain baryon mass fraction f_WHIM, but systematic uncertainties in host-galaxy and Milky Way halo DM subtraction in localized FRB samples prevent a definitive resolution.	[ "Baseline astrophysical mechanism in intergalactic medium and lya forest constrained by DESI, XRISM", "Alternative non-equilibrium, feedback, or multi-component physical model for Spatial Distribution and Baryon Partition of the Warm-Hot Intergalacti" ]	[ "High-significance multi-wavelength or dynamical measurement of fast radio burst dispersion measure DM(z) using DESI, XRISM, eROSITA.", "Breaking the model degeneracy between electron column density versus gas metallicity in X-ray O VII/O VIII absorption to better than 3-5 sigma." ]	Resolving this question in Large-Scale Structure, Intergalactic Medium, and Cosmic Web is essential for calibrating baryon mass fraction f_WHIM and testing fundamental astrophysical theory.	Cosmological hydrodynamics, radiative cooling and photoionization equilibrium, X-ray and Sunyaev-Zel'dovich cluster physics, and Lyman-alpha forest statistics.	3	Localized fast radio bursts (Macquart relation) and stacked tSZ/X-ray filaments confirm that the total cosmic baryon density Omega_b is present at low redshift, but the radial partition between extended circumgalactic halos and diffuse intergalactic filaments remains model-dependent.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Cosmic Ecosystems: Unveiling the Drivers of Galaxy Growth, Question CE-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-005328", "citation": "Zhai et al. (2026, arXiv (astro-ph.CO))", "sup...	[ "UAST-000030", "UAST-000031", "UAST-000032", "UAST-000033", "UAST-000034", "UAST-000035", "UAST-000576", "UAST-000577", "UAST-000578", "UAST-000579", "UAST-000580", "UAST-000581", "UAST-000582", "UAST-000583", "UAST-000584", "UAST-008084", "UAST-010053", "UAST-008116" ]	null	[]	[ "large_scale_structure_igm_cosmic_web", "intergalactic_medium_and_lya_forest", "warm-hot intergalactic medium (WHIM)", "cosmic web filaments", "missing baryon budget" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000006	UAST-000006	uast-000006-seeding-mechanism-of-overmassive-black-holes-at-redshifts-z-6-light-population-iii-re	Seeding Mechanism of Overmassive Black Holes at Redshifts z > 6: Light Population III Remnants versus Heavy Direct-Collapse Seeds	Did the supermassive black holes of mass 10^7-10^9 M_sun observed by JWST and quasar surveys at redshifts z > 6 grow from light Population III stellar remnants (~10^2 M_sun) via sustained super-Eddington accretion, from intermediate-mass runaway cluster collapses (~10^3 M_sun), or from heavy direct-collapse black hole ...	How did the first giant black holes in the universe grow so massive in less than a billion years after the Big Bang?	For the population of broad-line AGN and quasars at 6 <= z <= 11 discovered by JWST and wide-field surveys, what initial seed mass function dN/dM_seed at z = 15-30 and Eddington duty-cycle distribution f_Edd(t) produce the observed black hole mass function and elevated M_BH / M_* ratios?	galaxies_supermassive_black_holes	4	Galaxies and Supermassive Black Holes	high_redshift_galaxy_formation_and_first_galaxies	[]	model_discrimination	[ "galaxy", "agn_quasar", "compact_object" ]	population_level	Astrophysical systems in high redshift galaxy formation and first galaxies	[ "pc", "kpc", "mpc" ]	[ { "name": "first_galaxies_through_cosmic_noon", "redshift_min": 0, "redshift_max": 14, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 13.5 } ]	[ "near_ir", "mid_ir", "optical", "mm_submm", "x_ray", "radio_cm_m_lowfreq" ]	[ "JWST", "ALMA", "Chandra", "VLT/MUSE", "SDSS/BOSS" ]	[ "JWST broad H-alpha/H-beta line widths and luminosities", "black hole-to-stellar mass ratio M_BH/M_* at z = 6-10", "LISA gravitational-wave merger rates at z > 10" ]	[ "seed mass distribution M_seed", "time-averaged Eddington accretion ratio lambda_Edd", "black hole occupation fraction in dwarf/high-z galaxies" ]	[ "Lauer bias and flux-limit selection favoring the highest-M_BH/M_* outliers in high-z spectroscopic samples" ]	[ "single-epoch virial black hole mass calibration uncertainties at high redshift and super-Eddington rates", "X-ray weakness and Compton-thick obscuration in JWST 'Little Red Dots'" ]	[ "heavy initial seed mass M_seed ~ 10^5 M_sun with sub-Eddington growth versus light seed M_seed ~ 100 M_sun with episodic super-Eddington accretion" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	JWST has revealed abundant broad-line AGN and compact 'Little Red Dots' at z = 5-10 with apparent M_BH/M_* ratios 10-100x above local relations, but virial mass systematics and lack of direct z > 10 gravitational-wave detections prevent distinguishing heavy seeds from super-Eddington light seeds.	observational_and_theoretical	decade_scale	Direct detection of black hole seed mergers at z = 10-20 with LISA, combined with reverberation mapping and X-ray/infrared spectral disentangling of z > 7 AGN with JWST, NewAthena, and ELTs.	Current observations from JWST, ALMA, Chandra constrain seed mass distribution M_seed, but systematic uncertainties in single-epoch virial black hole mass calibration uncertainties at high prevent a definitive resolution.	[ "Baseline astrophysical mechanism in high redshift galaxy formation and first galaxies constrained by JWST, ALMA", "Alternative non-equilibrium, feedback, or multi-component physical model for Seeding Mechanism of Overmassive Black Holes at Redshifts z > 6: Light" ]	[ "High-significance multi-wavelength or dynamical measurement of JWST broad H-alpha/H-beta line widths and luminosities using JWST, ALMA, Chandra.", "Breaking the model degeneracy between heavy initial seed mass M_seed ~ 10^5 M_sun with sub-Eddington growth versus light seed M_ to better than 3-5 sigma." ]	Resolving this question in Galaxies and Supermassive Black Holes is essential for calibrating seed mass distribution M_seed and testing fundamental astrophysical theory.	Galaxy formation and evolution, active galactic nucleus accretion and feedback physics, stellar population synthesis, and galactic dynamics.	4	JWST has revealed abundant broad-line AGN and compact 'Little Red Dots' at z = 5-10 with apparent M_BH/M_* ratios 10-100x above local relations, but virial mass systematics and lack of direct z > 10 gravitational-wave detections prevent distinguishing heavy seeds from super-Eddington light seeds.	true	[ { "source_id": "SRC-AST-000011", "support_type": "direct_open_question", "locator": "LISA Science Objective 2: Trace the Origin and Growth of Massive Black Holes, Objective SO2", "verbatim_quote_used": false }, { "source_id": "SRC-AST-022601", "citation": "Ellis et al. (2023, ApJ 964 11 ...	[ "UAST-000036", "UAST-000037", "UAST-000038", "UAST-000039", "UAST-000040", "UAST-000041", "UAST-000814", "UAST-000815", "UAST-000816", "UAST-000817", "UAST-000818", "UAST-000819", "UAST-000820", "UAST-000821", "UAST-000822", "UAST-023721", "UAST-012071", "UAST-011713" ]	null	[]	[ "galaxies_supermassive_black_holes", "high_redshift_galaxy_formation_and_first_galaxies", "high-redshift supermassive black hole seeds", "direct-collapse black holes", "JWST broad-line AGN" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000011).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000007	UAST-000007	uast-000007-core-cusp-density-profiles-and-dark-subhalo-abundance-in-milky-way-ultra-faint-dwarf	Core-Cusp Density Profiles and Dark Subhalo Abundance in Milky Way Ultra-Faint Dwarf Galaxies and Stellar Streams	Do the central dark matter density profiles of ultra-faint dwarf galaxies (M_* < 10^5 M_sun) and the perturbation spectrum of cold Milky Way stellar streams match collisionless cold dark matter predictions (steep cusps and abundant 10^6-10^8 M_sun dark subhalos), or do they require self-interacting, warm, or wave-like ...	Are the centers of the faintest dwarf galaxies and the gaps in Milky Way star streams consistent with standard cold dark matter, or do they point to dark matter with new particle properties?	In Milky Way ultra-faint dwarf galaxies where supernova baryonic core formation is energetically negligible (M_*/M_halo < 10^{-4}) and along thin globular-cluster stellar streams (such as GD-1 and Pal 5), what are the inner logarithmic dark matter density slope gamma = -d ln rho / d ln r and the subhalo mass function d...	milky_way_local_group_near_field	5	Milky Way, Local Group, and Near-Field Cosmology	galactic_center_and_fermi_erosita_bubbles	[]	mechanism	[ "milky_way_component", "stellar_population", "galaxy", "dark_sector" ]	population_level	Astrophysical systems in galactic center and fermi erosita bubbles	[ "pc", "kpc" ]	[ { "name": "milky_way_assembly_history", "redshift_min": 0, "redshift_max": 4, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 12.2 } ]	[ "optical", "near_ir", "radio_cm_m_lowfreq", "gamma_ray", "x_ray" ]	[ "Gaia", "SDSS-V", "APOGEE", "GALAH", "WEAVE" ]	[ "3D stellar velocity dispersions and Gaia proper motions in ultra-faint dwarfs", "stellar stream density gaps and spur phase-space perturbations", "strong-lensing flux-ratio and image perturbations" ]	[ "inner dark matter density slope gamma(r < 100 pc)", "subhalo mass function dN/dM_sub at 10^6-10^8 M_sun", "dark matter self-interaction cross section sigma/m or particle mass m_WDM" ]	[ "surface-brightness completeness limits in satellite discovery prior to Rubin LSST", "tidal disruption of inner-halo subhalos by the Milky Way disk" ]	[ "velocity anisotropy beta(r) degeneracy in Jeans dynamical modeling", "unresolved binary-star orbital velocity inflation", "baryonic perturbation of streams by giant molecular clouds and the Galactic bar" ]	[ "Jeans mass-anisotropy degeneracy between a cored halo with tangential orbits and a cuspy NFW halo with radial orbits" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Line-of-sight velocity dispersions alone suffer from the Jeans mass-anisotropy degeneracy, and observed stream gaps in GD-1 must be separated from baryonic substructures in the Milky Way disk and halo.	observational_and_theoretical	near_term_1_to_5_years	Internal 3D plane-of-sky proper motion dispersions of >=20 ultra-faint dwarfs from Gaia + Roman + 30m-class ELTs together with Rubin LSST + Desi/Spec-S5 phase-space mapping of >=50 cold stellar streams.	Current observations from Gaia, SDSS-V, APOGEE constrain inner dark matter density slope gamma(r < 100 pc), but systematic uncertainties in velocity anisotropy beta(r) degeneracy in Jeans dynamical modeling prevent a definitive resolution.	[ "Baseline astrophysical mechanism in galactic center and fermi erosita bubbles constrained by Gaia, SDSS-V", "Alternative non-equilibrium, feedback, or multi-component physical model for Core-Cusp Density Profiles and Dark Subhalo Abundance in Milky Way Ult" ]	[ "High-significance multi-wavelength or dynamical measurement of 3D stellar velocity dispersions and Gaia proper motions in ultra-faint dwarfs using Gaia, SDSS-V, APOGEE.", "Breaking the model degeneracy between Jeans mass-anisotropy degeneracy between a cored halo with tangential orbits and a cuspy N to better th...	Resolving this question in Milky Way, Local Group, and Near-Field Cosmology is essential for calibrating inner dark matter density slope gamma(r < 100 pc) and testing fundamental astrophysical theory.	Galactic dynamics, action-angle phase-space modeling, stellar nucleosynthesis and chemical evolution, and Local Group near-field cosmology.	3	Line-of-sight velocity dispersions alone suffer from the Jeans mass-anisotropy degeneracy, and observed stream gaps in GD-1 must be separated from baryonic substructures in the Milky Way disk and halo.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Panel on Galaxies and Near-Field Cosmology, Question NFC-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-003601", "citation": "Yang et al. (2024, ApJ, 1001:54 (2026))", "support_type": "e...	[ "UAST-000042", "UAST-000043", "UAST-000044", "UAST-000045", "UAST-000046", "UAST-000047", "UAST-001122", "UAST-001123", "UAST-001124", "UAST-001125", "UAST-001126", "UAST-001127", "UAST-001128", "UAST-001129", "UAST-001130", "UAST-006595", "UAST-006246", "UAST-001136" ]	null	[]	[ "milky_way_local_group_near_field", "galactic_center_and_fermi_erosita_bubbles", "ultra-faint dwarf galaxies", "Milky Way stellar streams", "dark matter subhalo mass function" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000008	UAST-000008	uast-000008-relative-roles-of-magnetic-fields-supersonic-turbulence-and-stellar-feedback-in-regul	Relative Roles of Magnetic Fields, Supersonic Turbulence, and Stellar Feedback in Regulating the Low Efficiency of Molecular Cloud Star Formation	What quantitative balance among magnetohydrodynamic turbulence, magnetic flux support (mass-to-flux ratio mu_Phi), and protostellar/massive-star feedback restricts the star formation efficiency per free-fall time in giant molecular clouds to epsilon_ff ~ 1% across diverse galactic environments?	Why do giant interstellar gas clouds convert only about one percent of their mass into stars during each gravitational collapse timescale?	Across giant molecular clouds and dense clumps from local spiral disks to starburst and high-redshift environments, how do the virial parameter alpha_vir, sonic Mach number M_s, Alfvénic Mach number M_A, and radiative/momentum feedback jointly set the star formation efficiency per free-fall time epsilon_ff and the core...	ism_star_formation_astrochemistry	6	Interstellar Medium, Star Formation, and Astrochemistry	astrochemistry_and_complex_organic_molecules	[]	mechanism	[ "interstellar_medium", "dust_and_ice", "star" ]	population_level	Astrophysical systems in astrochemistry and complex organic molecules	[ "au", "pc", "kpc" ]	[ { "name": "present_day_and_galactic_ism", "redshift_min": 0, "redshift_max": 2, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 10.4 } ]	[ "mm_submm", "far_ir", "mid_ir", "radio_cm_m_lowfreq", "uv" ]	[ "ALMA", "JWST", "NOEMA", "VLA", "ngVLA" ]	[ "Zeeman splitting and dust polarization maps", "molecular line velocity dispersion-size relations", "dense-gas HCN/HCO+/CO ratios and young stellar object counts" ]	[ "star formation efficiency per free-fall time epsilon_ff", "mass-to-magnetic-flux ratio mu_Phi", "turbulent driving scale and compressive-to-solenoidal ratio" ]	[ "evolutionary snapshot bias when inferring cloud-lifetime epsilon_ff from instantaneous YSO-to-gas ratios" ]	[ "CO-to-H2 conversion factor X_CO and HCN optical-depth variations", "Davis-Chandrasekhar-Fermi magnetic field strength calibration uncertainties", "radiative transfer and dust grain alignment efficiency" ]	[ "gravoturbulent fragmentation regulated by supersonic turbulence versus magnetically subcritical ambipolar-diffusion regulation" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Both turbulence-regulated (gravo-turbulent) and magnetically regulated models can reproduce epsilon_ff ~ 0.01 in simulations, while 3D magnetic field strengths at the prestellar core scale remain difficult to measure directly across large cloud samples.	observational_and_theoretical	near_term_1_to_5_years	High-resolution ALMA and ngVLA Zeeman + dust-polarization and kinematic surveys across thousands of cores spanning Milky Way and PHANGS extragalactic clouds, benchmarked against radiation-MHD simulations resolving 0.01 pc scales.	Current observations from ALMA, JWST, NOEMA constrain star formation efficiency per free-fall time epsilon_ff, but systematic uncertainties in CO-to-H2 conversion factor X_CO and HCN optical-depth variations prevent a definitive resolution.	[ "Baseline astrophysical mechanism in astrochemistry and complex organic molecules constrained by ALMA, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Relative Roles of Magnetic Fields, Supersonic Turbulence, and Stellar " ]	[ "High-significance multi-wavelength or dynamical measurement of Zeeman splitting and dust polarization maps using ALMA, JWST, NOEMA.", "Breaking the model degeneracy between gravoturbulent fragmentation regulated by supersonic turbulence versus magnetically subcri to better than 3-5 sigma." ]	Resolving this question in Interstellar Medium, Star Formation, and Astrochemistry is essential for calibrating star formation efficiency per free-fall time epsilon_ff and testing fundamental astrophysical theory.	Magnetohydrodynamic interstellar turbulence, radiative transfer in molecular lines and dust continuum, star formation physics, and astrochemical reaction networks.	3	Both turbulence-regulated (gravo-turbulent) and magnetically regulated models can reproduce epsilon_ff ~ 0.01 in simulations, while 3D magnetic field strengths at the prestellar core scale remain difficult to measure directly across large cloud samples.	true	[ { "source_id": "SRC-AST-000007", "support_type": "direct_open_question", "locator": "ngVLA Key Science Goal 3: Star Formation and the Interstellar Medium, KSG 3.1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-032610", "citation": "Bertram et al. (2011, arXiv (astro-ph.SR))", ...	[ "UAST-000048", "UAST-000049", "UAST-000050", "UAST-000051", "UAST-000052", "UAST-000053", "UAST-001325", "UAST-001326", "UAST-001327", "UAST-001328", "UAST-001329", "UAST-001330", "UAST-001331", "UAST-001332", "UAST-001333", "UAST-032884", "UAST-016091", "UAST-011510" ]	null	[]	[ "ism_star_formation_astrochemistry", "astrochemistry_and_complex_organic_molecules", "giant molecular clouds", "star formation efficiency epsilon_ff", "interstellar magnetic fields and turbulence" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000007).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000009	UAST-000009	uast-000009-physical-mechanism-of-common-envelope-ejection-and-orbital-shrinkage-in-interacting-b	Physical Mechanism of Common-Envelope Ejection and Orbital Shrinkage in Interacting Binary Stars	During common-envelope evolution in close binary stars, what combination of gravitational drag, hydrogen/helium ionization recombination energy, magnetohydrodynamic jets, and dust-driven winds ejects the shared stellar envelope and sets the final post-common-envelope orbital separation?	When a giant star engulfs its companion star, what physical forces eject the shared gas envelope and determine how close the two stellar cores end up?	In binary systems undergoing dynamically unstable mass transfer onto a main-sequence or compact companion, what fraction of the released orbital binding energy (alpha_CE) and internal recombination/enthalpy energy unbinds the envelope without causing a premature stellar merger, and how does this depend on donor mass M_...	stars_stellar_populations_evolution	7	Stars, Stellar Populations, and Stellar Evolution	binary_and_multiple_star_evolution	[]	population_evolution	[ "star", "stellar_population", "transient" ]	population_level	Astrophysical systems in binary and multiple star evolution	[ "1000km_to_rsun", "au", "pc" ]	[ { "name": "stellar_evolution_across_metallicity", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "uv", "near_ir", "mid_ir", "x_ray" ]	[ "Kepler", "TESS", "PLATO", "Gaia", "HST" ]	[ "post-common-envelope binary period-mass distributions", "light curves and ejecta kinematics of luminous red novae", "compact binary merger rate densities" ]	[ "common-envelope ejection efficiency alpha_CE", "recombination energy thermalization fraction", "post-infall final orbital separation a_f" ]	[ "observational bias toward short-period eclipsing post-CE white dwarf + M-dwarf binaries" ]	[ "3D radiation-hydrodynamic spatial resolution near the inspiraling companion cores", "convective energy transport and radiation leakage timescales during hydrogen recombination" ]	[ "orbital energy conversion efficiency alpha_CE versus internal thermal/recombination energy and jet-assisted envelope removal" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Three-dimensional hydrodynamic simulations of the dynamical plunge typically stall before unbinding the entire envelope unless recombination energy or jets are included, leaving population synthesis models reliant on phenomenological alpha_CE prescriptions that vary by an order of magnitude.	observational_and_theoretical	near_term_1_to_5_years	3D radiation-magnetohydrodynamic simulations spanning the dynamical plunge to thermal relaxation, tested against Rubin LSST luminous red nova transient demographics and Gaia DR4/DR5 post-CE binary populations.	Current observations from Kepler, TESS, PLATO constrain common-envelope ejection efficiency alpha_CE, but systematic uncertainties in 3D radiation-hydrodynamic spatial resolution near the inspiraling comp prevent a definitive resolution.	[ "Baseline astrophysical mechanism in binary and multiple star evolution constrained by Kepler, TESS", "Alternative non-equilibrium, feedback, or multi-component physical model for Physical Mechanism of Common-Envelope Ejection and Orbital Shrinkage i" ]	[ "High-significance multi-wavelength or dynamical measurement of post-common-envelope binary period-mass distributions using Kepler, TESS, PLATO.", "Breaking the model degeneracy between orbital energy conversion efficiency alpha_CE versus internal thermal/recombination energy to better than 3-5 sigma." ]	Resolving this question in Stars, Stellar Populations, and Stellar Evolution is essential for calibrating common-envelope ejection efficiency alpha_CE and testing fundamental astrophysical theory.	Stellar structure and evolution, asteroseismology, radiation-driven stellar winds, binary interaction and common-envelope hydrodynamics, and core-collapse supernova physics.	3	Three-dimensional hydrodynamic simulations of the dynamical plunge typically stall before unbinding the entire envelope unless recombination energy or jets are included, leaving population synthesis models reliant on phenomenological alpha_CE prescriptions that vary by an order of magnitude.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Panel on Stars, the Sun, and Stellar Populations, Question SSP-2", "verbatim_quote_used": false }, { "source_id": "SRC-AST-008572", "citation": "Alonso-Álvarez et al. (2024, arXiv (astro-ph.CO))", "s...	[ "UAST-000054", "UAST-000055", "UAST-000056", "UAST-000057", "UAST-000058", "UAST-000059", "UAST-001598", "UAST-001599", "UAST-001600", "UAST-001601", "UAST-001602", "UAST-001603", "UAST-001604", "UAST-001605", "UAST-001606", "UAST-011021", "UAST-033681", "UAST-028507" ]	null	[]	[ "stars_stellar_populations_evolution", "binary_and_multiple_star_evolution", "common-envelope binary evolution", "luminous red novae", "close compact-object binary progenitors" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000010	UAST-000010	uast-000010-cold-dense-matter-equation-of-state-and-existence-of-deconfined-quark-cores-inside-ma	Cold Dense Matter Equation of State and Existence of Deconfined Quark Cores Inside Massive Neutron Stars	What is the cold supranuclear equation of state P(epsilon) inside neutron stars at densities of 2-8 times nuclear saturation density, and do massive neutron stars (~2 M_sun) contain deconfined quark matter or hyperonic cores via a first-order phase transition or smooth crossover?	What form of matter exists at the ultra-dense centers of the heaviest neutron stars—ordinary neutrons and protons, exotic hyperons, or deconfined quark matter?	At baryon number densities 2 n_0 <= n_B <= 8 n_0 and zero temperature in beta-equilibrated neutron-star interiors, what is the speed-of-sound profile c_s^2(n_B) = dP/d epsilon, the maximum Tolman-Oppenheimer-Volkoff mass M_TOV, and does a strong first-order deconfinement phase transition produce twin-star mass-radius b...	compact_objects_accretion_high_energy	8	Compact Objects, Accretion, and High-Energy Astrophysics	white_dwarfs_and_thermonuclear_transients	[]	mechanism	[ "compact_object", "star", "nonthermal_particle" ]	population_level	Astrophysical systems in white dwarfs and thermonuclear transients	[ "km_to_1000km", "1000km_to_rsun", "au" ]	[ { "name": "compact_object_populations", "redshift_min": 0, "redshift_max": 1.5, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 9.3 } ]	[ "x_ray", "radio_cm_m_lowfreq", "gamma_ray", "gravitational_wave", "optical" ]	[ "NICER", "IXPE", "XRISM", "Chandra", "XMM-Newton" ]	[ "NICER X-ray pulse-profile mass-radius posteriors", "radio pulsar Shapiro delay masses (PSR J0740+6620)", "binary neutron star tidal deformability Lambda and post-merger kilohertz GW peak frequency f_2" ]	[ "pressure-energy density relation P(epsilon)", "sound speed squared c_s^2(n_B)", "maximum non-rotating neutron star mass M_TOV", "quark deconfinement threshold density" ]	[ "mass distribution of binary neutron stars in LIGO/Virgo/KAGRA clustering near 1.35 M_sun" ]	[ "NICER hot-spot surface geometry and atmospheric composition modeling", "nuclear chiral EFT truncation above 1.5 n_0 and perturbative QCD matching below 40 n_0" ]	[ "hadronic equation of state with repulsive three-body forces versus hybrid crossover quark-hadron equation of state (masquerade problem)" ]	open	true	partial_observational_constraint	open_consensus	2026-10-16T00:00:00	NICER radius measurements (~12.4 km at 1.4 and 2.08 M_sun) and GW170817 tidal deformability rule out extreme soft and stiff equations of state, but smooth quark-hadron crossovers and stiff nucleonic models yield nearly identical macroscopic M(R) curves ('the masquerade problem').	multimessenger	decade_scale	Sub-2% radius measurements across 1.2-2.2 M_sun neutron stars with NewAthena/eXTP, together with kilohertz post-merger gravitational-wave spectroscopy in Cosmic Explorer and Einstein Telescope detecting or excluding a phase-transition frequency shift Delta f_2.	Current observations from NICER, IXPE, XRISM constrain pressure-energy density relation P(epsilon), but systematic uncertainties in NICER hot-spot surface geometry and atmospheric composition modeling prevent a definitive resolution.	[ "Baseline astrophysical mechanism in white dwarfs and thermonuclear transients constrained by NICER, IXPE", "Alternative non-equilibrium, feedback, or multi-component physical model for Cold Dense Matter Equation of State and Existence of Deconfined Quark " ]	[ "High-significance multi-wavelength or dynamical measurement of NICER X-ray pulse-profile mass-radius posteriors using NICER, IXPE, XRISM.", "Breaking the model degeneracy between hadronic equation of state with repulsive three-body forces versus hybrid crossover quark- to better than 3-5 sigma." ]	Resolving this question in Compact Objects, Accretion, and High-Energy Astrophysics is essential for calibrating pressure-energy density relation P(epsilon) and testing fundamental astrophysical theory.	General relativistic compact objects, supranuclear dense matter equations of state, pulsar magnetospheric electrodynamics, and black hole accretion disk/jet magnetohydrodynamics.	4	NICER radius measurements (~12.4 km at 1.4 and 2.08 M_sun) and GW170817 tidal deformability rule out extreme soft and stiff equations of state, but smooth quark-hadron crossovers and stiff nucleonic models yield nearly identical macroscopic M(R) curves ('the masquerade problem').	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Panel on Compact Objects and Energetic Phenomena, Question COEP-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-019660", "citation": "German (2023, Astrophysics & Astronomy Literature)", ...	[ "UAST-000060", "UAST-000061", "UAST-000062", "UAST-000063", "UAST-000064", "UAST-000065", "UAST-001871", "UAST-001872", "UAST-001873", "UAST-001874", "UAST-001875", "UAST-001876", "UAST-001877", "UAST-001878", "UAST-001879", "UAST-021052", "UAST-020727", "UAST-022515" ]	null	[]	[ "compact_objects_accretion_high_energy", "white_dwarfs_and_thermonuclear_transients", "neutron star interior equation of state", "deconfined quark cores", "maximum neutron star mass M_TOV" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000011	UAST-000011	uast-000011-emission-mechanism-and-progenitor-diversity-of-repeating-versus-apparently-non-repeat	Emission Mechanism and Progenitor Diversity of Repeating versus Apparently Non-Repeating Fast Radio Bursts	Are all extragalactic fast radio bursts powered by magnetars formed across both core-collapse and delayed merger/accretion-induced collapse channels, and is their coherent gigahertz radio emission generated inside the closed magnetosphere near the neutron star surface or in relativistic magnetized shocks at >>10^{10} c...	Do all fast radio bursts come from highly magnetized neutron stars, and is the radio flash produced close to the star's surface or far out in a shock wave?	Across the extragalactic fast radio burst population, do repeating and apparently one-off FRBs represent distinct progenitor classes or evolutionary stages of magnetar engines, and does the coherent radiation mechanism operate via magnetospheric curvature/maser plasma processes at r ~ 10^6-10^8 cm or synchrotron maser ...	transients_gravitational_waves_multimessenger	9	Transients, Gravitational Waves, and Multi-Messenger Astronomy	fast_radio_bursts_and_coherent_radio_transients	[]	origin	[ "transient", "compact_object", "galaxy" ]	population_level	Astrophysical systems in fast radio bursts and coherent radio transients	[ "km_to_1000km", "au", "pc", "gpc" ]	[ { "name": "time_domain_and_multimessenger_universe", "redshift_min": 0, "redshift_max": 6, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 12.8 } ]	[ "gravitational_wave", "radio_cm_m_lowfreq", "optical", "x_ray", "gamma_ray", "near_ir" ]	[ "LIGO-Virgo-KAGRA", "CHIME/FRB", "DSA-110", "ASKAP", "NANOGrav/EPTA/PPTA/IPTA" ]	[ "sub-microsecond burst temporal microstructure", "polarization position-angle swings and circular polarization fractions", "host-galaxy stellar population ages and globular-cluster offsets (e.g., FRB 20200120E in M81)" ]	[ "emission radius r_em", "Lorentz factor and magnetization sigma of the emitting plasma", "progenitor delay-time distribution" ]	[ "instrumental fluence thresholds and repetition-rate censorship making low-rate repeaters appear one-off" ]	[ "propagation-induced Faraday conversion, scintillation, and plasma lensing in the circumburst medium" ]	[ "intrinsic magnetospheric polarization swings versus propagation effects in a magnetized wind nebula" ]	partially_solved	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	While FRB 200428 from Galactic magnetar SGR 1935+2154 established that magnetars can produce FRBs, the discovery of FRB 20200120E in an old M81 globular cluster requires delayed formation channels, and nanosecond-to-microsecond temporal structures and polarization swings challenge pure far-away shock models while high-...	multimessenger	near_term_1_to_5_years	Sub-arcsecond VLBI localization and polarimetric microstructure analysis of >=1,000 repeaters and non-repeaters with CHIME Outriggers, DSA-2000, and SKAO, plus simultaneous X-ray/optical counterpart detections.	Current observations from LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110 constrain emission radius r_em, but systematic uncertainties in propagation-induced Faraday conversion, scintillation, and plasma lens prevent a definitive resolution.	[ "Baseline astrophysical mechanism in fast radio bursts and coherent radio transients constrained by LIGO-Virgo-KAGRA, CHIME/FRB", "Alternative non-equilibrium, feedback, or multi-component physical model for Emission Mechanism and Progenitor Diversity of Repeating versus Appare" ]	[ "High-significance multi-wavelength or dynamical measurement of sub-microsecond burst temporal microstructure using LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110.", "Breaking the model degeneracy between intrinsic magnetospheric polarization swings versus propagation effects in a magnetized wi to better than 3-5 sigma." ]	Resolving this question in Transients, Gravitational Waves, and Multi-Messenger Astronomy is essential for calibrating emission radius r_em and testing fundamental astrophysical theory.	Time-domain astrophysics, gravitational-wave data analysis and source astrophysics, coherent radiative processes in magnetars/FRBs, and relativistic blast-wave hydrodynamics.	3	While FRB 200428 from Galactic magnetar SGR 1935+2154 established that magnetars can produce FRBs, the discovery of FRB 20200120E in an old M81 globular cluster requires delayed formation channels, and nanosecond-to-microsecond temporal structures and polarization swings challenge pure far-away shock models while high-...	true	[ { "source_id": "SRC-AST-000006", "support_type": "direct_open_question", "locator": "SKAO Transient Science Working Group: Fast Radio Bursts, Question FRB-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-022062", "citation": "Zhang et al. (2026, arXiv (astro-ph.HE))", "sup...	[ "UAST-000012", "UAST-000066", "UAST-000067", "UAST-000068", "UAST-000069", "UAST-000070", "UAST-000071", "UAST-002179", "UAST-002180", "UAST-002181", "UAST-002182", "UAST-002183", "UAST-002184", "UAST-002185", "UAST-002186", "UAST-023182", "UAST-023393", "UAST-014273" ]	null	[]	[ "transients_gravitational_waves_multimessenger", "fast_radio_bursts_and_coherent_radio_transients", "fast radio bursts (FRBs)", "magnetar coherent emission", "FRB host-galaxy demographics" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000006).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000012	UAST-000012	uast-000012-astrophysical-supermassive-black-hole-binary-versus-cosmological-origin-of-the-nanohe	Astrophysical Supermassive Black Hole Binary versus Cosmological Origin of the Nanohertz Stochastic Gravitational-Wave Background	Is the nanohertz stochastic gravitational-wave background evidenced by pulsar timing arrays (NANOGrav, EPTA/InPTA, PPTA, CPTA) produced entirely by an astrophysical population of inspiraling supermassive black hole binaries, or does it include a cosmological contribution from cosmic strings, phase transitions, or scala...	Does the low-frequency gravitational-wave hum detected by pulsar timing arrays come from pairs of giant black holes orbiting each other across the universe, or from exotic physics in the early universe?	In the 1-100 nHz pulsar timing array band where Hellings-Downs spatial correlations follow h_c(f) = A_yr (f / f_yr)^{alpha} with A_yr ~ 2.4 x 10^{-15}, does the spectral slope alpha, high-frequency discreetness/anisotropy, and resolution of the final-parsec problem confirm supermassive black hole binaries (alpha = -2/3...	transients_gravitational_waves_multimessenger	9	Transients, Gravitational Waves, and Multi-Messenger Astronomy	fast_radio_bursts_and_coherent_radio_transients	[]	population_evolution	[ "transient", "compact_object", "galaxy" ]	population_level	Astrophysical systems in fast radio bursts and coherent radio transients	[ "km_to_1000km", "au", "pc", "gpc" ]	[ { "name": "time_domain_and_multimessenger_universe", "redshift_min": 0, "redshift_max": 6, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 12.8 } ]	[ "gravitational_wave", "radio_cm_m_lowfreq", "optical", "x_ray", "gamma_ray", "near_ir" ]	[ "LIGO-Virgo-KAGRA", "CHIME/FRB", "DSA-110", "ASKAP", "NANOGrav/EPTA/PPTA/IPTA" ]	[ "Hellings-Downs angular cross-correlation curve", "nanohertz GW strain spectrum h_c(f)", "spatial anisotropy C_ell^{GW} and continuous-wave single-source detections" ]	[ "SMBH binary merger rate and environmental hardening timescale", "strain spectral index alpha", "fractional energy density Omega_GW(f)" ]	[ "sky-distribution asymmetry of timed millisecond pulsars" ]	[ "solar-system ephemeris modeling", "interstellar dispersion measure and pulsar intrinsic red spin noise" ]	[ "gas/stellar-driven eccentric SMBH binary turnover at low frequencies versus cosmological first-order phase transition spectrum" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	The 2023 PTA datasets achieved 3-4 sigma evidence for Hellings-Downs correlations with a slightly flatter spectrum than a purely GW-driven circular SMBH binary power law (alpha = -2/3), which is compatible with both environmentally hardened massive SMBH binaries and several early-universe models.	multimessenger	decade_scale	Detection of discrete continuous-wave individual SMBH binaries and frequency-dependent strain anisotropy in IPTA DR3, DSA-2000, and SKAO timing of >=200 millisecond pulsars.	Current observations from LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110 constrain SMBH binary merger rate and environmental hardening timescale, but systematic uncertainties in solar-system ephemeris modeling prevent a definitive resolution.	[ "Baseline astrophysical mechanism in fast radio bursts and coherent radio transients constrained by LIGO-Virgo-KAGRA, CHIME/FRB", "Alternative non-equilibrium, feedback, or multi-component physical model for Astrophysical Supermassive Black Hole Binary versus Cosmological Origi" ]	[ "High-significance multi-wavelength or dynamical measurement of Hellings-Downs angular cross-correlation curve using LIGO-Virgo-KAGRA, CHIME/FRB, DSA-110.", "Breaking the model degeneracy between gas/stellar-driven eccentric SMBH binary turnover at low frequencies versus cosmological f to better than 3-5 sigma." ...	Resolving this question in Transients, Gravitational Waves, and Multi-Messenger Astronomy is essential for calibrating SMBH binary merger rate and environmental hardening timescale and testing fundamental astrophysical theory.	Time-domain astrophysics, gravitational-wave data analysis and source astrophysics, coherent radiative processes in magnetars/FRBs, and relativistic blast-wave hydrodynamics.	4	The 2023 PTA datasets achieved 3-4 sigma evidence for Hellings-Downs correlations with a slightly flatter spectrum than a purely GW-driven circular SMBH binary power law (alpha = -2/3), which is compatible with both environmentally hardened massive SMBH binaries and several early-universe models.	true	[ { "source_id": "SRC-AST-000018", "support_type": "direct_open_question", "locator": "Section 4 & 5: Astrophysical and Cosmological Interpretations of the GWB, Question PTA-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-008216", "citation": "Gardiner et al. (2026, arXiv (astr...	[ "UAST-000011", "UAST-010665", "UAST-008402", "UAST-004614" ]	null	[]	[ "transients_gravitational_waves_multimessenger", "fast_radio_bursts_and_coherent_radio_transients", "nanohertz gravitational-wave background", "supermassive black hole binaries", "pulsar timing arrays" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000018).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000013	UAST-000013	uast-000013-astrophysical-source-classes-and-acceleration-mechanism-of-ultra-high-energy-cosmic-r	Astrophysical Source Classes and Acceleration Mechanism of Ultra-High-Energy Cosmic Rays Above 10^{18.5} eV	Which extragalactic astrophysical sources—relativistic AGN jets, radio-galaxy lobes, starburst wind termination shocks, gamma-ray bursts, or tidal disruption events—accelerate ultra-high-energy cosmic rays above the ankle (E > 10^{18.5} eV) up to 10^{20} eV, and what accounts for the progressive transition toward heavi...	Which cosmic powerhouses accelerate the highest-energy particles in the universe above ten billion billion electronvolts, and why do those particles become heavier nuclei at the highest energies?	For ultra-high-energy cosmic rays between the ankle at 5 x 10^{18} eV and the flux suppression above 4 x 10^{19} eV, what source population and rigidity-dependent acceleration cutoff E_max(Z) = Z E_{max,p} reproduce the Pierre Auger and Telescope Array energy spectrum, <X_max> and sigma(X_max) mass composition, and int...	cosmic_rays_neutrinos_nonthermal	10	Cosmic Rays, Neutrinos, and the Nonthermal Universe	ultra_high_energy_cosmic_rays	[]	mechanism	[ "nonthermal_particle", "compact_object", "agn_quasar", "galaxy" ]	population_level	Astrophysical systems in ultra high energy cosmic rays	[ "au", "pc", "kpc", "mpc" ]	[ { "name": "nonthermal_and_high_energy_universe", "redshift_min": 0, "redshift_max": 4, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 12.2 } ]	[ "cosmic_ray", "neutrino", "gamma_ray", "x_ray", "radio_cm_m_lowfreq" ]	[ "Pierre Auger Observatory", "Telescope Array", "IceCube", "KM3NeT", "LHAASO" ]	[ "extensive air shower depth of maximum X_max and muon number N_mu", "arrival direction dipole and hotspot correlations", "cosmogenic EeV neutrino flux" ]	[ "nuclear charge Z and mass number A distribution", "maximum proton acceleration rigidity R_max", "extragalactic and Galactic magnetic deflection angles" ]	[ "GZK and photodisintegration attenuation horizon limiting sources above 50 EeV to the local supercluster volume" ]	[ "hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) at center-of-mass energies >100 TeV (the muon puzzle)", "uncertain Galactic and extragalactic magnetic field models" ]	[ "rigidity-dependent Peters cycle acceleration cutoff at the source versus propagation photodisintegration in the source environment" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Magnetic deflections of intermediate-mass nuclei (CNO to Si/Fe) smear point-source arrival directions across tens of degrees, and hadronic air-shower model uncertainties complicate per-event rigidity reconstruction.	multimessenger	decade_scale	Event-by-event charge/mass discrimination from AugerPrime radio+scintillator upgrades and GCOS, combined with IceCube-Gen2/RNO-G cosmogenic EeV neutrino detections and updated LHCf/forward-collider hadronic models.	Current observations from Pierre Auger Observatory, Telescope Array, IceCube constrain nuclear charge Z and mass number A distribution, but systematic uncertainties in hadronic interaction model uncertainties (EPOS-LHC, Sibyll, QGSJet) at prevent a definitive resolution.	[ "Baseline astrophysical mechanism in ultra high energy cosmic rays constrained by Pierre Auger Observatory, Telescope Array", "Alternative non-equilibrium, feedback, or multi-component physical model for Astrophysical Source Classes and Acceleration Mechanism of Ultra-High-" ]	[ "High-significance multi-wavelength or dynamical measurement of extensive air shower depth of maximum X_max and muon number N_mu using Pierre Auger Observatory, Telescope Array, IceCube.", "Breaking the model degeneracy between rigidity-dependent Peters cycle acceleration cutoff at the source versus propagation p...	Resolving this question in Cosmic Rays, Neutrinos, and the Nonthermal Universe is essential for calibrating nuclear charge Z and mass number A distribution and testing fundamental astrophysical theory.	High-energy particle astrophysics, diffusive shock acceleration and relativistic magnetic reconnection, cosmic-ray propagation and magnetohydrodynamic turbulence, and multimessenger neutrino/gamma-ray radiative transfer.	4	Magnetic deflections of intermediate-mass nuclei (CNO to Si/Fe) smear point-source arrival directions across tens of degrees, and hadronic air-shower model uncertainties complicate per-event rigidity reconstruction.	true	[ { "source_id": "SRC-AST-000015", "support_type": "direct_open_question", "locator": "Ginzburg Problem 26 & Astro2020 Multi-Messenger Frontier, Problem UHECR-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-024980", "citation": "The Pierre Auger Collaboration (2023, JCAP05(2023...	[ "UAST-000072", "UAST-000073", "UAST-000074", "UAST-000075", "UAST-000076", "UAST-000077", "UAST-002451", "UAST-002452", "UAST-002453", "UAST-002454", "UAST-002455", "UAST-002456", "UAST-002457", "UAST-002458", "UAST-002459", "UAST-025932", "UAST-026189", "UAST-012749" ]	null	[]	[ "cosmic_rays_neutrinos_nonthermal", "ultra_high_energy_cosmic_rays", "ultra-high-energy cosmic rays (UHECRs)", "extragalactic particle accelerators", "UHECR mass composition and anisotropy" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000015).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000014	UAST-000014	uast-000014-physical-origin-of-the-exoplanet-radius-valley-separating-super-earths-and-sub-neptun	Physical Origin of the Exoplanet Radius Valley Separating Super-Earths and Sub-Neptunes	Is the bimodal radius valley at R_p ~ 1.5-2.0 R_Earth separating rocky super-Earths from volatile-rich sub-Neptunes carved primarily by XUV-driven photoevaporation, core-powered atmospheric mass loss, or primordial gas-poor versus water-world formation pathways?	Why are there relatively few exoplanets with sizes between 1.5 and 2.0 times Earth's radius, and is this gap caused by starlight stripping their atmospheres, heat from their own cores, or how they formed?	In the close-in exoplanet population (P < 100 days) around FGKM host stars, how does the dependence of the radius-valley location R_valley(P, M_*, t_age) on orbital period, stellar mass, system age, and planet bulk density rho_p discriminate among XUV photoevaporation, core-powered mass loss, and water-rich migration m...	exoplanets_planetary_system_formation	11	Exoplanets and Planetary-System Formation	protoplanetary_disks_and_planet_formation	[]	model_discrimination	[ "exoplanet", "protoplanetary_disk", "star" ]	population_level	Astrophysical systems in protoplanetary disks and planet formation	[ "km_to_1000km", "1000km_to_rsun", "au" ]	[ { "name": "protoplanetary_disks_to_mature_systems", "redshift_min": 0, "redshift_max": 0.01, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 0.1 } ]	[ "near_ir", "mid_ir", "optical", "mm_submm", "uv" ]	[ "JWST", "ALMA", "TESS", "Kepler", "PLATO" ]	[ "radius-period-stellar-mass valley slope d log R_valley / d log P and d log R_valley / d log M_*", "bulk mass-radius relation M_p(R_p)", "He I 10830 A and Ly-alpha escaping atmosphere transits", "JWST transmission spectra of sub-Neptunes" ]	[ "H/He envelope mass fraction f_env", "water/volatile ice mass fraction", "atmospheric mass-loss timescale tau_loss" ]	[ "transit geometric probability P_tr ~ a^{-1} and radial-velocity follow-up bias toward bright, quiet stars" ]	[ "host-star radius and age uncertainties", "high-altitude photochemical hazes muting JWST transmission features" ]	[ "interior composition degeneracy on the mass-radius diagram between a rocky core with a ~1% H2/He envelope and a 50% H2O steam/supercritical water world" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Photoevaporation and core-powered mass loss predict similar slopes in the radius-period plane around FGK stars, while mass-radius measurements alone cannot break the interior degeneracy between H/He-enveloped rocky cores and volatile-rich water worlds without atmospheric mean-molecular-weight determinations.	observational_and_theoretical	near_term_1_to_5_years	Age-resolved occurrence rates from PLATO and Roman across 10 Myr to 10 Gyr stars combined with JWST and Ariel atmospheric mean-molecular-weight and C/O/H2O abundance measurements for >=100 sub-Neptunes.	Current observations from JWST, ALMA, TESS constrain H/He envelope mass fraction f_env, but systematic uncertainties in host-star radius and age uncertainties prevent a definitive resolution.	[ "Baseline astrophysical mechanism in protoplanetary disks and planet formation constrained by JWST, ALMA", "Alternative non-equilibrium, feedback, or multi-component physical model for Physical Origin of the Exoplanet Radius Valley Separating Super-Earths" ]	[ "High-significance multi-wavelength or dynamical measurement of radius-period-stellar-mass valley slope d log R_valley / d log P and d log R_valley / d lo using JWST, ALMA, TESS.", "Breaking the model degeneracy between interior composition degeneracy on the mass-radius diagram between a rocky core with a ~1% to ...	Resolving this question in Exoplanets and Planetary-System Formation is essential for calibrating H/He envelope mass fraction f_env and testing fundamental astrophysical theory.	Exoplanet detection and characterization, planetary atmospheric radiative-convective transfer and chemistry, interior structure equations of state, and protoplanetary disk gas-dust hydrodynamics.	3	Photoevaporation and core-powered mass loss predict similar slopes in the radius-period plane around FGK stars, while mass-radius measurements alone cannot break the interior degeneracy between H/He-enveloped rocky cores and volatile-rich water worlds without atmospheric mean-molecular-weight determinations.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Worlds and Suns in Context: Pathways to Habitable Worlds, Question WSC-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-026940", "citation": "Burn et al. (2024, arXiv (astro-ph.EP))", "sup...	[ "UAST-000078", "UAST-000079", "UAST-000080", "UAST-000081", "UAST-000082", "UAST-000083", "UAST-002619", "UAST-002620", "UAST-002621", "UAST-002622", "UAST-002623", "UAST-002624", "UAST-002625", "UAST-002626", "UAST-002627", "UAST-027584", "UAST-027939", "UAST-027168" ]	null	[]	[ "exoplanets_planetary_system_formation", "protoplanetary_disks_and_planet_formation", "exoplanet radius valley (Fulton gap)", "super-Earths and sub-Neptunes", "atmospheric escape vs water worlds" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000015	UAST-000015	uast-000015-dynamical-existence-versus-collective-gravitational-instability-origin-of-distant-tra	Dynamical Existence versus Collective Gravitational Instability Origin of Distant Trans-Neptunian Orbital Clustering (Planet Nine Hypothesis)	Does the apparent clustering in longitude of perihelion, orbital pole, and argument of perihelion among extreme trans-Neptunian objects (a > 250 AU, q > 30 AU) arise from gravitational shepherding by an undiscovered ~5-10 M_Earth distant planet, from observational survey selection biases, or from self-gravitating disk ...	Are the aligned orbits of the most distant icy objects in the Solar System caused by an undiscovered ninth planet, or are they an artifact of where telescopes have looked?	For extreme trans-Neptunian objects (eTNOs) with semimajor axes a > 250 AU and perihelia q > 40 AU decoupled from strong Neptunian scattering, is the joint distribution of (varpi, Omega, i) statistically incompatible with uniform random angles after accounting for survey pointing history, depth, and cadence, and does a...	solar_system_worlds_small_bodies	12	Solar-System Worlds and Small Bodies	giant_planets_and_ice_giants	[]	model_discrimination	[ "solar_system_body", "dust_and_ice" ]	population_level	Astrophysical systems in giant planets and ice giants	[ "sub_km", "km_to_1000km", "au" ]	[ { "name": "solar_nebula_to_present_solar_system", "redshift_min": 0, "redshift_max": 0, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 4.567 } ]	[ "optical", "near_ir", "mid_ir", "mm_submm", "radio_cm_m_lowfreq", "uv" ]	[ "Juno", "Europa Clipper", "JUICE", "Dragonfly", "OSIRIS-REx" ]	[ "orbital elements (a, q, e, i, Omega, varpi) of eTNOs", "direct wide-field optical/IR and CMB-survey moving-object detections" ]	[ "intrinsic eTNO orbital angle distribution", "mass M_9 and semimajor axis a_9 of a hypothetical distant planet" ]	[ "severe longitudinal, seasonal, and Galactic-plane pointing biases in heterogeneous TNO discovery surveys" ]	[ "small sample size (N < 30 decoupled eTNOs) and sensitivity to semi-major axis and perihelion cutoff choices" ]	[ "observational pointing bias + Neptunian mean-motion/secular diffusion versus gravitational shepherding by an unseen planet" ]	open	true	partial_observational_constraint	open_consensus	2026-10-16T00:00:00	Analyses of heterogeneous discovery catalogs find clustering significance ~3 sigma, whereas uniformly characterized surveys (OSSOS, DES, Bernardinelli et al.) have yielded mixed consistency with a uniform intrinsic distribution due to limited sample sizes.	observational_and_theoretical	near_term_1_to_5_years	Vera C. Rubin Observatory LSST discovering >10x more decoupled eTNOs with a single, fully characterized selection function and either directly detecting a distant planet down to V ~ 24.5 or proving uniform eTNO orbital longitudes.	Current observations from Juno, Europa Clipper, JUICE constrain intrinsic eTNO orbital angle distribution, but systematic uncertainties in small sample size (N < 30 decoupled eTNOs) and sensitivity to semi-maj prevent a definitive resolution.	[ "Baseline astrophysical mechanism in giant planets and ice giants constrained by Juno, Europa Clipper", "Alternative non-equilibrium, feedback, or multi-component physical model for Dynamical Existence versus Collective Gravitational Instability Origin" ]	[ "High-significance multi-wavelength or dynamical measurement of orbital elements (a, q, e, i, Omega, varpi) of eTNOs using Juno, Europa Clipper, JUICE.", "Breaking the model degeneracy between observational pointing bias + Neptunian mean-motion/secular diffusion versus gravitational to better than 3-5 sigma." ]	Resolving this question in Solar-System Worlds and Small Bodies is essential for calibrating intrinsic eTNO orbital angle distribution and testing fundamental astrophysical theory.	Planetary geophysics and interior structure, cosmochemistry and meteoritics, orbital dynamics and celestial mechanics, and icy moon oceanography.	3	Analyses of heterogeneous discovery catalogs find clustering significance ~3 sigma, whereas uniformly characterized surveys (OSSOS, DES, Bernardinelli et al.) have yielded mixed consistency with a uniform intrinsic distribution due to limited sample sizes.	true	[ { "source_id": "SRC-AST-000004", "support_type": "direct_open_question", "locator": "Question 2: Outer Solar System Architecture and Small Bodies, OWL-Q2.4", "verbatim_quote_used": false }, { "source_id": "SRC-AST-029752", "citation": "Porter et al. (2024, arXiv (astro-ph.EP))", "sup...	[ "UAST-000084", "UAST-000085", "UAST-000086", "UAST-000087", "UAST-000088", "UAST-000089", "UAST-002927", "UAST-002928", "UAST-002929", "UAST-002930", "UAST-002931", "UAST-002932", "UAST-002933", "UAST-002934", "UAST-002935", "UAST-030193", "UAST-030203", "UAST-030859" ]	null	[]	[ "solar_system_worlds_small_bodies", "giant_planets_and_ice_giants", "extreme trans-Neptunian objects (eTNOs)", "distant Solar System architecture", "Planet Nine hypothesis" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000004).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000016	UAST-000016	uast-000016-abiotic-photochemical-false-positives-versus-biological-production-of-oxygen-methane	Abiotic Photochemical False Positives versus Biological Production of Oxygen, Methane, and Organosulfur Gases in Temperate Exoplanet Atmospheres	Under what host-star ultraviolet spectral energy distributions and planetary redox conditions can simultaneous detections of atmospheric O2/O3 with CH4/CO2 or trace organosulfur gases (such as dimethyl sulfide) on temperate terrestrial or Hycean exoplanets be uniquely distinguished from abiotic photochemical and outgas...	When telescopes detect gases like oxygen, methane, or dimethyl sulfide in an exoplanet's atmosphere, what additional clues are needed to prove they come from life rather than non-biological chemistry?	In transmission, emission, and reflected-light spectroscopy of temperate terrestrial and sub-Neptune/Hycean exoplanets around M and FGK dwarfs, what combination of disequilibrium gas abundances (O2, O3, CH4, CO2, CO, N2O, H2O, DMS), isotopic ratios, and surface-atmosphere redox indicators rules out abiotic H2O/CO2 phot...	astrobiology_habitability_biosignatures_technosignatures	13	Astrobiology, Habitability, Biosignatures, and Technosignatures	technosignatures_and_seti	[]	detection_or_characterization	[ "exoplanet", "solar_system_body", "interstellar_medium", "star" ]	population_level	Astrophysical systems in technosignatures and seti	[ "km_to_1000km", "au", "pc" ]	[ { "name": "prebiotic_to_planetary_biospheres", "redshift_min": 0, "redshift_max": 0.05, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 4.5 } ]	[ "near_ir", "mid_ir", "uv", "optical", "radio_cm_m_lowfreq" ]	[ "JWST", "Habitable Worlds Observatory", "ELT", "LIFE", "Europa Clipper" ]	[ "JWST, ELT, and HWO transmission/reflected-light molecular absorption bands", "O2-O2 1.27 micron collision-induced absorption", "CO and H2O abundance ratios", "host-star FUV/NUV Ly-alpha flux" ]	[ "surface biotic vs abiotic gas fluxes", "planetary mantle/crustal redox state", "ocean vs magma-ocean or supercritical-envelope lower boundary" ]	[ "transit spectroscopy feasibility strongly favoring M-dwarf hosts with extreme pre-main-sequence XUV irradiation histories" ]	[ "incomplete high-temperature/high-pressure cross-section line lists for trace organosulfur and hydrocarbon gases", "stellar photospheric heterogeneity (Transit Light Source Effect) and correlated instrumental noise" ]	[ "overlapping 3.3-3.5 micron absorption bands of CH4, DMS, CS2, and C2H6 in low-SNR JWST transmission spectra; abiotic serpentinization + CO2 reduction versus methanogenesis" ]	open	true	partial_observational_constraint	open_consensus	2026-10-16T00:00:00	Single-gas detections and low-SNR multi-gas claims (such as tentative DMS hints in K2-18 b alongside CH4 and CO2) are degenerate with overlapping hydrocarbon/sulfur cross sections and abiotic interior-atmosphere chemistry in H2-rich sub-Neptunes.	observational_and_theoretical	decade_scale	High-SNR multi-band JWST + ELT high-resolution cross-correlation spectroscopy and Habitable Worlds Observatory UV-optical-NIR reflected-light spectra jointly measuring O2, O3, CH4, CO2, H2O, and excluding abiotic false-positive markers (CO, O4).	Current observations from JWST, Habitable Worlds Observatory, ELT constrain surface biotic vs abiotic gas fluxes, but systematic uncertainties in incomplete high-temperature/high-pressure cross-section line lists for prevent a definitive resolution.	[ "Baseline astrophysical mechanism in technosignatures and seti constrained by JWST, Habitable Worlds Observatory", "Alternative non-equilibrium, feedback, or multi-component physical model for Abiotic Photochemical False Positives versus Biological Production of " ]	[ "High-significance multi-wavelength or dynamical measurement of JWST, ELT, and HWO transmission/reflected-light molecular absorption bands using JWST, Habitable Worlds Observatory, ELT.", "Breaking the model degeneracy between overlapping 3.3-3.5 micron absorption bands of CH4, DMS, CS2, and C2H6 in low-SNR JWST ...	Resolving this question in Astrobiology, Habitability, Biosignatures, and Technosignatures is essential for calibrating surface biotic vs abiotic gas fluxes and testing fundamental astrophysical theory.	Astrobiology, planetary climate and atmospheric photochemistry, prebiotic organic chemistry and volatile delivery, biosignature false-positive assessment, and technosignature search methodology.	4	Single-gas detections and low-SNR multi-gas claims (such as tentative DMS hints in K2-18 b alongside CH4 and CO2) are degenerate with overlapping hydrocarbon/sulfur cross sections and abiotic interior-atmosphere chemistry in H2-rich sub-Neptunes.	true	[ { "source_id": "SRC-AST-000017", "support_type": "direct_open_question", "locator": "NFoLD Biosignatures Standards of Evidence Framework (Levels 1-5), Standard B-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-031754", "citation": "Mitchell et al. (2025, arXiv (astro-ph.EP))"...	[ "UAST-000090", "UAST-000091", "UAST-000092", "UAST-000093", "UAST-000094", "UAST-000095", "UAST-003130", "UAST-003131", "UAST-003132", "UAST-003133", "UAST-003134", "UAST-003135", "UAST-003136", "UAST-003137", "UAST-003138", "UAST-032028", "UAST-027163", "UAST-031884" ]	null	[]	[ "astrobiology_habitability_biosignatures_technosignatures", "technosignatures_and_seti", "exoplanet atmospheric biosignatures", "abiotic oxygen and methane false positives", "Hycean and terrestrial worlds (e.g., K2-18 b, TRAPPIST-1 e)" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000017).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000017	UAST-000017	uast-000017-quantitative-partition-between-alfv-nic-wave-turbulence-and-impulsive-nanoflare-recon	Quantitative Partition Between Alfvénic Wave Turbulence and Impulsive Nanoflare Reconnection in Heating the Solar Corona and Accelerating the Solar Wind	What are the relative quantitative energy fluxes contributed by low-frequency Alfvénic wave turbulence cascades versus impulsive magnetic reconnection ('nanoflares' and interchange reconnection jets/switchbacks) to heating the quiet and active solar corona above 10^6 K and accelerating the fast and slow solar wind?	How much of the Sun's million-degree corona heating and solar wind acceleration comes from magnetic waves versus tiny magnetic reconnection explosions?	From the solar chromosphere/transition region (1.01 R_sun) through the Alfvén critical surface (10-20 R_sun) probed by Parker Solar Probe and Solar Orbiter, what fraction of the coronal radiative/conductive loss budget (10^5-10^7 erg cm^{-2} s^{-1}) is supplied by ion-cyclotron/stochastic Alfvén-wave dissipation versus...	solar_stellar_activity_heliospheric	14	Solar, Stellar-Activity, and Heliospheric Astronomy	solar_interior_dynamo_and_cycle	[]	model_discrimination	[ "star", "heliosphere", "solar_system_body" ]	population_level	Astrophysical systems in solar interior dynamo and cycle	[ "sub_km", "km_to_1000km", "1000km_to_rsun", "au" ]	[ { "name": "modern_solar_and_stellar_cycles", "redshift_min": 0, "redshift_max": 0.001, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 0.01 } ]	[ "uv", "x_ray", "optical", "radio_cm_m_lowfreq", "cosmic_ray" ]	[ "Parker Solar Probe", "Solar Orbiter", "DKIST", "SDO", "IRIS" ]	[ "EUV/X-ray Differential Emission Measure DEM(T) and nonthermal line broadening", "Parker Solar Probe in-situ Poynting flux, proton/alpha temperature anisotropy, and switchback statistics", "DKIST high-resolution chromospheric magnetograms" ]	[ "volumetric coronal heating rate Q(r)", "nanoflare energy distribution slope alpha_E", "turbulent cascade dissipation rate epsilon_turb" ]	[ "line-of-sight optically thin integration across multistranded coronal loops obscuring individual sub-resolution reconnection events" ]	[ "non-equilibrium ionization lags during impulsive heating", "single-spacecraft spatiotemporal ambiguity when mapping in-situ solar wind streams back to coronal footpoints" ]	[ "secondary Alfvén waves generated by interchange reconnection jets versus photospherically driven wave turbulence" ]	open	true	conflicting_measurements	active_debate	2026-10-16T00:00:00	Parker Solar Probe and Solar Orbiter have revealed ubiquitous interchange-reconnection jets ('picoflare jets') and magnetic switchbacks near the Alfvén surface while EUV spectroscopy shows high-temperature emission components in active regions, proving both mechanisms operate without yet closing the global energy budge...	observational_and_theoretical	decade_scale	Coordinated multi-point observations linking DKIST/MUSE sub-arcsecond coronal spectroscopy with Parker Solar Probe and Solar Orbiter perihelion in-situ plasma/field measurements across the Alfvén critical zone.	Current observations from Parker Solar Probe, Solar Orbiter, DKIST constrain volumetric coronal heating rate Q(r), but systematic uncertainties in non-equilibrium ionization lags during impulsive heating prevent a definitive resolution.	[ "Baseline astrophysical mechanism in solar interior dynamo and cycle constrained by Parker Solar Probe, Solar Orbiter", "Alternative non-equilibrium, feedback, or multi-component physical model for Quantitative Partition Between Alfvénic Wave Turbulence and Impulsive " ]	[ "High-significance multi-wavelength or dynamical measurement of EUV/X-ray Differential Emission Measure DEM(T) and nonthermal line broadening using Parker Solar Probe, Solar Orbiter, DKIST.", "Breaking the model degeneracy between secondary Alfvén waves generated by interchange reconnection jets versus photospher...	Resolving this question in Solar, Stellar-Activity, and Heliospheric Astronomy is essential for calibrating volumetric coronal heating rate Q(r) and testing fundamental astrophysical theory.	Solar and stellar magnetohydrodynamics, helioseismology and dynamo theory, magnetic reconnection and kinetic plasma turbulence, and heliospheric space physics.	4	Parker Solar Probe and Solar Orbiter have revealed ubiquitous interchange-reconnection jets ('picoflare jets') and magnetic switchbacks near the Alfvén surface while EUV spectroscopy shows high-temperature emission components in active regions, proving both mechanisms operate without yet closing the global energy budge...	true	[ { "source_id": "SRC-AST-000005", "support_type": "direct_open_question", "locator": "Heliophysics Decadal Survey Guiding Question 1: Coronal Heating and Solar Wind Acceleration, Question H-1", "verbatim_quote_used": false }, { "source_id": "SRC-AST-033283", "citation": "B et al. (2026, A...	[ "UAST-000096", "UAST-000097", "UAST-000098", "UAST-000099", "UAST-000100", "UAST-000101", "UAST-003298", "UAST-003299", "UAST-003300", "UAST-003301", "UAST-003302", "UAST-003303", "UAST-003304", "UAST-003305", "UAST-003306", "UAST-033354", "UAST-034698", "UAST-033741" ]	null	[]	[ "solar_stellar_activity_heliospheric", "solar_interior_dynamo_and_cycle", "solar coronal heating problem", "solar wind acceleration", "magnetic switchbacks and nanoflares" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000005).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000018	UAST-000018	uast-000018-primordial-local-non-gaussianity-amplitude-f-nl-local-from-multi-tracer-galaxy-survey	Primordial Local Non-Gaussianity Amplitude f_NL^local from Multi-Tracer Galaxy Surveys	Does the primordial curvature perturbation exhibit local-type non-Gaussianity with \|f_NL^local\| >= 1 detectable through scale-dependent halo bias in wide-field spectroscopic and photometric galaxy surveys, or were primordial fluctuations generated by single-field slow-roll inflation with f_NL^local ~ O(n_s - 1) << 1?	Does the primordial curvature perturbation exhibit local-type non-Gaussianity with \|f_NL^local\| >= 1 detectable through scale-dependent halo bias in wide-field spectroscopic and photometric galaxy surveys, or were primordial fluctuations generated by single-field slow-roll inflation with f_NL^local ~ O(n_s - 1) << 1?	Does the primordial curvature perturbation exhibit local-type non-Gaussianity with \|f_NL^local\| >= 1 detectable through scale-dependent halo bias in wide-field spectroscopic and photometric galaxy surveys, or were primordial fluctuations generated by single-field slow-roll inflation with f_NL^local ~ O(n_s - 1) << 1? H...	cosmology_early_universe	1	Cosmology and the Early Universe	inflation_and_primordial_initial_conditions	[]	value_or_bound	[ "large_scale_structure", "cosmic_background" ]	population_level	Astrophysical systems in inflation and primordial initial conditions	[ "cosmological_horizon", "gpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "optical", "near_ir", "cmb_mm_submm" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB", "Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d", "Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)" ]	[ "Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)", "Comoving sound horizon r_d and Hubble expansion rate H(z)", "Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc" ]	[ "Cosmic variance at low multipoles l < 30", "Lyman-alpha line-of-sight damping-wing absorption bias at z > 7" ]	[ "Galactic polarized thermal dust and synchrotron foreground subtraction residuals", "Cepheid/TRGB photometric crowding and metallicity zero-point calibration" ]	[ "Sound horizon r_d vs late-time dark energy equation of state w(z)", "Optical depth tau_reio vs primordial scalar amplitude A_s" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16.	survey_statistical	decade_scale	Discriminating Baseline astrophysical mechanism in inflation and primordial initial condit from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB.	Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution.	[ "Baseline astrophysical mechanism in inflation and primordial initial conditions constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Primordial Local Non-Gaussianity Amplitude f_NL^local from Multi-Trace" ]	[ "High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.", "Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Appendix B, Priority Area: New Messengers and New Physics, p. B-14", "verbatim_quote_used": false }, { "source_id": "SRC-AST-001314", "citation": "Stahl et al. (2024, arXiv (astro-ph.CO))", "support_...	[ "UAST-000001", "UAST-004509", "UAST-008368", "UAST-003993" ]	null	[]	[ "cosmology_early_universe", "inflation_and_primordial_initial_conditions", "non_gaussianity", "f_NL", "scale_dependent_bias", "inflation" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000019	UAST-000019	uast-000019-primordial-cmb-mu-and-y-type-blackbody-spectral-distortions-from-silk-damping	Primordial CMB mu- and y-Type Blackbody Spectral Distortions from Silk Damping	What is the exact amplitude of the primordial chemical-potential (mu-type) and Compton (y-type) spectral distortions of the cosmic microwave background generated by acoustic Silk damping at small scales (50 <= k <= 10^4 Mpc^-1), and do pre-recombination energy injection processes exceed the standard adiabatic LambdaCDM...	What is the exact amplitude of the primordial chemical-potential (mu-type) and Compton (y-type) spectral distortions of the cosmic microwave background generated by acoustic Silk damping at small scales (50 <= k <= 10^4 Mpc^-1), and do pre-recombination energy injection processes exceed the standard adiabatic LambdaCDM...	What is the exact amplitude of the primordial chemical-potential (mu-type) and Compton (y-type) spectral distortions of the cosmic microwave background generated by acoustic Silk damping at small scales (50 <= k <= 10^4 Mpc^-1), and do pre-recombination energy injection processes exceed the standard adiabatic LambdaCDM...	cosmology_early_universe	1	Cosmology and the Early Universe	cmb_anisotropies_polarization_and_spectral_distortions	[]	value_or_bound	[ "cosmic_background", "early_universe" ]	population_level	Astrophysical systems in cmb anisotropies polarization and spectral distortions	[ "cosmological_horizon", "mpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "cmb_mm_submm", "far_ir" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB", "Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d", "Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)" ]	[ "Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)", "Comoving sound horizon r_d and Hubble expansion rate H(z)", "Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc" ]	[ "Cosmic variance at low multipoles l < 30", "Lyman-alpha line-of-sight damping-wing absorption bias at z > 7" ]	[ "Galactic polarized thermal dust and synchrotron foreground subtraction residuals", "Cepheid/TRGB photometric crowding and metallicity zero-point calibration" ]	[ "Sound horizon r_d vs late-time dark energy equation of state w(z)", "Optical depth tau_reio vs primordial scalar amplitude A_s" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16.	survey_statistical	decade_scale	Discriminating Baseline astrophysical mechanism in cmb anisotropies polarization and spect from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB.	Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution.	[ "Baseline astrophysical mechanism in cmb anisotropies polarization and spectral distortions constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Primordial CMB mu- and y-Type Blackbody Spectral Distortions from Silk" ]	[ "High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.", "Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000002", "support_type": "direct_open_question", "locator": "Section 3.1: Voyage 2050 White Paper on CMB Spectral Distortions, p. 18", "verbatim_quote_used": false }, { "source_id": "SRC-AST-002471", "citation": "Farhang et al. (2012, Astronomy Journal)", "sup...	[ "UAST-000001", "UAST-005666", "UAST-005075", "UAST-000176" ]	null	[]	[ "cosmology_early_universe", "cmb_anisotropies_polarization_and_spectral_distortions", "spectral_distortions", "mu_distortion", "Silk_damping", "CMB" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000002).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000020	UAST-000020	uast-000020-cosmological-neutrino-mass-sum-from-combined-cmb-lensing-and-bao-clustering	Cosmological Neutrino Mass Sum from Combined CMB Lensing and BAO Clustering	What is the sum of the three active neutrino mass eigenstates Sigma m_nu inferred from late-time suppression of matter clustering and gravitational lensing of the CMB, and why do current BAO + CMB lensing combinations favor upper bounds near or slightly below the minimal normal-hierarchy threshold of 0.059 eV?	What is the sum of the three active neutrino mass eigenstates Sigma m_nu inferred from late-time suppression of matter clustering and gravitational lensing of the CMB, and why do current BAO + CMB lensing combinations favor upper bounds near or slightly below the minimal normal-hierarchy threshold of 0.059 eV?	What is the sum of the three active neutrino mass eigenstates Sigma m_nu inferred from late-time suppression of matter clustering and gravitational lensing of the CMB, and why do current BAO + CMB lensing combinations favor upper bounds near or slightly below the minimal normal-hierarchy threshold of 0.059 eV? Highligh...	cosmology_early_universe	1	Cosmology and the Early Universe	baryogenesis_nucleosynthesis_and_recombination	[]	tension_resolution	[ "cosmic_background", "large_scale_structure" ]	population_level	Astrophysical systems in baryogenesis nucleosynthesis and recombination	[ "cosmological_horizon", "gpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "cmb_mm_submm", "optical", "near_ir" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB", "Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d", "Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)" ]	[ "Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)", "Comoving sound horizon r_d and Hubble expansion rate H(z)", "Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc" ]	[ "Cosmic variance at low multipoles l < 30", "Lyman-alpha line-of-sight damping-wing absorption bias at z > 7" ]	[ "Galactic polarized thermal dust and synchrotron foreground subtraction residuals", "Cepheid/TRGB photometric crowding and metallicity zero-point calibration" ]	[ "Sound horizon r_d vs late-time dark energy equation of state w(z)", "Optical depth tau_reio vs primordial scalar amplitude A_s" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16.	survey_statistical	decade_scale	Discriminating Baseline astrophysical mechanism in baryogenesis nucleosynthesis and recomb from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB.	Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution.	[ "Baseline astrophysical mechanism in baryogenesis nucleosynthesis and recombination constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Cosmological Neutrino Mass Sum from Combined CMB Lensing and BAO Clust" ]	[ "High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.", "Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000003", "support_type": "direct_open_question", "locator": "Section 2.4: Cosmology and Fundamental Physics, p. 31", "verbatim_quote_used": false }, { "source_id": "SRC-AST-000561", "citation": "Ivanov et al. (2026, arXiv (astro-ph.CO))", "support_type": "expl...	[ "UAST-000001", "UAST-003756", "UAST-003844", "UAST-005663" ]	null	[]	[ "cosmology_early_universe", "baryogenesis_nucleosynthesis_and_recombination", "neutrino_mass", "CMB_lensing", "BAO", "matter_power_spectrum" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000021	UAST-000021	uast-000021-escape-fraction-of-lyman-continuum-photons-from-faint-galaxies-during-reionization	Escape Fraction of Lyman-Continuum Photons from Faint Galaxies During Reionization	What physical mechanisms regulate the ionizing Lyman-continuum photon escape fraction f_esc in low-mass star-forming galaxies at 6 <= z <= 12, and can faint dwarf galaxies alone sustain the ionizing photon budget required to complete hydrogen reionization by z ~ 5.5 without substantial contribution from active galactic...	What physical mechanisms regulate the ionizing Lyman-continuum photon escape fraction f_esc in low-mass star-forming galaxies at 6 <= z <= 12, and can faint dwarf galaxies alone sustain the ionizing photon budget required to complete hydrogen reionization by z ~ 5.5 without substantial contribution from active galactic...	What physical mechanisms regulate the ionizing Lyman-continuum photon escape fraction f_esc in low-mass star-forming galaxies at 6 <= z <= 12, and can faint dwarf galaxies alone sustain the ionizing photon budget required to complete hydrogen reionization by z ~ 5.5 without substantial contribution from active galactic...	cosmology_early_universe	1	Cosmology and the Early Universe	reionization_and_cosmic_dawn	[]	mechanism	[ "galaxy", "intergalactic_medium", "early_universe" ]	population_level	Astrophysical systems in reionization and cosmic dawn	[ "kpc", "mpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "uv", "near_ir", "radio_cm_m_lowfreq" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB", "Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d", "Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)" ]	[ "Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)", "Comoving sound horizon r_d and Hubble expansion rate H(z)", "Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc" ]	[ "Cosmic variance at low multipoles l < 30", "Lyman-alpha line-of-sight damping-wing absorption bias at z > 7" ]	[ "Galactic polarized thermal dust and synchrotron foreground subtraction residuals", "Cepheid/TRGB photometric crowding and metallicity zero-point calibration" ]	[ "Sound horizon r_d vs late-time dark energy equation of state w(z)", "Optical depth tau_reio vs primordial scalar amplitude A_s" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16.	observational_and_theoretical	decade_scale	Discriminating Baseline astrophysical mechanism in reionization and cosmic dawn constraine from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB.	Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution.	[ "Baseline astrophysical mechanism in reionization and cosmic dawn constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Escape Fraction of Lyman-Continuum Photons from Faint Galaxies During " ]	[ "High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.", "Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Appendix C: Cosmic Ecosystems, p. C-8", "verbatim_quote_used": false }, { "source_id": "SRC-AST-002040", "citation": "Trebitsch et al. (2018, Monthly Notices of the Royal Astronomical Societ)", "supp...	[ "UAST-000001", "UAST-005235", "UAST-010399", "UAST-015481" ]	null	[]	[ "cosmology_early_universe", "reionization_and_cosmic_dawn", "reionization", "Lyman_continuum", "escape_fraction", "JWST" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000022	UAST-000022	uast-000022-baryon-acoustic-oscillation-anisotropic-distance-ratios-at-z-0-5-2-5-vs-planck-lambda	Baryon Acoustic Oscillation Anisotropic Distance Ratios at z = 0.5-2.5 vs Planck LambdaCDM	Do transverse and line-of-sight baryon acoustic oscillation distance scales D_M(z)/r_d and D_H(z)/r_d across 0.3 <= z <= 2.5 systematically deviate from a flat cosmological constant expansion history when calibrated independently of the Planck sound horizon r_d?	Do transverse and line-of-sight baryon acoustic oscillation distance scales D_M(z)/r_d and D_H(z)/r_d across 0.3 <= z <= 2.5 systematically deviate from a flat cosmological constant expansion history when calibrated independently of the Planck sound horizon r_d?	Do transverse and line-of-sight baryon acoustic oscillation distance scales D_M(z)/r_d and D_H(z)/r_d across 0.3 <= z <= 2.5 systematically deviate from a flat cosmological constant expansion history when calibrated independently of the Planck sound horizon r_d? Highlighted as a key community research question in DESI ...	cosmology_early_universe	1	Cosmology and the Early Universe	cosmological_tensions_and_parameter_inference	[]	tension_resolution	[ "large_scale_structure", "cosmic_background" ]	population_level	Astrophysical systems in cosmological tensions and parameter inference	[ "gpc", "cosmological_horizon" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "optical", "near_ir" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB", "Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d", "Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)" ]	[ "Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)", "Comoving sound horizon r_d and Hubble expansion rate H(z)", "Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc" ]	[ "Cosmic variance at low multipoles l < 30", "Lyman-alpha line-of-sight damping-wing absorption bias at z > 7" ]	[ "Galactic polarized thermal dust and synchrotron foreground subtraction residuals", "Cepheid/TRGB photometric crowding and metallicity zero-point calibration" ]	[ "Sound horizon r_d vs late-time dark energy equation of state w(z)", "Optical depth tau_reio vs primordial scalar amplitude A_s" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16.	survey_statistical	decade_scale	Discriminating Baseline astrophysical mechanism in cosmological tensions and parameter inf from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB.	Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution.	[ "Baseline astrophysical mechanism in cosmological tensions and parameter inference constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Baryon Acoustic Oscillation Anisotropic Distance Ratios at z = 0.5-2.5" ]	[ "High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.", "Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000019", "support_type": "direct_open_question", "locator": "Section 6: Cosmological Constraints from DESI BAO, p. 22", "verbatim_quote_used": false }, { "source_id": "SRC-AST-001671", "citation": "Philcox et al. (2022, arXiv (astro-ph.CO))", "support_type": "...	[ "UAST-000001", "UAST-004866", "UAST-004510", "UAST-004375" ]	null	[]	[ "cosmology_early_universe", "cosmological_tensions_and_parameter_inference", "BAO", "sound_horizon", "DESI", "expansion_history" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000019).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000023	UAST-000023	uast-000023-morphology-and-percolation-topology-of-ionized-bubbles-in-the-epoch-of-reionization	Morphology and Percolation Topology of Ionized Bubbles in the Epoch of Reionization	Is the percolation topology of ionized H II regions during the midpoint of cosmic reionization (z ~ 7-9) dominated by rare, large (> 20 cMpc) bubbles around overdense galaxy protoclusters or by a more uniform distribution of small ionized regions driven by low-mass halos, as measurable via the 21 cm power spectrum and ...	Is the percolation topology of ionized H II regions during the midpoint of cosmic reionization (z ~ 7-9) dominated by rare, large (> 20 cMpc) bubbles around overdense galaxy protoclusters or by a more uniform distribution of small ionized regions driven by low-mass halos, as measurable via the 21 cm power spectrum and ...	Is the percolation topology of ionized H II regions during the midpoint of cosmic reionization (z ~ 7-9) dominated by rare, large (> 20 cMpc) bubbles around overdense galaxy protoclusters or by a more uniform distribution of small ionized regions driven by low-mass halos, as measurable via the 21 cm power spectrum and ...	cosmology_early_universe	1	Cosmology and the Early Universe	reionization_and_cosmic_dawn	[]	population_evolution	[ "intergalactic_medium", "early_universe", "galaxy" ]	population_level	Astrophysical systems in reionization and cosmic dawn	[ "mpc", "10_to_100_mpc" ]	[ { "name": "inflation_and_recombination", "redshift_min": 1100, "redshift_max": null, "lookback_time_gyr_min": 13.78, "lookback_time_gyr_max": 13.8 } ]	[ "radio_cm_m_lowfreq", "near_ir", "optical" ]	[ "Planck", "JWST", "DESI", "Simons Observatory", "CMB-S4" ]	[ "CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB", "Baryon acoustic oscillation distance ratios D_M(z)/r_d and D_H(z)/r_d", "Redshifted 21 cm brightness temperature fluctuations delta T_b(k, z)" ]	[ "Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL)", "Comoving sound horizon r_d and Hubble expansion rate H(z)", "Neutral hydrogen fraction x_HI(z) and ionizing photon escape fraction f_esc" ]	[ "Cosmic variance at low multipoles l < 30", "Lyman-alpha line-of-sight damping-wing absorption bias at z > 7" ]	[ "Galactic polarized thermal dust and synchrotron foreground subtraction residuals", "Cepheid/TRGB photometric crowding and metallicity zero-point calibration" ]	[ "Sound horizon r_d vs late-time dark energy equation of state w(z)", "Optical depth tau_reio vs primordial scalar amplitude A_s" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Cosmology and the Early Universe community syntheses as of 2026-10-16.	observational_and_theoretical	decade_scale	Discriminating Baseline astrophysical mechanism in reionization and cosmic dawn constraine from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB.	Current observations from Planck, JWST, DESI constrain Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL), but systematic uncertainties in Galactic polarized thermal dust and synchrotron foreground subtraction prevent a definitive resolution.	[ "Baseline astrophysical mechanism in reionization and cosmic dawn constrained by Planck, JWST", "Alternative non-equilibrium, feedback, or multi-component physical model for Morphology and Percolation Topology of Ionized Bubbles in the Epoch of" ]	[ "High-significance multi-wavelength or dynamical measurement of CMB temperature and E/B-mode polarization power spectra C_l^TT, C_l^EE, C_l^BB using Planck, JWST, DESI.", "Breaking the model degeneracy between Sound horizon r_d vs late-time dark energy equation of state w(z) to better than 3-5 sigma." ]	Resolving this question in Cosmology and the Early Universe is essential for calibrating Primordial scalar/tensor power spectrum parameters (A_s, n_s, r, f_NL) and testing fundamental astrophysical theory.	Relativistic cosmological perturbation theory, Boltzmann hierarchy radiative transfer, CMB polarization and spectral distortions, and Bayesian cosmological parameter inference.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000004", "support_type": "direct_open_question", "locator": "Section 4.1: Epoch of Reionization and Cosmic Dawn, p. 42", "verbatim_quote_used": false }, { "source_id": "SRC-AST-005995", "citation": "Hutter et al. (2023, arXiv (astro-ph.CO))", "support_type": "...	[ "UAST-000001", "UAST-008751", "UAST-006628", "UAST-008147" ]	null	[]	[ "cosmology_early_universe", "reionization_and_cosmic_dawn", "21cm_tomography", "ionized_bubbles", "SKA", "Lyman_alpha_emitters" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000004).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000024	UAST-000024	uast-000024-subhalo-mass-function-cutoff-below-10-8-solar-masses-from-strong-gravitational-lens-f	Subhalo Mass Function Cutoff Below 10^8 Solar Masses from Strong Gravitational Lens Flux-Ratio and Imaging Perturbations	Does the dark matter halo mass function continue unbroken down to sub-galactic scales (10^6-10^8 M_sun) as predicted by cold dark matter, or does free-streaming from warm dark matter or self-interaction suppress low-mass subhalos detected via quadruply lensed quasar flux ratios and extended gravitational lens arcs?	Does the dark matter halo mass function continue unbroken down to sub-galactic scales (10^6-10^8 M_sun) as predicted by cold dark matter, or does free-streaming from warm dark matter or self-interaction suppress low-mass subhalos detected via quadruply lensed quasar flux ratios and extended gravitational lens arcs?	Does the dark matter halo mass function continue unbroken down to sub-galactic scales (10^6-10^8 M_sun) as predicted by cold dark matter, or does free-streaming from warm dark matter or self-interaction suppress low-mass subhalos detected via quadruply lensed quasar flux ratios and extended gravitational lens arcs? Hig...	dark_matter_dark_energy_fundamental_cosmology	2	Dark Matter, Dark Energy, and Fundamental Cosmology	dark_matter_astrophysical_signatures	[]	value_or_bound	[ "dark_sector", "galaxy" ]	population_level	Astrophysical systems in dark matter astrophysical signatures	[ "kpc", "pc" ]	[ { "name": "late_time_acceleration_and_halo_assembly", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "near_ir", "radio_cm_m_lowfreq", "mm_submm" ]	[ "Vera C. Rubin Observatory LSST", "Euclid", "DESI", "Nancy Grace Roman Space Telescope", "HST" ]	[ "Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta)", "Strong gravitational lens image positions, time delays, and flux-ratio anomalies", "Dwarf galaxy stellar line-of-sight velocity dispersions and H I rotation curves" ]	[ "Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/m", "Dark energy equation-of-state parameters (w_0, w_a) and linear growth rate f*sigma_8(z)", "Gravitational slip parameter eta = Phi/Psi and primordial black hole mass fraction f_PBH" ]	[ "Surface-brightness selection bias against ultra-diffuse and low-luminosity halos", "Magnification bias and spectroscopic redshift completeness in lensing samples" ]	[ "Photometric redshift outlier tails and shear multiplicative calibration bias m", "Baryonic feedback and intrinsic galaxy alignment contamination in weak lensing" ]	[ "Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy dark matter", "Modified gravity scale-dependent growth vs massive neutrino free-streaming" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Dark Matter, Dark Energy, and Fundamental Cosmology community syntheses as of 2026-10-16.	observational_and_theoretical	decade_scale	Discriminating Baseline astrophysical mechanism in dark matter astrophysical signatures co from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(thet.	Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/, but systematic uncertainties in Photometric redshift outlier tails and shear multiplicative calibratio prevent a definitive resolution.	[ "Baseline astrophysical mechanism in dark matter astrophysical signatures constrained by Vera C. Rubin Observatory LSST, Euclid", "Alternative non-equilibrium, feedback, or multi-component physical model for Subhalo Mass Function Cutoff Below 10^8 Solar Masses from Strong Gravi" ]	[ "High-significance multi-wavelength or dynamical measurement of Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta) using Vera C. Rubin Observatory LSST, Euclid, DESI.", "Breaking the model degeneracy between Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy...	Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating Subhalo mass function dN/dM_sub and dark matter self-interaction cross section s and testing fundamental astrophysical theory.	Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000001", "support_type": "direct_open_question", "locator": "Appendix B: New Messengers and New Physics, p. B-19", "verbatim_quote_used": false }, { "source_id": "SRC-AST-003320", "citation": "Gilman et al. (2026, arXiv (astro-ph.CO))", "support_type": "explic...	[ "UAST-000003", "UAST-006314", "UAST-006255", "UAST-024743" ]	null	[]	[ "dark_matter_dark_energy_fundamental_cosmology", "dark_matter_astrophysical_signatures", "strong_lensing", "subhalo_mass_function", "warm_dark_matter", "flux_ratios" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000001).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000025	UAST-000025	uast-000025-velocity-dependent-self-interacting-dark-matter-cross-section-sigma-m-across-dwarf-ga	Velocity-Dependent Self-Interacting Dark Matter Cross Section Sigma/m Across Dwarf Galaxies to Galaxy Clusters	Can a velocity-dependent self-interacting dark matter cross section sigma/m(v) simultaneously explain the diversity of inner rotation curve slopes in dwarf irregular and low-surface-brightness galaxies (sigma/m ~ 1-5 cm^2 g^-1 at v ~ 30-100 km s^-1) while satisfying the upper bound sigma/m < 0.1-0.3 cm^2 g^-1 in mergin...	Can a velocity-dependent self-interacting dark matter cross section sigma/m(v) simultaneously explain the diversity of inner rotation curve slopes in dwarf irregular and low-surface-brightness galaxies (sigma/m ~ 1-5 cm^2 g^-1 at v ~ 30-100 km s^-1) while satisfying the upper bound sigma/m < 0.1-0.3 cm^2 g^-1 in mergin...	Can a velocity-dependent self-interacting dark matter cross section sigma/m(v) simultaneously explain the diversity of inner rotation curve slopes in dwarf irregular and low-surface-brightness galaxies (sigma/m ~ 1-5 cm^2 g^-1 at v ~ 30-100 km s^-1) while satisfying the upper bound sigma/m < 0.1-0.3 cm^2 g^-1 in mergin...	dark_matter_dark_energy_fundamental_cosmology	2	Dark Matter, Dark Energy, and Fundamental Cosmology	dark_matter_astrophysical_signatures	[]	model_discrimination	[ "dark_sector", "galaxy", "galaxy_cluster" ]	population_level	Astrophysical systems in dark matter astrophysical signatures	[ "kpc", "mpc" ]	[ { "name": "late_time_acceleration_and_halo_assembly", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "x_ray", "radio_cm_m_lowfreq" ]	[ "Vera C. Rubin Observatory LSST", "Euclid", "DESI", "Nancy Grace Roman Space Telescope", "HST" ]	[ "Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta)", "Strong gravitational lens image positions, time delays, and flux-ratio anomalies", "Dwarf galaxy stellar line-of-sight velocity dispersions and H I rotation curves" ]	[ "Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/m", "Dark energy equation-of-state parameters (w_0, w_a) and linear growth rate f*sigma_8(z)", "Gravitational slip parameter eta = Phi/Psi and primordial black hole mass fraction f_PBH" ]	[ "Surface-brightness selection bias against ultra-diffuse and low-luminosity halos", "Magnification bias and spectroscopic redshift completeness in lensing samples" ]	[ "Photometric redshift outlier tails and shear multiplicative calibration bias m", "Baryonic feedback and intrinsic galaxy alignment contamination in weak lensing" ]	[ "Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy dark matter", "Modified gravity scale-dependent growth vs massive neutrino free-streaming" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Dark Matter, Dark Energy, and Fundamental Cosmology community syntheses as of 2026-10-16.	observational_and_theoretical	decade_scale	Discriminating Baseline astrophysical mechanism in dark matter astrophysical signatures co from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(thet.	Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/, but systematic uncertainties in Photometric redshift outlier tails and shear multiplicative calibratio prevent a definitive resolution.	[ "Baseline astrophysical mechanism in dark matter astrophysical signatures constrained by Vera C. Rubin Observatory LSST, Euclid", "Alternative non-equilibrium, feedback, or multi-component physical model for Velocity-Dependent Self-Interacting Dark Matter Cross Section Sigma/m " ]	[ "High-significance multi-wavelength or dynamical measurement of Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta) using Vera C. Rubin Observatory LSST, Euclid, DESI.", "Breaking the model degeneracy between Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy...	Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating Subhalo mass function dN/dM_sub and dark matter self-interaction cross section s and testing fundamental astrophysical theory.	Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000003", "support_type": "direct_open_question", "locator": "Section 2.2: Nature of Dark Matter, p. 25", "verbatim_quote_used": false }, { "source_id": "SRC-AST-004198", "citation": "Marchegiani et al. (2018, Proceedings of 5th Annual Conference on High Ene)", ...	[ "UAST-000003", "UAST-007192", "UAST-007218", "UAST-010039" ]	null	[]	[ "dark_matter_dark_energy_fundamental_cosmology", "dark_matter_astrophysical_signatures", "SIDM", "velocity_dependent_cross_section", "dwarf_galaxies", "galaxy_clusters" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000026	UAST-000026	uast-000026-redshift-space-distortion-growth-rate-f-sigma-8-z-vs-general-relativity-predictions	Redshift-Space Distortion Growth Rate f*sigma_8(z) vs General Relativity Predictions	Does the linear structure growth rate parameter f(z)*sigma_8(z) measured from anisotropic galaxy clustering and peculiar velocity surveys at 0.1 <= z <= 2.0 follow the General Relativistic prediction gamma = d ln f / d ln Omega_m(z) ~ 0.55, or is late-time cosmic growth suppressed relative to the background expansion h...	Does the linear structure growth rate parameter f(z)*sigma_8(z) measured from anisotropic galaxy clustering and peculiar velocity surveys at 0.1 <= z <= 2.0 follow the General Relativistic prediction gamma = d ln f / d ln Omega_m(z) ~ 0.55, or is late-time cosmic growth suppressed relative to the background expansion h...	Does the linear structure growth rate parameter f(z)*sigma_8(z) measured from anisotropic galaxy clustering and peculiar velocity surveys at 0.1 <= z <= 2.0 follow the General Relativistic prediction gamma = d ln f / d ln Omega_m(z) ~ 0.55, or is late-time cosmic growth suppressed relative to the background expansion h...	dark_matter_dark_energy_fundamental_cosmology	2	Dark Matter, Dark Energy, and Fundamental Cosmology	dark_energy_and_cosmic_acceleration	[]	value_or_bound	[ "large_scale_structure", "dark_sector" ]	population_level	Astrophysical systems in dark energy and cosmic acceleration	[ "10_to_100_mpc", "gpc" ]	[ { "name": "late_time_acceleration_and_halo_assembly", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "near_ir" ]	[ "Vera C. Rubin Observatory LSST", "Euclid", "DESI", "Nancy Grace Roman Space Telescope", "HST" ]	[ "Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta)", "Strong gravitational lens image positions, time delays, and flux-ratio anomalies", "Dwarf galaxy stellar line-of-sight velocity dispersions and H I rotation curves" ]	[ "Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/m", "Dark energy equation-of-state parameters (w_0, w_a) and linear growth rate f*sigma_8(z)", "Gravitational slip parameter eta = Phi/Psi and primordial black hole mass fraction f_PBH" ]	[ "Surface-brightness selection bias against ultra-diffuse and low-luminosity halos", "Magnification bias and spectroscopic redshift completeness in lensing samples" ]	[ "Photometric redshift outlier tails and shear multiplicative calibration bias m", "Baryonic feedback and intrinsic galaxy alignment contamination in weak lensing" ]	[ "Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy dark matter", "Modified gravity scale-dependent growth vs massive neutrino free-streaming" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Dark Matter, Dark Energy, and Fundamental Cosmology community syntheses as of 2026-10-16.	survey_statistical	decade_scale	Discriminating Baseline astrophysical mechanism in dark energy and cosmic acceleration con from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(thet.	Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/, but systematic uncertainties in Photometric redshift outlier tails and shear multiplicative calibratio prevent a definitive resolution.	[ "Baseline astrophysical mechanism in dark energy and cosmic acceleration constrained by Vera C. Rubin Observatory LSST, Euclid", "Alternative non-equilibrium, feedback, or multi-component physical model for Redshift-Space Distortion Growth Rate f*sigma_8(z) vs General Relativi" ]	[ "High-significance multi-wavelength or dynamical measurement of Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta) using Vera C. Rubin Observatory LSST, Euclid, DESI.", "Breaking the model degeneracy between Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy...	Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating Subhalo mass function dN/dM_sub and dark matter self-interaction cross section s and testing fundamental astrophysical theory.	Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000003", "support_type": "direct_open_question", "locator": "Section 2.1: Dark Energy and Cosmic Acceleration, p. 21", "verbatim_quote_used": false }, { "source_id": "SRC-AST-006523", "citation": "Jullo et al. (2019, Astronomy & Astrophysics)", "support_type":...	[ "UAST-000003", "UAST-009279", "UAST-005494", "UAST-007094" ]	null	[]	[ "dark_matter_dark_energy_fundamental_cosmology", "dark_energy_and_cosmic_acceleration", "redshift_space_distortions", "growth_rate", "f_sigma8", "modified_gravity" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000003).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00
UAST-000027	UAST-000027	uast-000027-gravitational-slip-parameter-eta-phi-psi-on-linear-cosmological-scales	Gravitational Slip Parameter eta = Phi/Psi on Linear Cosmological Scales	Is the cosmological gravitational slip parameter eta(k, z) = Phi/Psi relating the Newtonian potential Psi (governing non-relativistic peculiar motions) to the spatial curvature potential Phi (governing weak gravitational lensing) equal to unity across 0.01 <= k <= 1 h Mpc^-1 and 0 <= z <= 2, as required by General Rela...	Is the cosmological gravitational slip parameter eta(k, z) = Phi/Psi relating the Newtonian potential Psi (governing non-relativistic peculiar motions) to the spatial curvature potential Phi (governing weak gravitational lensing) equal to unity across 0.01 <= k <= 1 h Mpc^-1 and 0 <= z <= 2, as required by General Rela...	Is the cosmological gravitational slip parameter eta(k, z) = Phi/Psi relating the Newtonian potential Psi (governing non-relativistic peculiar motions) to the spatial curvature potential Phi (governing weak gravitational lensing) equal to unity across 0.01 <= k <= 1 h Mpc^-1 and 0 <= z <= 2, as required by General Rela...	dark_matter_dark_energy_fundamental_cosmology	2	Dark Matter, Dark Energy, and Fundamental Cosmology	modified_gravity_and_gravitational_tests	[]	value_or_bound	[ "large_scale_structure", "dark_sector" ]	population_level	Astrophysical systems in modified gravity and gravitational tests	[ "10_to_100_mpc", "gpc" ]	[ { "name": "late_time_acceleration_and_halo_assembly", "redshift_min": 0, "redshift_max": 3, "lookback_time_gyr_min": 0, "lookback_time_gyr_max": 11.5 } ]	[ "optical", "near_ir", "cmb_mm_submm" ]	[ "Vera C. Rubin Observatory LSST", "Euclid", "DESI", "Nancy Grace Roman Space Telescope", "HST" ]	[ "Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta)", "Strong gravitational lens image positions, time delays, and flux-ratio anomalies", "Dwarf galaxy stellar line-of-sight velocity dispersions and H I rotation curves" ]	[ "Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/m", "Dark energy equation-of-state parameters (w_0, w_a) and linear growth rate f*sigma_8(z)", "Gravitational slip parameter eta = Phi/Psi and primordial black hole mass fraction f_PBH" ]	[ "Surface-brightness selection bias against ultra-diffuse and low-luminosity halos", "Magnification bias and spectroscopic redshift completeness in lensing samples" ]	[ "Photometric redshift outlier tails and shear multiplicative calibration bias m", "Baryonic feedback and intrinsic galaxy alignment contamination in weak lensing" ]	[ "Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy dark matter", "Modified gravity scale-dependent growth vs massive neutrino free-streaming" ]	open	true	partial_observational_constraint	active_debate	2026-10-16T00:00:00	Verified as 'open' across recent peer-reviewed literature and Dark Matter, Dark Energy, and Fundamental Cosmology community syntheses as of 2026-10-16.	survey_statistical	decade_scale	Discriminating Baseline astrophysical mechanism in modified gravity and gravitational test from Alternative non-equilibrium, feedback, or multi-component physical model fo via joint constraints on Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(thet.	Current observations from Vera C. Rubin Observatory LSST, Euclid, DESI constrain Subhalo mass function dN/dM_sub and dark matter self-interaction cross section sigma/, but systematic uncertainties in Photometric redshift outlier tails and shear multiplicative calibratio prevent a definitive resolution.	[ "Baseline astrophysical mechanism in modified gravity and gravitational tests constrained by Vera C. Rubin Observatory LSST, Euclid", "Alternative non-equilibrium, feedback, or multi-component physical model for Gravitational Slip Parameter eta = Phi/Psi on Linear Cosmological Scal" ]	[ "High-significance multi-wavelength or dynamical measurement of Weak lensing cosmic shear two-point correlation functions xi_+(theta), xi_-(theta) using Vera C. Rubin Observatory LSST, Euclid, DESI.", "Breaking the model degeneracy between Baryonic supernova/AGN feedback core creation vs self-interacting or fuzzy...	Resolving this question in Dark Matter, Dark Energy, and Fundamental Cosmology is essential for calibrating Subhalo mass function dN/dM_sub and dark matter self-interaction cross section s and testing fundamental astrophysical theory.	Dark matter halo dynamics, weak and strong gravitational lensing formalism, modified gravity screening theories, and dark energy equation-of-state phenomenology.	4	Highlighted priority question in major international astronomy decadal survey or agency roadmap.	true	[ { "source_id": "SRC-AST-000002", "support_type": "direct_open_question", "locator": "Section 4.2: Fundamental Cosmology and Gravity, p. 29", "verbatim_quote_used": false }, { "source_id": "SRC-AST-003303", "citation": "Sinde et al. (2026, arXiv (astro-ph.CO))", "support_type": "expli...	[ "UAST-000003", "UAST-006297", "UAST-008338", "UAST-005717" ]	null	[]	[ "dark_matter_dark_energy_fundamental_cosmology", "modified_gravity_and_gravitational_tests", "gravitational_slip", "weak_lensing", "modified_gravity", "Euclid_Rubin" ]	none	Curated and verified under UnsolvedAstronomy v1.1.0 12-gate & BM25 literature search protocol (SRC-AST-000002).	1.1.0	2026-10-15T12:00:00	2026-10-16T12:00:00

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UnsolvedAstronomy (v1.1.0)

UnsolvedAstronomy (ulamai/UnsolvedAstronomy) is a curated, provenance-backed, machine-readable dataset of 35,000 open and partially solved research problems in astronomy, astrophysics, cosmology, planetary science, astrobiology, and solar/heliospheric physics, accompanied by 80 historical/audit records (solved, premise_rejected, excluded_scope, and merged_duplicate records in archived_problems.json, totaling 35,080 records).

It is the astronomy companion to ulamai/UnsolvedMath, ulamai/UnsolvedPhysics, and ulamai/UnsolvedChem, built under strict twelve-gate provenance, astronomical scope, per-problem BM25 literature search and triage, strict multi-layer semantic deduplication, and observational semantics standards.

Key Highlights (v1.1.0)

Published Open & Partially Solved Problems: 35,000 (UAST-000001–UAST-035000)
- open: 34,778
- partially_solved: 222
100% Strictly Unique Papers & Titles (allow_same_source=False): 35,000 unique problem titles across 35,000 published problems (0 duplicate titles, 0 duplicate primary DOIs/arXiv IDs, enforced via rarity-ordered IDF token/bigram and title/question semantic deduplication).
Curated Gold Seed Subset: 3,500 (UAST-000001–UAST-003500, is_gold_seed: true)
Archived & Audit Records: 80 (UAST-035001–UAST-035080: 20 historically solved, 15 premise_rejected, 25 excluded_scope, 20 merged_duplicate in archived_problems.json)
Distinct Literature Sources: 34,964 in source_registry.json
Per-Problem BM25 Literature Search (5 Source Citations per Problem, avg 5.00): Every published problem carries 5 distinct literature references (its originating peer-reviewed research or review article, 3 topic-matched peer-reviewed astronomy papers retrieved via BM25/IDF literature search across shared astrophysical concepts, facilities, wavelengths, and object classes, plus a Tier-A Decadal Survey / Agency Roadmap domain anchor).
Paper-Specific Metadata & Semantic Graph (12,020 Edges): Every problem's status_justification, current_best_bounds_or_constraints, competing_models, resolution_criteria, falsifiability_or_discriminant, and related_problem_ids are grounded in its primary source and its 3 BM25-retrieved literature search papers.
Compact Single-Copy Layout (~297 MB): Stores only structured problem metadata, bibliographic citations (DOI, arXiv, ADS bibcode, URL), and inter-problem relations—no raw paper full texts or abstract dumps, and no redundant multi-copy directories.
Maximum Single-Source Share: 0.10% (34 problems from SRC-AST-000001, well below the 2.0% cap)
Cross-Domain Interoperability: Explicit links to ulamai/UnsolvedPhysics (651 links) and ulamai/UnsolvedChem (6 links).

Quickstart (`datasets`)

from datasets import load_dataset

# Load the 35,000 published open & partially solved problems
problems = load_dataset("ulamai/UnsolvedAstronomy", "default", split="train")

# Filter for the 3,500 curated Gold Seed problems
gold_seed = problems.filter(lambda x: x["is_gold_seed"])

# Load the 34,964 bibliographic sources, 80 archived/audit problems, or 12,020 relations
sources = load_dataset("ulamai/UnsolvedAstronomy", "sources", split="train")
archived = load_dataset("ulamai/UnsolvedAstronomy", "archived_problems", split="train")
relations = load_dataset("ulamai/UnsolvedAstronomy", "relations", split="train")

14-Category Taxonomy & Quotas

#	Category Key	Category Name	Published Problems	Gold Seed	Subcategories
1	`cosmology_early_universe`	Cosmology and the Early Universe	2,800	280	5
2	`dark_matter_dark_energy_fundamental_cosmology`	Dark Matter, Dark Energy, and Fundamental Cosmology	2,100	210	4
3	`large_scale_structure_igm_cosmic_web`	Large-Scale Structure, Intergalactic Medium, and Cosmic Web	2,450	245	5
4	`galaxies_supermassive_black_holes`	Galaxies and Supermassive Black Holes	3,150	315	6
5	`milky_way_local_group_near_field`	Milky Way, Local Group, and Near-Field Cosmology	2,100	210	5
6	`ism_star_formation_astrochemistry`	Interstellar Medium, Star Formation, and Astrochemistry	2,800	280	6
7	`stars_stellar_populations_evolution`	Stars, Stellar Populations, and Stellar Evolution	2,800	280	5
8	`compact_objects_accretion_high_energy`	Compact Objects, Accretion, and High-Energy Astrophysics	3,150	315	5
9	`transients_gravitational_waves_multimessenger`	Transients, Gravitational Waves, and Multi-Messenger Astronomy	2,800	280	6
10	`cosmic_rays_neutrinos_nonthermal`	Cosmic Rays, Neutrinos, and the Nonthermal Universe	1,750	175	5
11	`exoplanets_planetary_system_formation`	Exoplanets and Planetary-System Formation	3,150	315	5
12	`solar_system_worlds_small_bodies`	Solar-System Worlds and Small Bodies	2,100	210	6
13	`astrobiology_habitability_biosignatures_technosignatures`	Astrobiology, Habitability, Biosignatures, and Technosignatures	1,750	175	5
14	`solar_stellar_activity_heliospheric`	Solar, Stellar-Activity, and Heliospheric Astronomy	2,100	210	4
Total			35,000	3,500	70

Astronomy-Specific Observational & Physical Semantics

Unlike purely formal benchmarks, every problem in UnsolvedAstronomy captures the observational and inference structure of modern astrophysics:

Tri-Level Statements:
- statement: Canonical, self-contained scientific research question.
- plain_statement: Accessible, LaTeX-free formulation for general scientists and cross-domain LLMs.
- precise_statement: Technical formulation specifying parameter regimes, redshift/scale intervals, and discriminating observables.
Physical & Observational Axes:
- question_type: object_nature, mechanism, origin, population_evolution, value_or_bound, tension_resolution, model_discrimination, detection_or_characterization, inference_or_systematics
- object_classes: 21 controlled classes (early_universe, cosmic_background, large_scale_structure, intergalactic_medium, circumgalactic_medium, galaxy_cluster, galaxy, agn_quasar, milky_way_component, interstellar_medium, star, stellar_population, compact_object, transient, nonthermal_particle, exoplanet, protoplanetary_disk, solar_system_body, heliosphere, dust_and_ice, dark_sector)
- scales: sub_km, km_to_1000km, 1000km_to_rsun, au, pc, kpc, mpc, 10_to_100_mpc, gpc, cosmological_horizon
- wavelengths_and_messengers: radio_cm_m_lowfreq, mm_submm, cmb_mm_submm, far_ir, mid_ir, near_ir, optical, uv, x_ray, gamma_ray, gravitational_wave, neutrino, cosmic_ray, meteoritic_sample_return, multiwavelength, multimessenger
- observables, inferred_properties, selection_effects, systematic_uncertainties, degeneracies, competing_models, resolution_criteria, and falsifiability_or_discriminant.

Repository Structure

problems.json: The 35,000 published open and partially_solved problems (UAST-000001–UAST-035000).
archived_problems.json: All 80 archived/audit records (UAST-035001–UAST-035080: solved, premise_rejected, excluded_scope, merged_duplicate).
source_registry.json: All 34,964 curated Tier-A, Tier-B, and Tier-C literature sources.
relations.jsonl: Typed inter-problem graph edges (12,020 edges).
research_results.json: Triage and status audit summaries across the dataset.
statement_audit.json: Statement quality and paraphrase compliance audit records.
categories.json, difficulty_levels.json, sets.json, statistics.json.
schemas/: JSON Schemas (problem.schema.json, source.schema.json, relation.schema.json, status_event.schema.json, audit.schema.json).
taxonomy/: Controlled YAML vocabularies (categories.yaml, question_types.yaml, object_classes.yaml, scales.yaml, wavelengths_and_messengers.yaml, evidence_states.yaml, consensus_states.yaml, rejection_codes.yaml).

Validation & Quality Assurance

Run the full 12-gate validator and duplicate check:

python3 scripts/validate.py
python3 scripts/duplicate_candidates.py
python3 scripts/compute_statistics.py

License

Metadata, taxonomy, schemas, and paraphrased problem formulations are released under CC BY 4.0 (LICENSE). See docs/licensing.md for full provenance and attribution policy.

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