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REVIEW 3 major objections 6 minor 86 references

The Hubble tension is anchored in the calibrated brightness of Type Ia supernovae, not in the universe's late-time expansion history.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-03 04:31 UTC pith:ZA7HOQ3Q

load-bearing objection Efstathiou's argument that the Hubble tension is really an M_B tension insulated from DESI's evolving dark energy is logically sound and likely correct; the quantitative 7σ is conditional on distance-ladder systematics that the paper itself does not fully close. the 3 major comments →

arxiv 2607.29562 v1 pith:ZA7HOQ3Q submitted 2026-07-31 astro-ph.CO

Late Time Dynamical Dark Energy and the CMB-Distance Ladder Tension

George Efstathiou This is my paper
classification astro-ph.CO PACS 98.80.-k95.36.+x
keywords Hubble tensionType Ia supernovaeabsolute magnitudedark energy equation of statebaryon acoustic oscillationsinverse distance ladderCMBdistance ladder
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper argues that the so-called Hubble tension is really a tension in one number: the standardized peak absolute magnitude M_B of Type Ia supernovae at maximum light. The distance ladder fixes M_B without any cosmology, while CMB data plus the standard cosmological model predict a value 0.23 magnitudes brighter, a gap of about 7 sigma. The paper shows this gap does not depend on which late-time expansion history is assumed, including evolving dark energy hinted by recent baryon-acoustic-oscillation data. Converting M_B into a Hubble constant requires a model, but the supernova magnitude-redshift relation constrains that model tightly enough that the conversion error is an order of magnitude below the measured tension. Therefore any resolution must be either cumulative systematic errors in the ladder or new physics more exotic than smooth dark energy.

Core claim

On the paper's own terms, the central discovery is a reframing: the 'Hubble tension' between local distance measurements and the CMB is not primarily a conflict over the expansion rate H0 but a conflict over the standardized peak absolute magnitude M_B of Type Ia supernovae. The first two rungs of the distance ladder measure M_B = -19.204 ± 0.030 from 17 nearby Cepheid-calibrated host galaxies, with no cosmological assumption. The same supernova population, inserted into CMB-constrained standard cosmology and fit over redshifts 0.04 to 1, demands M_B = -19.430 ± 0.013. The 0.23-magnitude gap is about 7 sigma and survives any smooth change in the late-time expansion history; fitting the magni

What carries the argument

The load-bearing object is M_B, the standardized peak absolute magnitude of Type Ia supernovae, tied to distance by m_B = M_B + 25 + 5 log10 D_L. The distance ladder's first two rungs measure M_B locally without cosmology; CMB plus standard cosmology fixes it from Hubble-flow supernovae. The paper also uses the intercept a_B of the magnitude-redshift relation and the inverse distance ladder (baryon acoustic oscillations calibrated by the CMB sound horizon) to show the low-H0 side is robust. The identity that carries the argument: because supernova magnitude-redshift data constrain the expansion history tightly, any uncertainty in converting M_B to H0 is an order of magnitude smaller than the

Load-bearing premise

The load-bearing premise is that the 17 nearby Cepheid-calibrated supernova host galaxies and their distance moduli are free of unidentified systematic errors and are a representative sample of the more distant Hubble-flow supernovae; if that fails, the roughly 7-sigma M_B gap collapses into a calibration effect.

What would settle it

Find a currently unknown distance-ladder systematic—for example a magnitude-dependent bias in Cepheid photometry or a host-galaxy selection effect that correlates M_B with distance modulus—that shifts the mean M_B of the 17 calibrator hosts by about 0.2 magnitudes. Alternatively, an independent geometric calibration of supernova absolute magnitude at 0.05-magnitude precision using gravitational-wave standard sirens would settle whether the offset is real.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the M_B tension is real, the Hubble tension cannot be dissolved by any smooth dynamical-dark-energy model consistent with current BAO plus CMB data; a resolution requires new physics that changes the early universe or cumulative ladder systematics.
  • Using a distance-ladder prior on H0 rather than on M_B to test cosmological models can produce misleading conclusions; the M_B prior plus supernova data is the safer route.
  • Supernova-only fits with the Cepheid M_B calibration give H0 = 75.0 ± 1.1 km/s/Mpc, 1.5 km/s/Mpc above the baseline multi-indicator value, indicating the host-galaxy distance moduli carry a systematic offset that the quoted error bars may not cover.
  • The inverse distance ladder returns H0 near 69 km/s/Mpc, matching the CMB value, so the high-H0 side cannot be achieved without abandoning the standard sound-horizon scale.
  • A revised supernova catalogue shifts the inferred H0 by only 0.4 km/s/Mpc relative to the standard one, so the main conclusions are robust to the choice of supernova compilation.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • A testable extension: split the 17 calibrator host galaxies by distance and compare Cepheid-based distance moduli with an independent distance indicator in the same galaxies; if the trend visible in the paper's Figure 1 survives, it points to a distance-dependent selection effect rather than new physics.
  • Future distance-ladder results should be published as M_B with the full covariance, not only H0; propagation of M_B into H0 under different expansion models is then a trivial re-weighting that hides no information.
  • If unidentified systematics are ruled out, the next concrete discriminator is a measurement of the sound horizon from a local, model-independent probe such as gravitational-wave standard sirens, since the inverse ladder pins H0 low only through the CMB sound-horizon anchor.
  • The argument suggests a consistency check: determine whether the 0.23-magnitude offset between local and cosmological M_B is constant with redshift or evolves; a constant offset would favor a zero-point error in the Cepheid anchor, while an evolving offset would favor new physics.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper argues that the Hubble tension is most directly expressed as a tension in the standardized SNIa absolute magnitude M_B between the distance-ladder calibration (Eq. 2: M_B = −19.204 ± 0.030) and the value inferred from CMB+ΛCDM plus the SN magnitude–redshift relation (Eq. 3: M_B = −19.430 ± 0.013), a 0.23 mag discrepancy at ~7σ. The central logical claim is that this M_B tension is independent of the late-time expansion history: the ladder calibration requires no cosmology, and converting M_B to H0 via the SN Hubble diagram introduces only small shifts (Table 2: H0 = 74.7–75.2 km/s/Mpc across fitting schemes). The paper then shows that DESI BAO+CMB hints for evolving dark energy, when extrapolated to z ≈ 0 through a CPL prior (Eqs. 9a,b), change H0 by only 0.3–0.4 km/s/Mpc, so smooth late-time dynamical dark energy cannot resolve the tension. The conclusions are explicitly conditional on the absence of unidentified distance-ladder systematics, and the paper itself documents a 0.04–0.05 mag offset between JWST-Cepheid and H0DN-baseline distance moduli for the same host galaxies.

Significance. If the central claim holds, the paper provides a clean reframing of the Hubble tension: it is a SNIa absolute-magnitude tension that cannot be removed by any smooth late-time dark-energy evolution, including the DESI-favored w0wa models. This is an important and clarifying contribution to the field, with direct implications for model-building (resolution requires either distance-ladder systematics or new physics beyond late-time expansion modifications). The paper's strengths include a transparent, simplified reproduction of the H0DN analysis; explicit covariance treatment for the geometric anchor (Eq. 1b); multiple fitting schemes demonstrating the H0-conversion insensitivity; and a fair, quantitative comparison with the inverse distance ladder and with DES-Dovekie. However, the quantitative '~7σ' claim rests on an assumed covariance model whose goodness of fit is not reported, and the paper itself surfaces systematic offsets in the distance moduli that could affect that significance. These points are load-bearing for the headline significance.

major comments (3)
  1. [§2, Eq. (1b), Fig. 1] The headline '~7σ' rests on Eq. (2), but no goodness-of-fit statistic is reported for the covariance model of Eq. (1b). Fig. 1 shows a visible trend in M_B with distance modulus, with several points >2σ from the mean. The authors condition the central claim on the absence of unidentified systematics; a trend of this type is exactly the symptom that would invalidate that condition. Please report χ²/dof, the significance of a slope β in M_B = α + β(µ − µ_ref), and a version of Eq. (2) with any trend accounted for. If the trend is driven by sample selection or residual Cepheid/SN systematics, the 0.23 mag tension could be reduced, so this is load-bearing.
  2. [§3, distance moduli] The paper itself notes that replacing JWST Cepheid moduli with H0DN baseline moduli for the same 17 galaxies shifts M_B from −19.204 ± 0.030 to −19.24 ± 0.02 and H0 from 75.0 to 73.5 km/s/Mpc. The corresponding ~0.04–0.05 mag offset is larger than the formal error of Eq. (2) and more than twice the H0DN H0 error; the text acknowledges this 'calls into question whether the H0DN error budget accurately reflects... systematic errors.' This is an internal admission that distance moduli are not settled. Please quantify the impact of this offset on the M_B tension with Eq. (3) and include a systematic term in Eq. (1b) or justify why it can be neglected.
  3. [§4, Eqs. (9a,b), Table 2] The demonstration that late-time dark energy does not affect the tension uses a specific CPL extrapolation with the PACT+DESI+CMB prior. The statement 'insensitive to the actual late time expansion history' is supported for smooth w0wa models, but not for early-time or sound-horizon modifications, which the paper acknowledges only briefly in §4. Since the abstract makes a stronger claim, please add a sentence in the conclusions clarifying the domain of validity (smooth late-time DE parameterizations) and explicitly referencing the sound-horizon caveat.
minor comments (6)
  1. [Abstract, §1, §6] Typos: 'provides tight constrains' → 'provides tight constraints'; 'summarize' → 'summarized'; 'distance latter' → 'distance ladder'.
  2. [§4] The text says 'The value in Table 4 is also consistent...' but the relevant table is Table 2.
  3. [Eq. (4b)] The definition 5a_B = −(M_B + 25 − 5 log10 H0) appears to omit the 5 log10 c term. Since a_B is used consistently this does not affect the results, but the notation should be clarified.
  4. [Fig. 1] The caption lists green and blue bands but the figure as rendered may not distinguish them clearly; please ensure the printed version labels the bands directly.
  5. [Table 1] For galaxies with multiple SNe, the paper says the standardized apparent magnitudes are averaged using the Pan+ covariance matrix, but the table only lists the resulting M_B. State explicitly how the covariance between multiple SNe in the same host enters Eq. (1b).
  6. [Reproducibility] The MultiNest fits in Table 2 and Figs. 2–3 depend on the prior in Eqs. (9a,b). A short reproducibility note with the chains or scripts would strengthen the paper, since the PACT+DESI prior is not tabulated elsewhere.

Circularity Check

0 steps flagged

No significant circularity: the M_B-tension comparison is a direct measurement between two independent estimates, Table 2 H0 values are explicit algebraic conversions of the adopted M_B prior, and the self-citations are not load-bearing.

full rationale

The derivation chain is self-contained. Section 2 computes the ladder value M_B^SN = -19.204 +/- 0.030 (Eq. 2) by minimizing the covariance-weighted chi-square of Eq. (1a) against JWST Cepheid distance moduli and Pan+ SN photometry, and compares it with the CMB+LambdaCDM+Pan+ value M_B^SN = -19.430 +/- 0.013 (Eq. 3). These are two independent estimates, so the 0.226 mag ~7 sigma discrepancy is a measured comparison, not a fitted input renamed as a prediction. The H0 values in Table 2 are not independent predictions: the paper explicitly defines the conversion through 5a_B = -(M_B + 25 - 5 log10 H0) (Eq. 4b), so the quoted H0 values are algebraic re-parameterizations of the adopted M_B prior plus the fitted intercept a_B; this is acknowledged rather than disguised. The DESI-w0wa exercise is labelled as a phenomenological question ('amounts to asking: if the CPL parameterization is extrapolated to z=0 ... what is the impact on H0 if we fit the SN magnitude-redshift relation imposing the distance ladder prior of Eq.2?'), so no prediction is being claimed from the input prior. Self-citations to E21 and Efstathiou 2025 appear, but the cosmology-independence of rungs (i)-(ii) is argued from the structure of the distance ladder and reproduced in Section 2, and the inverse-distance-ladder low H0 is supported by the DESI+Pan+ fit in Table 2; the citations are therefore supporting, not load-bearing. The paper's explicit caveats (Section 1: 'Provided that there are no unidentified systematic errors in the distance ladder measurements...'; Section 3: the 0.048 mag Cepheid-vs-baseline offset 'calls into question whether the H0DN error budget accurately reflects the contributions from systematic errors') qualify the quantitative significance but are honest limitations, not circular steps. No equation is equivalent to its own input by construction.

Axiom & Free-Parameter Ledger

3 free parameters · 6 axioms · 0 invented entities

The paper introduces no new physics, entities, or fitted constants: it re-analyses public data with standard catalogs. The only tuning inputs are the fitting choices above (anchor error, cosmographic pivot values, redshift windows, and the external DESI+CMB prior of Eqs. 9a–9b). The central claim is a logical consequence of how the ladder M_B is defined plus the robustness of the measured M_B offset.

free parameters (3)
  • geometric anchor correlated error δµ_anchor = 0.02 mag
    Input from Riess et al. (2021b) used to set the off-diagonal covariance in Eq. 1b; it directly sets the reported error on the ladder M_B (Eq. 2).
  • fixed cosmographic parameters q0, j0 (baseline fit) = q0 = −0.55, j0 = 1
    Fixed near-ΛCDM values in Eq. 5 for the baseline intercept a_B = 0.7164 ± 0.0017 (Eq. 6) and Table 1 galaxy-by-galaxy H0 values; freeing them (Table 2) shifts H0 by ≤ 0.2 km/s/Mpc within the same redshift window.
  • redshift fitting windows = 0.023–0.15; 0.04–0.30; 0.04–1.0
    Choice of SN fitting range changes a_B and hence H0; the spread across windows (Table 2) is used to argue the H0 conversion is insensitive.
axioms (6)
  • domain assumption Standardized SNIa peak magnitudes are universal — the nearby Cepheid-host SN and the distant z = 0.04–1 Hubble-flow SN have the same M_B after Pan+ light-curve standardization.
    Load-bearing for comparing Eq. 2 with Eq. 3; footnote 6 waives the representativeness requirement.
  • domain assumption The 17 JWST Cepheid host galaxies are a representative, unbiased calibration sample.
    Fig. 1 shows a trend of M_B with distance modulus; Riess et al. (2024) attribute part to selection; CCHP contests the calibration (Freedman et al. 2025).
  • domain assumption Flat base ΛCDM with the PACT+Planck-lowl likelihood combination is the correct reference model for the CMB-derived M_B (Eq. 3).
    The tension is defined against this model; the paper tests it, does not derive it.
  • standard math Distance-modulus relation m_B = M_B + 25 + 5 log10 D_L (Eq. 4a) and the Hubble-constant conversion 5a_B = −(M_B + 25 − 5 log10 H0) (Eq. 4b).
    Definitional identity used throughout the analysis.
  • domain assumption Spatially flat geometry (footnote 7).
    Flatness is assumed in all distance fits; the PACT+DESI priors also assume it.
  • domain assumption The CPL parameterization w(z) = w0 + wa z/(1+z) (Eq. 8) describes plausible smooth late-time dark energy.
    Adopted from Chevallier & Polarski (2001) and Linder (2003); §6 calls the z→0 extrapolation 'extraordinarily poorly motivated'.

pith-pipeline@v1.3.0-daily-deepseek · 11600 in / 27949 out tokens · 270577 ms · 2026-08-03T04:31:15.784515+00:00 · methodology

0 comments
read the original abstract

The traditional distance ladder measures the standardized peak absolute magnitude M^B of Type Ia supernovae (SNIa). According to the SH0ES collaboration, the distance ladder value of M^B is highly discrepant with the value inferred from the cosmic microwave background (CMB) assuming the LCDM cosmology. This CMB-distance ladder tension is insensitive to the actual late time expansion history of the Universe. To derive a value of the Hubble constant H_0, from M^B requires a cosmological model. However, the magnitude-redshift relation of SNIa provides tight constrains the expansion history. As a consequence, uncertainties in the conversion of M^B into H_0 have no significant impact on the CMB-distance ladder tension. The tentative claim by the Dark Energy Spectroscopic Instrument collaboration for late time evolution of the dark energy equation of state does not alter this conclusion.

Figures

Figures reproduced from arXiv: 2607.29562 by George Efstathiou.

Figure 1
Figure 1. Figure 1: The points with error bars show the peak standardized Type Ia SN magnitude, MSN B , plotted against distance modulus, µ for SN host galaxies with JWST Cepheid-based distances as listed in Table1. In cases where galaxies host more than one SN, we plot the mean SN magnitude. The green bands show the 1 and 2σ ranges around the mean value of MSN B (Eq. 2) allowed by the data points. The blue band show the 1 an… view at source ↗
Figure 2
Figure 2. Figure 2: The red contours show the constraints on w0 and wa from the CMB combined with DESI DR2 BAO measure￾ments. The CMB constraints use the PACT likelihood com￾bined with CMB lensing (labelled PACT+DESIDR2+lensing). The solid contours show the 1 and 2σ regions allowed by the Pan+ magnitude-redshift relation when the PACT+DESIDR2+lensing constraints on Ωm, w0, wa are imposed as a prior (Eqs. 9a and 9b). The point… view at source ↗
Figure 3
Figure 3. Figure 3: Constraints on w0 and wa combining SN data from Pan+ (blue contours, identical to the solid black con￾tours in [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

discussion (0)

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Reference graph

Works this paper leans on

86 extracted references · 4 canonical work pages · 2 internal anchors

  1. [1]

    Updated 1.1% Precision Values of the Hubble Constant with Corrected Pantheon+ and Dark Energy Survey (DES)-DOVEKIE Type Ia Supernovae

    Updated 1.1\. arXiv e-prints , keywords =. doi:10.48550/arXiv.2607.24443 , archivePrefix =. 2607.24443 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2607.24443

  2. [2]

    , keywords =

    On the stability of H _ 0 and the inverse distance ladder. , keywords =. doi:10.1093/mnras/stag1267 , archivePrefix =. 2602.12822 , primaryClass =

    arXiv

  3. [3]

    arXiv e-prints , keywords =

    A Reassessment of the Pantheon+ and DES 5YR Calibration Uncertainties: Dovekie. arXiv e-prints , keywords =. doi:10.48550/arXiv.2506.05471 , archivePrefix =. 2506.05471 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2506.05471

  4. [4]

    , keywords =

    The Dark Energy Survey supernova program: a reanalysis of cosmology results and evidence for evolving dark energy with an updated Type Ia supernova calibration. , keywords =. doi:10.1093/mnras/stag632 , archivePrefix =. 2511.07517 , primaryClass =

    Pith/arXiv arXiv

  5. [5]

    , keywords =

    Comparing the DES-SN5YR and Pantheon+ SN cosmology analyses: investigation based on 'evolving dark energy or supernovae systematics'?. , keywords =. doi:10.1093/mnras/staf943 , archivePrefix =. 2501.06664 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    , keywords =

    Cosmological Model Insensitivity of Local H _ 0 from the Cepheid Distance Ladder. , keywords =. doi:10.3847/1538-4357/ab7fb0 , archivePrefix =. 2001.09260 , primaryClass =

    Pith/arXiv arXiv 2001

  7. [7]

    MultiNest: Efficient and Robust Bayesian Inference

  8. [9]

    Physics of the Dark Universe , keywords =

    The Ups and Downs of Early Dark Energy solutions to the Hubble tension: A review of models, hints and constraints circa 2023. Physics of the Dark Universe , keywords =. doi:10.1016/j.dark.2023.101348 , archivePrefix =. 2302.09032 , primaryClass =

    arXiv 2023

  9. [10]

    arXiv e-prints , keywords =

    The Mirage of w=-1. arXiv e-prints , keywords =. doi:10.48550/arXiv.0708.0024 , archivePrefix =. 0708.0024 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.0708.0024

  10. [11]

    , keywords =

    DESI 2024: Constraints on physics-focused aspects of dark energy using DESI DR1 BAO data. , keywords =. doi:10.1103/PhysRevD.111.023532 , archivePrefix =. 2405.13588 , primaryClass =

    Pith/arXiv arXiv 2024

  11. [12]

    arXiv e-prints , keywords =

    Union3.1: Self-consistent Measurements of Host Galaxy Properties for 2000 Type Ia Supernovae. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.19424 , archivePrefix =. 2601.19424 , primaryClass =

    doi:10.48550/arxiv.2601.19424 2000

  12. [13]

    , keywords =

    Evolving dark energy or supernovae systematics?. , keywords =. doi:10.1093/mnras/staf301 , archivePrefix =. 2408.07175 , primaryClass =

    Pith/arXiv arXiv

  13. [14]

    , keywords =

    Exploring the Expansion History of the Universe. , keywords =. doi:10.1103/PhysRevLett.90.091301 , archivePrefix =. astro-ph/0208512 , primaryClass =

    Pith/arXiv arXiv

  14. [15]

    International Journal of Modern Physics D , keywords =

    Accelerating Universes with Scaling Dark Matter. International Journal of Modern Physics D , keywords =. doi:10.1142/S0218271801000822 , archivePrefix =. gr-qc/0009008 , primaryClass =

    Pith/arXiv arXiv

  15. [16]

    arXiv e-prints , keywords =

    DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations. arXiv e-prints , keywords =. doi:10.48550/arXiv.2404.03002 , archivePrefix =. 2404.03002 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2404.03002 2024

  16. [17]

    , keywords =

    Cosmological implications of baryon acoustic oscillation measurements. , keywords =. doi:10.1103/PhysRevD.92.123516 , archivePrefix =. 1411.1074 , primaryClass =

    Pith/arXiv arXiv

  17. [18]

    , keywords =

    Standard Rulers, Candles, and Clocks from the Low-Redshift Universe. , keywords =. doi:10.1103/PhysRevLett.113.241302 , archivePrefix =. 1409.6217 , primaryClass =

    Pith/arXiv arXiv

  18. [19]

    , keywords =

    Baryon acoustic oscillations in the Sloan Digital Sky Survey Data Release 7 galaxy sample. , keywords =. doi:10.1111/j.1365-2966.2009.15812.x , archivePrefix =. 0907.1660 , primaryClass =

    arXiv 2009

  19. [20]

    , keywords =

    The Dark Energy Survey Supernova Program: Cosmological Analysis and Systematic Uncertainties. , keywords =. doi:10.3847/1538-4357/ad5e6c , archivePrefix =. 2401.02945 , primaryClass =

    Pith/arXiv arXiv

  20. [21]

    , keywords =

    The Dark Energy Survey Supernova Program: an updated measurement of the Hubble constant using the inverse distance ladder. , keywords =. doi:10.1093/mnras/staf122 , archivePrefix =. 2406.05049 , primaryClass =

    Pith/arXiv arXiv

  21. [22]

    , keywords =

    Baryon acoustic oscillations from a different angle. , keywords =. doi:10.1093/mnras/staf906 , archivePrefix =. 2505.02658 , primaryClass =

    Pith/arXiv arXiv

  22. [23]

    , keywords =

    JWST Validates HST Distance Measurements: Selection of Supernova Subsample Explains Differences in JWST Estimates of Local H _ 0. , keywords =. doi:10.3847/1538-4357/ad8c21 , archivePrefix =. 2408.11770 , primaryClass =

    Pith/arXiv arXiv

  23. [24]

    , keywords =

    SRoll2: an improved mapmaking approach to reduce large-scale systematic effects in the Planck High Frequency Instrument legacy maps. , keywords =. doi:10.1051/0004-6361/201834882 , archivePrefix =. 1901.11386 , primaryClass =

    Pith/arXiv arXiv 1901

  24. [25]

    , keywords =

    Reionization optical depth determination from Planck HFI data with ten percent accuracy. , keywords =. doi:10.1051/0004-6361/201936630 , archivePrefix =. 1908.09856 , primaryClass =

    Pith/arXiv arXiv 1908

  25. [26]

    , keywords =

    Inference of the optical depth to reionization from low multipole temperature and polarization Planck data. , keywords =. doi:10.1093/mnras/stab2215 , archivePrefix =. 2103.14378 , primaryClass =

    Pith/arXiv arXiv

  26. [27]

    , keywords =

    The Atacama Cosmology Telescope: DR6 power spectra, likelihoods and CDM parameters. , keywords =. doi:10.1088/1475-7516/2025/11/062 , archivePrefix =. 2503.14452 , primaryClass =

    Pith/arXiv arXiv 2025

  27. [28]

    , keywords =

    The Pantheon+ Analysis: SuperCal-fragilistic Cross Calibration, Retrained SALT2 Light-curve Model, and Calibration Systematic Uncertainty. , keywords =. doi:10.3847/1538-4357/ac8bcc , archivePrefix =. 2112.03864 , primaryClass =

    Pith/arXiv arXiv

  28. [29]

    , keywords =

    The Pantheon+ Analysis: The Full Data Set and Light-curve Release. , keywords =. doi:10.3847/1538-4357/ac8b7a , archivePrefix =. 2112.03863 , primaryClass =

    Pith/arXiv arXiv

  29. [30]

    , keywords =

    The Perfect Host: JWST Cepheid Observations in a Background-free Type Ia Supernova Host Confirm No Bias in Hubble-constant Measurements. , keywords =. doi:10.3847/2041-8213/ae0ad6 , archivePrefix =. 2509.01667 , primaryClass =

    Pith/arXiv arXiv 2041

  30. [31]

    , keywords =

    Crowded No More: The Accuracy of the Hubble Constant Tested with High-resolution Observations of Cepheids by JWST. , keywords =. doi:10.3847/2041-8213/acf769 , archivePrefix =. 2307.15806 , primaryClass =

    Pith/arXiv arXiv 2041

  31. [32]

    arXiv e-prints , keywords =

    On the use of the local prior on the absolute magnitude of Type Ia supernovae in cosmological inference. arXiv e-prints , keywords =

  32. [33]

    , keywords =

    Can late dark energy transitions raise the Hubble constant?. , keywords =. doi:10.1103/PhysRevD.101.103517 , archivePrefix =. 2002.11707 , primaryClass =

    Pith/arXiv arXiv 2002

  33. [34]

    , keywords =

    A buyer's guide to the Hubble constant. , keywords =. doi:10.1007/s00159-021-00137-4 , archivePrefix =. 2109.01161 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    , keywords =

    Measurements of the Hubble Constant: Tensions in Perspective. , keywords =. doi:10.3847/1538-4357/ac0e95 , archivePrefix =. 2106.15656 , primaryClass =

    Pith/arXiv arXiv

  35. [36]

    , keywords =

    The trouble with H _ 0. , keywords =. doi:10.1088/1475-7516/2016/10/019 , archivePrefix =. 1607.05617 , primaryClass =

    Pith/arXiv arXiv 2016

  36. [37]

    The Hubble Constant Tension , year = 2024, editor =

    The Hubble Constant: A Historical Review. The Hubble Constant Tension , year = 2024, editor =. doi:10.1007/978-981-99-0177-7_2 , adsurl =

    work page doi:10.1007/978-981-99-0177-7_2 2024

  37. [38]

    , keywords =

    The Local Distance Network: A community consensus report on the measurement of the Hubble constant at 1\. , keywords =. doi:10.1051/0004-6361/202557993 , archivePrefix =. 2510.23823 , primaryClass =

    Pith/arXiv arXiv

  38. [39]

    , keywords =

    SPT-3G D1: CMB temperature and polarization power spectra and cosmology from 2019 and 2020 observations of the SPT-3G main field. , keywords =. doi:10.1103/7wt3-9v2y , archivePrefix =. 2506.20707 , primaryClass =

    Pith/arXiv arXiv 2019

  39. [40]

    , keywords =

    Status Report on the Chicago-Carnegie Hubble Program (CCHP): Measurement of the Hubble Constant Using the Hubble and James Webb Space Telescopes. , keywords =. doi:10.3847/1538-4357/adce78 , archivePrefix =. 2408.06153 , primaryClass =

    Pith/arXiv arXiv

  40. [41]

    , keywords =

    Progress in direct measurements of the Hubble constant. , keywords =. doi:10.1088/1475-7516/2023/11/050 , archivePrefix =. 2309.05618 , primaryClass =

    Pith/arXiv arXiv 2023

  41. [42]

    arXiv e-prints , keywords =

    Carnegie Supernova Project-I and -II: Measurements of H_0 using Cepheid, TRGB, and SBF Distance Calibration to Type Ia Supernovae. arXiv e-prints , keywords =. doi:10.48550/arXiv.2308.01875 , archivePrefix =. 2308.01875 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2308.01875

  42. [43]

    DESI DR2 results. II. Measurements of baryon acoustic oscillations and cosmological constraints. , keywords =. doi:10.1103/tr6y-kpc6 , archivePrefix =. 2503.14738 , primaryClass =

    Pith/arXiv arXiv

  43. [44]

    The DESI results impact the local determination of $H_0$

    The DESI results impact the local determination of H_0. arXiv e-prints , keywords =. doi:10.48550/arXiv.2606.05358 , archivePrefix =. 2606.05358 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2606.05358

  44. [45]

    , keywords =

    To H _ 0 or not to H _ 0 ?. , keywords =. doi:10.1093/mnras/stab1588 , archivePrefix =. 2103.08723 , primaryClass =

    Pith/arXiv arXiv

  45. [46]

    Classical and Quantum Gravity , keywords =

    In the realm of the Hubble tension-a review of solutions. Classical and Quantum Gravity , keywords =. doi:10.1088/1361-6382/ac086d , archivePrefix =. 2103.01183 , primaryClass =

    Pith/arXiv arXiv

  46. [47]

    Nature , keywords =

    A distance to the Large Magellanic Cloud that is precise to one per cent. Nature , keywords =. 2019. doi:10.1038/s41586-019-0999-4 , archivePrefix =. 1903.08096 , primaryClass =

    Pith/arXiv arXiv 2019

  47. [48]

    arXiv e-prints , keywords =

    An Improved Distance to NGC 4258 and its Implications for the Hubble Constant. arXiv e-prints , keywords =. 2019

    2019

  48. [49]

    , keywords =

    Cosmic Distances Calibrated to 1\. , keywords =. doi:10.3847/2041-8213/abdbaf , archivePrefix =. 2012.08534 , primaryClass =

    Pith/arXiv arXiv 2041

  49. [50]

    arXiv e-prints , keywords =

    Forward-modelling Milky Way Cepheids: selection effects and physical priors in the Gaia-HST calibration. arXiv e-prints , keywords =. doi:10.48550/arXiv.2603.09880 , archivePrefix =. 2603.09880 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2603.09880

  50. [51]

    , keywords =

    Local resolution of the Hubble tension: The impact of screened fifth forces on the cosmic distance ladder. , keywords =. doi:10.1103/PhysRevD.100.043537 , archivePrefix =. 1907.03778 , primaryClass =

    Pith/arXiv arXiv 1907

  51. [52]

    , keywords =

    w -M phantom transition at z _ t <0.1 as a resolution of the Hubble tension. , keywords =. doi:10.1103/PhysRevD.103.083517 , archivePrefix =. 2012.13932 , primaryClass =

    Pith/arXiv arXiv 2012

  52. [53]

    , keywords =

    Gaussian process cosmography. , keywords =. doi:10.1103/PhysRevD.85.123530 , archivePrefix =. 1204.2272 , primaryClass =

    Pith/arXiv arXiv

  53. [54]

    , keywords =

    Model independent inference of the expansion history and implications for the growth of structure. , keywords =. doi:10.1103/PhysRevD.97.123501 , archivePrefix =. 1710.04236 , primaryClass =

    Pith/arXiv arXiv

  54. [55]

    arXiv e-prints , keywords =

    Gaia Early Data Release 3: Parallax bias versus magnitude, colour, and position. arXiv e-prints , keywords =

  55. [56]

    arXiv e-prints , keywords =

    Gaia Early Data Release 3: The astrometric solution. arXiv e-prints , keywords =

  56. [57]

    , keywords =

    Sounds Discordant: Classical Distance Ladder and CDM-based Determinations of the Cosmological Sound Horizon. , keywords =. doi:10.3847/1538-4357/ab0898 , archivePrefix =. 1811.00537 , primaryClass =

    Pith/arXiv arXiv

  57. [58]

    The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions. , keywords =. doi:10.3847/1538-3881/aa8df0 , archivePrefix =. 1709.05146 , primaryClass =

    Pith/arXiv arXiv

  58. [59]

    , keywords =

    The Carnegie Supernova Project: The Low-Redshift Survey. , keywords =. doi:10.1086/500228 , archivePrefix =. astro-ph/0512039 , primaryClass =

    Pith/arXiv arXiv

  59. [60]

    , keywords =

    New Parallaxes of Galactic Cepheids from Spatially Scanning the Hubble Space Telescope: Implications for the Hubble Constant. , keywords =. 2018. doi:10.3847/1538-4357/aaadb7 , archivePrefix =. 1801.01120 , primaryClass =

    Pith/arXiv arXiv 2018

  60. [61]

    , keywords =

    Cepheid parallaxes and the Hubble constant. , keywords =. 2007. doi:10.1111/j.1365-2966.2007.11972.x , archivePrefix =. 0705.1592 , primaryClass =

    arXiv 2007

  61. [62]

    , keywords =

    Hubble Space Telescope Fine Guidance Sensor Parallaxes of Galactic Cepheid Variable Stars: Period-Luminosity Relations. , keywords =. doi:10.1086/511980 , archivePrefix =. astro-ph/0612465 , primaryClass =

    Pith/arXiv arXiv

  62. [63]

    , keywords =

    The evidence for a spatially flat Universe. , keywords =. doi:10.1093/mnrasl/slaa093 , archivePrefix =. 2002.06892 , primaryClass =

    Pith/arXiv arXiv 2002

  63. [64]

    , keywords =

    Model independent H(z) reconstruction using the cosmic inverse distance ladder. , keywords =. doi:10.1093/mnras/sty3082 , archivePrefix =. 1806.06781 , primaryClass =

    Pith/arXiv arXiv

  64. [65]

    ArXiv e-prints , year =

  65. [66]

    Hou, Jiamin and Sánchez, Ariel G and Ross, Ashley J and Smith, Alex and Neveux, Richard and Bautista, Julian and Burtin, Etienne and Zhao, Cheng and Scoccimarro, Román and Dawson, Kyle S and et al. , year=. The completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from anisotropic clustering analysis of the quasar sa...

  66. [67]

    , keywords =

    Baryon acoustic oscillations at z = 2.34 from the correlations of Ly absorption in eBOSS DR14. , keywords =. doi:10.1051/0004-6361/201935638 , archivePrefix =. 1904.03400 , primaryClass =

    Pith/arXiv arXiv 1904

  67. [68]

    , keywords =

    Baryon acoustic oscillations from the cross-correlation of Ly absorption and quasars in eBOSS DR14. , keywords =. doi:10.1051/0004-6361/201935641 , archivePrefix =. 1904.03430 , primaryClass =

    Pith/arXiv arXiv 1904

  68. [69]

    , keywords =

    The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: cosmological analysis of the DR12 galaxy sample. , keywords =. doi:10.1093/mnras/stx721 , archivePrefix =. 1607.03155 , primaryClass =

    Pith/arXiv arXiv

  69. [70]

    arXiv e-prints , keywords =

    A Lockdown Perspective on the Hubble Tension (with comments from the SH0ES team). arXiv e-prints , keywords =

  70. [71]

    , keywords =

    Calibration of the Tip of the Red Giant Branch. , keywords =. doi:10.3847/1538-4357/ab7339 , archivePrefix =. 2002.01550 , primaryClass =

    Pith/arXiv arXiv 2002

  71. [72]

    , keywords =

    Consistent Calibration of the Tip of the Red Giant Branch in the Large Magellanic Cloud on the Hubble Space Telescope Photometric System and a Redetermination of the Hubble Constant. , keywords =. doi:10.3847/1538-4357/ab4bc9 , archivePrefix =. 1908.00993 , primaryClass =

    Pith/arXiv arXiv 1908

  72. [73]

    The Carnegie-Chicago Hubble Program. VIII. An Independent Determination of the Hubble Constant Based on the Tip of the Red Giant Branch. , keywords =. doi:10.3847/1538-4357/ab2f73 , archivePrefix =. 1907.05922 , primaryClass =

    Pith/arXiv arXiv 1907

  73. [74]

    arXiv e-prints , keywords =

    A structured analysis of Hubble tension. arXiv e-prints , keywords =

  74. [75]

    , year = 2020, month = feb, volume =

    Hubble constant hunter's guide. , year = 2020, month = feb, volume =. doi:10.1103/PhysRevD.101.043533 , adsurl =

    doi:10.1103/physrevd.101.043533 2020

  75. [76]

    , keywords =

    Dark Energy Survey Year 1 Results: A Precise H _ 0 Estimate from DES Y1, BAO, and D/H Data. , keywords =. doi:10.1093/mnras/sty1939 , archivePrefix =. 1711.00403 , primaryClass =

    Pith/arXiv arXiv

  76. [77]

    , keywords =

    First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant. , keywords =. doi:10.1093/mnras/stz978 , archivePrefix =. 1811.02376 , primaryClass =

    Pith/arXiv arXiv

  77. [78]

    arXiv , doi =:1707.06547 , keywords =

    , year =. arXiv , doi =:1707.06547 , keywords =

    Pith/arXiv arXiv

  78. [79]

    , archivePrefix = "arXiv", eprint =

    The length of the low-redshift standard ruler. , archivePrefix = "arXiv", eprint =. doi:10.1093/mnras/stx116 , adsurl =

    work page doi:10.1093/mnras/stx116

  79. [80]

    The Astrophysical Journal , keywords =

    A 2.4\. The Astrophysical Journal , keywords =. 2016. doi:10.3847/0004-637X/826/1/56 , archivePrefix =. 1604.01424 , primaryClass =

    Pith/arXiv arXiv 2016

  80. [81]

    The Astrophysical Journal , keywords =

    Large Magellanic Cloud Cepheid Standards Provide a 1\. The Astrophysical Journal , keywords =. 2019. doi:10.3847/1538-4357/ab1422 , archivePrefix =. 1903.07603 , primaryClass =

    Pith/arXiv arXiv 2019

Showing first 80 references.