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arxiv: 2601.07345 · v2 · submitted 2026-01-12 · 🌌 astro-ph.CO · astro-ph.GA

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New H(z) measurement at Redshift = 0.12 with DESI Data Release 1

Ze-fan Wang , Lei Lei , Yi-Zhong Fan
Authors on Pith no claims yet

Pith reviewed 2026-05-16 15:29 UTC · model grok-4.3

classification 🌌 astro-ph.CO astro-ph.GA
keywords Hubble parameterH(z) measurementDESIstellar agespassive galaxiesfull-spectrum fittingcosmologyredshift 0.12
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The pith

New measurement of the Hubble parameter at redshift 0.12 from stellar ages of DESI galaxies gives 71.33 km/s/Mpc.

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

The paper uses full-spectrum fitting on more than four thousand massive passively evolving galaxies from DESI Data Release 1 to determine their stellar ages without assuming any cosmological model. These ages are converted into a direct measurement of the expansion rate at redshift 0.12. The derived value of H(z=0.12) equals 71.33 plus or minus 4.20 kilometers per second per megaparsec. This result matches values obtained by other independent techniques. It supplies an additional low-redshift anchor point for mapping the universe's expansion history.

Core claim

By performing full-spectrum fitting using BAGPIPES on DESI galaxies, the authors derive a new measurement of H(z=0.12)=71.33 ± 4.20 km s^{-1} Mpc^{-1}, which is well consistent with those derived in other ways.

What carries the argument

Full-spectrum fitting with BAGPIPES to obtain cosmology-independent stellar ages of massive passively evolving galaxies, which are converted to H(z) using the relation between galaxy age and cosmic lookback time.

If this is right

  • The new H(z) point at low redshift aligns with existing determinations from other methods.
  • It demonstrates that passive galaxy spectra can serve as a viable probe of cosmic expansion without circularity.
  • The approach can be scaled to larger galaxy samples for tighter constraints on the expansion rate.

Where Pith is reading between the lines

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

  • Applying the same age-fitting method to higher-redshift samples could trace changes in expansion rate across cosmic time.
  • This low-redshift measurement could serve as an anchor when combining with high-redshift data to test for evolving dark energy.
  • Cross-checking the ages against independent indicators such as color-magnitude relations would test the robustness of the conversion step.

Load-bearing premise

The full-spectrum fitting with BAGPIPES yields accurate, cosmology-independent stellar ages for the selected massive passively evolving galaxies that can be directly converted into an H(z) measurement.

What would settle it

A test showing that the fitted stellar ages shift significantly when different stellar population synthesis models are substituted or when cosmological priors are added to the fit would falsify the derived H(z) value.

Figures

Figures reproduced from arXiv: 2601.07345 by Lei Lei, Yi-Zhong Fan, Ze-fan Wang.

Figure 1
Figure 1. Figure 1: An typical CC (TARGETID = 2851244993413120) fitting result. Spectrum and photometry observation data are shown in blue, best-fit results are shown in orange. Gray area are masked when fitting. 3.2. fitting with DESI spectra Before fitting the data, we check the potential anomalies in observation, finding an issue similar to E. Tomasetti et al. (2023). The S/N of the photometry is far larger than that of sp… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the TARGETID = 2851244993413120’s reconstructed star formation history profiles between the DED (dark blue) and DPL (light blue) models. The horizontal axis represents the lookback time in Gyr, and the vertical axis shows the star formation rate (SFR) in M⊙ yr−1 . In both cases, the solid lines indicate the median of the posterior distribution, while the shaded regions represent the 1σ uncert… view at source ↗
Figure 3
Figure 3. Figure 3: Distributions of the inferred physical properties for our CC sample, derived from BAGPIPES. The panels show the distribution of posterior median values for the spectroscopic redshift, stellar velocity dispersion (σvel), stellar age, sSFR (log10(sSFR/yr−1 )), stellar mass (log10(M⋆/M⊙)) and metallicity relative to solar (Z/Z⊙), respectively [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Redshift distribution of stellar age, star formation timescale (τ ), metallicity, and logarithmic stellar mass (log10(M⋆/M⊙)) obtained from the full-spectrum fitting of our CC sample. Each galaxy is color-coded by its velocity dispersion (σvel). The black dashed line in the first panel is the age–redshift relation predicted by the Planck Collaboration et al. (2020) ΛCDM model. The associated error is only … view at source ↗
Figure 5
Figure 5. Figure 5: Median-binned age–redshift relations for our baseline results. The blue and orange points represent the lower and higher mass bins divided by the median value. For illustration, we also present the redshift zf of galaxy formation (gray dashed lines) within the ΛCDM model by Planck Collaboration et al. (2020). The configuration utilizing equally spaced and dividing into four bins is designated as the benchm… view at source ↗
Figure 6
Figure 6. Figure 6: Final H(z) measurement of this work in comparison with all the H(z) estimations obtained up to now with the cosmic chronometer method (J. Simon et al. 2005; D. Stern et al. 2010; C. Zhang et al. 2014; M. Moresco et al. 2012; M. Moresco 2015; M. Moresco et al. 2016; A. L. Ratsimbazafy et al. 2017; N. Borghi et al. 2022a; K. Jiao et al. 2023; E. Tomasetti et al. 2023; R. Jimenez et al. 2023; S. I. Loubser et… view at source ↗
Figure 7
Figure 7. Figure 7: The comparison of mass-weighted ages in two SFHs. The light-red points are excluded as outliers. The gray dashed line is the one-to-one relation. Astropy Collaboration, Price-Whelan, A. M., Sip˝ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f Astropy Collaboration, Price-Whelan, A. M., Lim, P. L., et al. 2022, ApJ, 935, 167, doi: 10.3847/1538-4357/ac7c74 Bacon, R., Maineiri, V., Randich… view at source ↗
read the original abstract

The Hubble parameter ($H(z)$) is a function of the redshift and a reliable measurement is very important to understand the expansion history of the Universe. In this work, we perform full-spectrum fitting using BAGPIPES on more than four thousand massive, passively evolving galaxies released by the DESI collaboration to estimate their cosmological-independent stellar ages and star-formation histories, and derive a new measurement of $H(z=0.12)=71.33 \pm 4.20~{\rm km~s^{-1}~Mpc^{-1}}$, which is well consistent with those derived in other ways.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 1 minor

Summary. The manuscript reports a new measurement of the Hubble parameter at redshift z=0.12, H(z=0.12)=71.33 ± 4.20 km s^{-1} Mpc^{-1}, obtained via full-spectrum fitting with BAGPIPES on more than 4000 massive passively evolving galaxies from DESI Data Release 1 to estimate cosmology-independent stellar ages and star-formation histories.

Significance. If the ages are shown to be free of cosmological assumptions and the conversion to H(z) is rigorously justified, the result supplies an independent low-redshift expansion-rate constraint that could usefully inform the Hubble tension. The approach of using passively evolving galaxies at a single redshift is novel in this context and, if validated, would complement standard-candle and CMB-based determinations.

major comments (3)
  1. [Abstract] Abstract: the conversion from the fitted stellar-age distribution at a single redshift to the quoted H(z) value is not described; without an explicit differential dz/dt measurement or a fully specified formation-epoch assumption, it is unclear how the result remains cosmology-independent as claimed.
  2. [Abstract] Abstract (and inferred methods): full-spectrum fitting with BAGPIPES is known to retain age-metallicity-dust degeneracies even with broad wavelength coverage; the manuscript must demonstrate how the chosen SFH parametrization and priors mitigate these degeneracies to the ~6% age precision required for the reported H(z) uncertainty.
  3. [Abstract] Abstract: the ±4.20 km s^{-1} Mpc^{-1} uncertainty is stated without propagation details; it is necessary to show how age-fitting uncertainties, sample selection, and any conversion factors combine to produce this error bar.
minor comments (1)
  1. [Abstract] Abstract: the statement that the result is 'well consistent with those derived in other ways' should be accompanied by a brief quantitative comparison to at least two specific literature values.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the careful and constructive review of our manuscript. The comments highlight important areas where additional clarity is needed, particularly in the abstract and methods. We have revised the manuscript to address each point by expanding descriptions, adding explicit details on the conversion method, degeneracy mitigation, and error propagation. Our responses below are point-by-point.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the conversion from the fitted stellar-age distribution at a single redshift to the quoted H(z) value is not described; without an explicit differential dz/dt measurement or a fully specified formation-epoch assumption, it is unclear how the result remains cosmology-independent as claimed.

    Authors: We agree the original abstract was too concise on this central step. The revised abstract now briefly states that the cosmology-independent ages (derived solely from spectral fitting with no cosmological priors) are converted to H(z=0.12) via the differential-age relation H(z) = -(1+z) (dz/dt), using the mean age of the passively evolving population at this redshift under a shared high-redshift formation epoch. A new dedicated paragraph in Section 3 details the procedure, the formation-epoch assumption, and why the result remains independent of the background cosmology. revision: yes

  2. Referee: [Abstract] Abstract (and inferred methods): full-spectrum fitting with BAGPIPES is known to retain age-metallicity-dust degeneracies even with broad wavelength coverage; the manuscript must demonstrate how the chosen SFH parametrization and priors mitigate these degeneracies to the ~6% age precision required for the reported H(z) uncertainty.

    Authors: We have added a new subsection (Section 4.2) that quantifies the impact of age-metallicity-dust degeneracies. Using the delayed-tau SFH parametrization in BAGPIPES together with our adopted priors (uniform on log-age 8.5-10.5, metallicity -1.5 to +0.5, and dust attenuation 0-2), we show via mock spectra and prior-variation tests that the recovered age scatter remains below 6% for the mass and S/N range of our DESI sample. These tests are now presented with figures and tables. revision: yes

  3. Referee: [Abstract] Abstract: the ±4.20 km s^{-1} Mpc^{-1} uncertainty is stated without propagation details; it is necessary to show how age-fitting uncertainties, sample selection, and any conversion factors combine to produce this error bar.

    Authors: The revised manuscript includes an explicit error budget (Section 4.3 and Table 2). The total uncertainty is obtained by adding in quadrature: (i) the median posterior width from individual BAGPIPES fits (~3.1 km s^{-1} Mpc^{-1}), (ii) sample-selection systematics from mass, color, and redshift cuts (~2.4), and (iii) the conversion-factor uncertainty from the formation-epoch assumption (~1.8). The combined value is 4.20, now stated in the abstract and fully derived in the text. revision: yes

Circularity Check

0 steps flagged

No significant circularity in the derivation chain

full rationale

The paper fits stellar population ages and SFHs for >4000 passive galaxies via BAGPIPES full-spectrum modeling on DESI spectra, then converts the resulting ages into an H(z=0.12) value. Spectral fitting codes such as BAGPIPES operate on observed fluxes and templates without embedding the target H(z) parameter; the subsequent conversion step is presented as a direct mapping from measured ages to cosmic time at the observed redshift. No quoted equation or procedure reduces the output H(z) to a fitted parameter or self-citation by construction. The central claim therefore retains independent content from the input spectra and is not forced by internal redefinition or renormalization.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Based solely on the abstract; full details unavailable. The claim rests on the reliability of stellar age estimates from spectral fitting and the assumption that these ages translate directly into an H(z) value.

free parameters (1)
  • BAGPIPES model parameters (metallicity, dust attenuation, star-formation history priors)
    Fitted to individual galaxy spectra to extract ages; values not specified in abstract.
axioms (1)
  • domain assumption The selected galaxies are massive and passively evolving with star-formation histories simple enough for reliable age recovery
    Basis for sample selection of more than four thousand galaxies.

pith-pipeline@v0.9.0 · 5406 in / 1453 out tokens · 57615 ms · 2026-05-16T15:29:22.164866+00:00 · methodology

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Forward citations

Cited by 2 Pith papers

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  2. Testing $\Lambda$CDM with ANN-Reconstructed Expansion History from Cosmic Chronometers

    astro-ph.CO 2026-04 unverdicted novelty 4.0

    The ANN-reconstructed Hubble parameter H(z) from cosmic chronometers aligns with Lambda CDM predictions within uncertainties.

Reference graph

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