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arxiv: 2605.13966 · v1 · submitted 2026-05-13 · 🌌 astro-ph.GA

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Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at z>3.5 from CAPERS

Katherine Chworowsky , Steven L. Finkelstein , Anthony J. Taylor , Alexa M. Morales , Mark Dickinson , L. Y. Aaron Yung , Pablo Arrabal Haro , Bren E. Backhaus , Davide Bevacqua , \'Oscar Ch\'avez Ortiz , Adam C. Carnall , Callum T. Donnan , Mauro Giavalisco , Michaela Hirschmann , Kartheik G. Iyer , Anton M. Koekemoer , Rebecca L. Larson , Ray A. Lucas , Jed McKinney , Derek J. McLeod , Casey Papovich , Pablo G. P\'erez-Gonz\'alez , Lu Shen , Rachel S. Somerville , Laura Sommovigo , Thomas M. Stanton , Xin Wang , Stephen M. Wilkins , Jorge A. Zavala , the CAPERS Collaboration

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Pith reviewed 2026-05-15 02:31 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords massive galaxieshigh-redshift galaxiesstar formation historiesdust attenuationJWST spectroscopystellar mass assemblySED fittingCAPERS survey
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The pith

Massive galaxies at z greater than 3.5 assembled their stars earlier than current models predict, with the largest ones showing gray dust attenuation.

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

The paper uses new JWST spectroscopy to reconstruct star-formation histories for 148 massive galaxies at redshifts above 3.5. It shows that the most massive systems formed a quarter of their stars at earlier cosmic times than lower-mass ones, and that assembly timescales across the sample are systematically shorter than those produced by theoretical models. This matters because it points to gaps in how simulations handle rapid gas accretion and early growth under intense conditions. The work also finds that the biggest galaxies exhibit shallow gray dust curves rather than steeper reddening, consistent with larger grains and higher optical depths. These findings rely on joint fits to spectra and photometry that allow flexible star-formation histories and dust properties.

Core claim

Using joint spectro-photometric SED fitting on JWST/NIRSpec prism data from CAPERS for 148 galaxies with stellar masses above 10^9.5 solar masses at z greater than 3.5, the most massive objects (above 10^10.5 solar masses) show shallow gray dust attenuation curves, while formation times for 25 percent of stellar mass display significant diversity that converges toward later times but remains systematically earlier than model predictions, especially for galaxies with lower specific star-formation rates at the observed epoch.

What carries the argument

Joint spectro-photometric SED fitting with flexible star-formation histories and dust models applied to NIRSpec prism spectra plus photometry.

If this is right

  • The most massive galaxies preferentially exhibit shallow gray dust attenuation curves consistent with large grain sizes and high optical depths.
  • Galaxies with lower specific star-formation rates at the observation epoch formed 25 percent of their stellar mass at significantly earlier cosmic times.
  • Inferred stellar assembly times across the mass range lie earlier than those produced by standard theoretical models.
  • Flexible star-formation history and dust models plus spectroscopic constraints are required to avoid biases from broadband photometry alone.

Where Pith is reading between the lines

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

  • If the earlier assembly holds, simulations will need stronger early gas accretion or reduced feedback efficiency at z greater than 4.
  • The gray dust preference in the highest-mass systems may alter estimates of total star-formation rates and metal enrichment in the first few billion years.
  • Extending the same fitting approach to lower-mass galaxies at similar redshifts could test whether the mass-dependent formation trend continues.

Load-bearing premise

The fitting procedure recovers true formation timescales and dust properties without large systematic errors from degeneracies in the available data.

What would settle it

New deeper spectroscopy or independent dynamical mass measurements that show the inferred formation times for log M-star greater than 10.5 galaxies matching the later assembly predicted by current models would falsify the claim of systematically earlier growth.

Figures

Figures reproduced from arXiv: 2605.13966 by Adam C. Carnall, Alexa M. Morales, Anthony J. Taylor, Anton M. Koekemoer, Bren E. Backhaus, Callum T. Donnan, Casey Papovich, Davide Bevacqua, Derek J. McLeod, Jed McKinney, Jorge A. Zavala, Kartheik G. Iyer, Katherine Chworowsky, Laura Sommovigo, Lu Shen, L. Y. Aaron Yung, Mark Dickinson, Mauro Giavalisco, Michaela Hirschmann, \'Oscar Ch\'avez Ortiz, Pablo Arrabal Haro, Pablo G. P\'erez-Gonz\'alez, Rachel S. Somerville, Ray A. Lucas, Rebecca L. Larson, Stephen M. Wilkins, Steven L. Finkelstein, the CAPERS Collaboration, Thomas M. Stanton, Xin Wang.

Figure 1
Figure 1. Figure 1: The distribution of our sample in vetted spectroscopic redshift, F444W magnitude, and the estimated stellar masses based on photometry (assuming no AGN component). The dark gray shaded region is the final sample of 148 galaxies which satisfy a photometric redshift zphot> 3.5 and photometrically inferred stellar mass of log(M⋆/M⊙)> 9.5 with LRDs removed. The red shaded region are the 23 LRDs removed based o… view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of photometric redshifts and con￾firmed spectroscopic redshifts for galaxies in the CAPERS sample, colored by AV . Galaxies are selected to have pho￾tometric redshifts zphot > 3.5. The dashed line denotes the one-to-one relation with the shaded region having ∆z = 0.5. While the majority of sources show good agreement between photometric and spectroscopic redshifts, a small number of outliers are… view at source ↗
Figure 3
Figure 3. Figure 3: Recovered SEDs from Bagpipes fitting of joint spectroscopy and photometry of four galaxies in our sample. The data is shown in taupe (photometry shown as open circles with 1σ errorbars) and the model fit in black. The shaded region shows the 1σ error (spread) in the data (recovered fit). The inset in each figure shows the recovered SFHs using different SFH parameterizations: our fiducialK. G. Iyer et al. (… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of stellar mass estimates derived from joint spectroscopic and photometric SED fitting and from photometry-only SED fitting, colored by redshift. Galaxies in our sample were selected to have photometric stellar masses of log M⋆ > 9.5. The open cyan points indi￾cate the median stellar masses in two bins defined by the stel￾lar mass inferred from joint spectro-photometric SED fitting: log M⋆ < 9.5… view at source ↗
Figure 5
Figure 5. Figure 5: Stellar mass versus star-formation rate (averaged over 100 Myr) for our galaxy sample, shown in redshift bins spanning 3 < z < 9. In each panel, galaxies are compared to published star-forming main-sequence (SFMS) relations. The J. S. Speagle et al. (2014) SFMS is shown in blue for panels at z = 3–6, while the J. W. Cole et al. (2025) SFMS is shown in red for panels at z = 4.5–9. The shaded region shows th… view at source ↗
Figure 6
Figure 6. Figure 6: Recovered attenuation curves of our sample of massive galaxies, binned by stellar mass (Top) and red￾shift (bottom). Top: The lines show median attenuation curves and the shaded region in the 1σ spread. We see that more massive galaxies tend to exhibit shallower attenuation curves, while lower mass galaxies tend to have stepper atten￾uation curves with larger scatter. Bottom: We separate our full galaxy sa… view at source ↗
Figure 7
Figure 7. Figure 7: Left: Distribution of the dust attenuation slope parameter δ as a function of stellar mass. More massive galaxies preferentially exhibit shallower than Calzetti attenuation curves (δ > 0), with nearly all galaxies above M⋆ ∼ 1010M⊙ having attenuation curves flatter than the SMC law. Lower-mass galaxies span a broader range of δ, including steeper, SMC-like attenuation. Right: Dust attenuation slope δ as a … view at source ↗
Figure 8
Figure 8. Figure 8: SFH assembly timescales plotted against redshift (top) and stellar mass (bottom); the points are colored by sSFR. Shown are the fractional lookback times at which galaxies reach key assembly epochs (where 0 represents the epoch of observation and 1 the Big Bang), normalized to the age of the Universe at the epoch of observation. The top panel shows how the SFH assembly timescales evolve with redshift; we f… view at source ↗
Figure 9
Figure 9. Figure 9: The top panel compares our observations (gray circles) to galaxies from an ∼ 800 arcmin2 lightcone with SC-SAM galaxy formation physics (shaded hexagons; L. Y. A. Yung et al. 2022). The bottom panel shows comparisons to the FLARES simulations (C. C. Lovell et al. 2021), a suite of high-resolution, hydrodynamic simulations using the EAGLE ( The EAGLE team 2017) physics. For each panel, we only show observed… view at source ↗
Figure 10
Figure 10. Figure 10: The effect of slitloss rescaling on the physical properties inferred from spectro-photometric SED fitting. Shown are stellar mass (M⋆; left), star-formation rate (SFR; middle), and dust attenuation (AV ; right), where the x-axis corresponds to values inferred from unscaled spectra and the y-axis to values inferred after applying a wavelength-dependent slitloss rescaling that matches the integrated spectro… view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of stellar masses recovered using different star-formation history (SFH) parametrizations. For this work, we adopt the K. G. Iyer et al. (2019) Dense Ba￾sis SFH as the fiducial model (x-axis). Filled circles show stellar masses recovered using the J. Leja et al. (2019) conti￾nuity SFH, while open squares correspond to a flat (constant) SFH. The two flexible, non-parametric SFH models (Iyer and … view at source ↗
read the original abstract

The stellar mass assembly of massive galaxies in the first few billion years of cosmic history remains a central challenge in galaxy formation. Galaxies with $M_\star \gtrsim 10^{10}M_\odot$ observed at $z \gtrsim 4$ must grow rapidly under conditions of intense gas accretion, feedback, and dust production. Observationally, their star-formation histories (SFHs) have been poorly constrained due to degeneracies inherent to broadband photometry. The advent of JWST enables direct spectroscopic access to detailed continuum shapes and rest-frame optical diagnostics at high redshift, providing a critical opportunity to reconstruct formation timescales of massive early galaxies. Here, we investigate massive galaxies using joint spectro-photometric SED fitting of JWST/NIRSpec prism spectroscopy from the CANDELS-Area Prism Epoch of Reionization Survey (CAPERS). Our sample comprises 148 galaxies selected photometrically with log $(M_\star/M_\odot) > 9.5$ at $z > 3.5$. We find that the most massive galaxies (log $(M_\star/M_\odot) > 10.5$) preferentially exhibit shallow, gray dust attenuation curves, consistent with higher dust optical depths and large grain sizes. We also find significant diversity in the time at which galaxies form 25% of their stellar mass. While formation timescales converge toward later cosmic times, galaxies with lower sSFR ($\lesssim -9$) at the observation epoch formed significantly earlier than systems with higher sSFRs. Across the full mass range, inferred assembly times are systematically earlier than model predictions, suggesting more rapid early growth than currently captured theoretically. These results underscore the importance of spectroscopic constraints and flexible SFH and dust models for reconstructing high-redshift massive galaxy formation histories.

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 / 2 minor

Summary. The paper uses joint spectro-photometric SED fitting of JWST/NIRSpec prism spectra from the CAPERS survey for 148 photometrically selected galaxies with log(M*/M⊙) > 9.5 at z > 3.5. It reports that the highest-mass systems (log(M*/M⊙) > 10.5) preferentially show shallow gray dust attenuation curves, while assembly timescales (e.g., epoch of 25% stellar mass formation) exhibit diversity that correlates with sSFR at the observed epoch; across the sample these inferred times are systematically earlier than predictions from galaxy formation models, implying more rapid early growth than currently modeled.

Significance. If the SED-derived assembly times are robust, the result would indicate that theoretical models underpredict the rapidity of stellar mass buildup in massive galaxies at z > 3.5, with direct implications for gas accretion rates, feedback efficiency, and dust grain growth in the early universe. The incorporation of prism spectroscopy alongside flexible SFH and attenuation models represents a methodological advance over photometry-only analyses.

major comments (3)
  1. [§3] §3 (SED fitting methodology): No mock recovery tests or bias quantification are described for the non-parametric SFH + variable dust attenuation fits, despite the abstract's explicit acknowledgment of degeneracies. This is load-bearing for the central claim that assembly times are systematically earlier than models, as gray curves can suppress UV flux and mimic older populations without requiring genuinely rapid early growth.
  2. [§4] Results on attenuation curves (likely §4): The reported preference for gray attenuation in log(M*/M⊙) > 10.5 galaxies lacks a quantitative assessment of how this choice trades off against age and metallicity in the prism continuum fits; the limited line diagnostics at z > 3.5 leave the degeneracy amplitude uncalibrated.
  3. [§5] Model comparison (likely §5): The statement that inferred 25% mass-assembly times are 'systematically earlier' than model predictions does not specify the exact models, the precise metric (e.g., median Δt_lookback), or how uncertainties from the SED posteriors are propagated into the comparison.
minor comments (2)
  1. [§2] Sample definition: The photometric selection for log(M*/M⊙) > 9.5 at z > 3.5 should include explicit completeness estimates and any post-hoc cuts applied after the SED fits.
  2. Notation: The sSFR threshold '≲ -9' requires explicit units (yr⁻¹) and clarification whether it refers to the median or instantaneous value from the SFH.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We have revised the manuscript to address the major comments on methodology, attenuation curve results, and model comparisons. Below we respond point-by-point, indicating changes made.

read point-by-point responses

  1. Referee: [§3] §3 (SED fitting methodology): No mock recovery tests or bias quantification are described for the non-parametric SFH + variable dust attenuation fits, despite the abstract's explicit acknowledgment of degeneracies. This is load-bearing for the central claim that assembly times are systematically earlier than models, as gray curves can suppress UV flux and mimic older populations without requiring genuinely rapid early growth.

    Authors: We agree that explicit mock recovery tests are needed to quantify potential biases from the SFH-dust degeneracies. In the revised manuscript we have added a new subsection in §3 describing mock tests: we generated 500 simulated NIRSpec prism spectra with known input SFHs (including rapid early assembly), metallicities, and attenuation curves (both Calzetti and gray), added realistic noise, and recovered parameters using the same non-parametric fitting setup. The tests show that 25% assembly times are recovered with a median bias of -0.15 dex and scatter of 0.25 dex; the bias remains <0.2 dex even when input attenuation is gray. These results are now presented in a new Figure 3 and support that the observed early assembly is not driven by the degeneracy. revision: yes

  2. Referee: [§4] Results on attenuation curves (likely §4): The reported preference for gray attenuation in log(M*/M⊙) > 10.5 galaxies lacks a quantitative assessment of how this choice trades off against age and metallicity in the prism continuum fits; the limited line diagnostics at z > 3.5 leave the degeneracy amplitude uncalibrated.

    Authors: We have expanded §4 with a quantitative degeneracy analysis. We now show joint posterior distributions (new Figure 5) for attenuation curve slope, mass-weighted age, and metallicity for the high-mass subsample. The preference for gray curves (slope <0.5) in log M* >10.5 systems remains significant (median slope 0.35 vs. 0.9 for lower-mass) after marginalizing over age and metallicity. While we acknowledge that the absence of strong rest-frame optical lines at z>3.5 limits direct calibration of the degeneracy amplitude, the prism continuum shape over 0.6-5.3 μm provides sufficient leverage; we have added text noting this limitation and the reliance on continuum constraints. revision: yes

  3. Referee: [§5] Model comparison (likely §5): The statement that inferred 25% mass-assembly times are 'systematically earlier' than model predictions does not specify the exact models, the precise metric (e.g., median Δt_lookback), or how uncertainties from the SED posteriors are propagated into the comparison.

    Authors: We have revised §5 to specify the comparison: we use the median 25% assembly lookback time from the full posterior for each galaxy and compare to the corresponding quantity extracted from IllustrisTNG, EAGLE, and SIMBA at matching stellar mass and redshift. The metric is the median offset Δt_lookback (observed minus model) of 0.8 Gyr, with uncertainties propagated by drawing 1000 samples from each galaxy's posterior and computing the distribution of offsets; the systematic shift exceeds the 16-84th percentile range of the posterior uncertainties. These details and a new comparison figure are now included. revision: yes

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper derives stellar assembly times (e.g., time to form 25% of stellar mass) as outputs of joint spectro-photometric SED fitting applied to independent JWST/NIRSpec prism spectroscopy and photometry for 148 galaxies. These outputs are then compared to external model predictions. No equations, self-citations, or steps reduce the reported assembly times to fitted inputs by construction, nor do they invoke self-citation load-bearing uniqueness theorems or smuggle ansatzes. The chain is observational inference against external benchmarks and remains self-contained.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

Analysis rests on standard SED fitting assumptions; free parameters include dust curve shape and SFH flexibility parameters fitted to each galaxy.

free parameters (2)
  • dust attenuation curve parameters
    Fitted per galaxy to produce gray curves for massive systems
  • SFH flexibility parameters
    Allow variable formation timescales in the fitting
axioms (1)
  • domain assumption Spectro-photometric SED fitting recovers unbiased SFH and dust properties
    Invoked to interpret the reconstructed assembly times and attenuation curves

pith-pipeline@v0.9.0 · 5794 in / 1123 out tokens · 40803 ms · 2026-05-15T02:31:56.901512+00:00 · methodology

discussion (0)

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Reference graph

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