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Even redder than we knew: color and $A_{\mathrm{V}}$ evolution up to $z=2.5$ from JWST/NIRCam photometry

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read JWST/NIRCam photometry shows that massive star-forming galaxies at z≈2 are far dustier than earlier surveys indicated, with V-J colors past 2.5 and visual extinction up to 3.5 magnitudes.

desk verdict A solid, transparent demonstration that massive star-forming galaxies at z~2 are much redder and more dust-attenuated than previously thought, with the main caveat being the small spectroscopic validation sample for the reddest objects. read the letter →

arxiv 2506.23669 v2 pith:EYD4XX6N submitted 2025-06-30 astro-ph.GA

A. van der Wel , M. Martorano , D. Marchesini , S. Wuyts , E.F. Bell , S.E. Meidt , A. Gebek , G. Brammer
show 9 more authors
K. Whitaker R. Bezanson E.J. Nelson G. Rudnick M. Kriek J. Leja J.S. Dunlop C. Casey J. Kartaltepe
This is my paper · ORCID
classification astro-ph.GA
keywords galaxyevolutiondustattenuationrest-framecolorsV-JcolorJWSTNIRCamphotometryphotometricredshiftsstar-forminggalaxiesmassive
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper shows that the rest-frame $V-J$ color — the difference in brightness between the optical $V$ band and the near-infrared $J$ band — of star-forming galaxies evolves strongly with cosmic time. Massive galaxies ($M_\star > 3\times10^{10}\,M_\odot$) at redshift $z>1.5$ develop a tail of very red objects reaching $V-J>2.5$ that has no counterpart at $z<1$, and the paper interprets these colors as dust attenuation, with visual extinction $A_{\mathrm{V}}$ between 1.5 and 3.5 magnitudes for $M_\star\approx10^{11}\,M_\odot$ galaxies at $z\approx2$. Earlier surveys missed this evolution, the paper argues, because their photometric redshifts for exactly these reddest, most attenuated galaxies were biased; JWST/NIRCam photometry removes the bias. If the claim is right, the dust content of massive high-redshift galaxies has been systematically underestimated, and their stellar masses and star-formation rates need to be rethought.

What carries the argument

The central machinery is the rest-frame $V-J$ color, the difference between rest-frame $V$-band and $J$-band magnitudes, measured from JWST/NIRCam photometry combined with HST imaging. In the $U-V$ versus $V-J$ diagram, dusty star-forming galaxies are red in $V-J$ while quiescent galaxies are blue in $V-J$, so this color separates attenuation by dust from the reddening caused by old stellar populations. The measurement works because NIRCam provides rest-frame near-infrared coverage up to $z\approx2.5$, and because the precise photometry removes the systematic redshift overestimates that previously pushed the reddest galaxies to the wrong distances and washed out the tail.

What would settle it

A spectroscopic redshift survey of galaxies with $V-J>2.5$ at $z\approx1.5$–$2.5$ would settle the claim: if the new photometric redshifts show the same roughly 0.4 overestimate seen in earlier catalogs, the red tail and the inferred rise in $A_{\mathrm{V}}$ would largely disappear.

Watch

Extended reading notes

Core claim

The central discovery is that the rest-frame $V-J$ versus stellar mass relation for star-forming galaxies becomes very steep at $z>1.5$, with high-mass galaxies ($M_\star > 3\times10^{10}\,M_\odot$) reaching $V-J\approx2$–$3$, while the same galaxies at $z<1$ have $V-J\approx1$–$1.5$. The reddest colors cannot be produced by old stellar populations, so they must come from dust; spectral-energy-distribution fitting gives $A_{\mathrm{V}}\approx1.5$–$3.5$ for $M_\star\approx10^{11}\,M_\odot$ at $z\approx2$, with about 90% of such galaxies having $A_{\mathrm{V}}>2$ at $z>1.5$. The paper attributes the previously unseen evolution to improved photometric redshifts for the reddest galaxies: for 25 galaxies with spectroscopic redshifts and $V-J>2.5$, the new median photometric redshift matches the spectroscopic median, whereas the older catalog overestimated it by about 0.4. The $U-V$ colors of these galaxies stay relatively blue, so the attenuation must be gray in the ultraviolet-optical, consistent with attenuation of most stars younger than about one gigayear rather than only the youngest star-forming regions.

Load-bearing premise

The result depends on the assumption that the photometric redshifts for the reddest, most dust-obscured galaxies are now correct, and the paper's own check of this assumption uses only 25 spectroscopic redshifts.

Editorial extensions

If this is right

  • At $0.5<z<2.5$ the rest-frame $U-V$ color distribution evolves only mildly, so the familiar UV-optical red sequence and blue cloud hide a strong optical-to-near-infrared evolution that only $V-J$ reveals.
  • Nearly all star-forming galaxies with $M_\star>10^{11}\,M_\odot$ at $z>1.5$ have $A_{\mathrm{V}}>2$, so these systems should be treated as heavily dust-obscured rather than moderately reddened.
  • Older photometric-redshift catalogs systematically misplaced the reddest galaxies toward higher redshift, so samples built from them need to be re-derived or re-calibrated for these objects.
  • The red $V-J$ tail of the mass-selected sample overlaps with the ALMA sub-mm selected population, indicating that the NIRCam colors and the sub-mm detections trace the same obscured star-forming galaxies.
  • Because $U-V$ remains relatively blue at high attenuation, using $U-V$ alone to infer dust content or to classify galaxies as quiescent will misclassify massive dusty galaxies.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the redshift improvement turns out to come from better templates rather than better photometry, the same correction could be applied to existing HST-only catalogs, shifting their color distributions without new observations.
  • If dust attenuation rises this steeply with redshift, the peak may lie beyond $z=2.5$, making the $z>1.5$ tail described here the low-redshift edge of the optically dark, dust-obscured population found at $z\gtrsim3$.
  • A direct test of the gray-attenuation interpretation would compare NIRCam-based $A_{\mathrm{V}}$ with independently measured far-infrared or millimeter dust luminosities for the same individual galaxies.
  • The steep mass dependence of $A_{\mathrm{V}}$ suggests that gas fraction and dust geometry, rather than metallicity, set the dust column; galaxy formation models that reproduce this $A_{\mathrm{V}}$–mass–redshift relation would be needed to explain the heavy obscuration of massive galaxies at $z\approx2$.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This paper uses JWST/NIRCam photometry from the DAWN JWST Archive to construct a stellar-mass-complete sample of about 28,000 galaxies with M* > 10^9 M_sun in the redshift range 0.5 < z < 2.5, and studies the evolution of rest-frame U-V and V-J colors and the dust attenuation parameter A_V. The central claim is that the V-J color distribution of star-forming galaxies evolves strongly with redshift: massive galaxies (M* > 3e10 M_sun) at z > 1.5 exhibit a pronounced tail reaching V-J > 2.5, which is absent at z < 1, and this tail is interpreted as arising from dust attenuation with A_V in the range 1.5-3.5 for M* ~ 1e11 M_sun at z ~ 2. The authors attribute the previous lack of detection of this population to overestimated photometric redshifts for the reddest objects in earlier catalogs, and support their interpretation with a comparison to 25 spectroscopic redshifts and with cross-matching to sub-mm selected galaxies. A check with an independent SED-fitting code (bagpipes) is presented for the A_V values of the reddest subsample.

Significance. If the central claim holds, this is an important result: it would mean that massive star-forming galaxies at cosmic noon are significantly more dust-attenuated than previously inferred from rest-frame optical colors, with A_V values extending to 3-4, and that earlier ground- and space-based surveys systematically underestimated this population because of photo-z biases. The paper is concise, uses high-quality public JWST data, and makes a falsifiable prediction that a comprehensive spectroscopic survey of high-A_V galaxies at z > 1 should confirm the high attenuation. The independent bagpipes check for the reddest galaxies and the sub-mm cross-match are notable strengths. However, the central claim rests on the reliability of photometric redshifts for a small and extreme subset of the sample, and the current validation sample is too small to fully secure that footing.

major comments (3)
  1. [Section 3.1, photo-z validation paragraph] The claim that the red V-J tail at z > 1.5 is real and was previously missed because of photo-z biases rests on the comparison with only 25 spectroscopic redshifts for galaxies with V-J > 2.5. This is a very small sample on which to base a strong evolutionary claim, and the paper itself notes that it remains undetermined whether the improvement comes from better photometry or better templates. The authors should quantify the impact of plausible photo-z errors on the inferred color distributions, for example by applying the old 3D-HST photo-z error distribution to the current sample and showing how the V-J tail and the z=1.5 boundary would shift. They should also report how many galaxies in the final sample have V-J > 2.5 in each redshift bin, and how many of those have spectroscopic redshifts, so that the reader can judge the statistical weight of the 25-object validation.
  2. [Section 3.1 and Figure 1] The statement that the red tail 'does not exist at z < 1' is based on running medians (shown as solid lines) and the visual appearance of the scatter plots, without any confidence intervals or counts of the tail population. Given that the running median is not sensitive to the existence of a tail and the reddest objects are sparse, the authors should provide a quantitative characterization of the tail—for example, the fraction of massive star-forming galaxies with V-J > 2.5 (or > 2.0) as a function of redshift, with bootstrap uncertainties. Without such a statistic, the absence of the tail at low redshift is not demonstrated to be significant.
  3. [Section 3.2, A_V evolution] The A_V values and the V-J colors are both outputs of the same EAZY SED fits, so the correlation between V-J and A_V used to interpret the red tail is partly built into the model. The bagpipes check is welcome, but it is applied only to the V-J > 2.5 subsample, leaving the redshift evolution of A_V for the full star-forming population untested in an independent way. The authors should either run bagpipes on a representative subsample spanning the full mass-redshift range, or explicitly state that the A_V evolution is a model-dependent inference whose robustness has only been verified for the extreme tail.
minor comments (4)
  1. [Abstract and Section 3.1] The sentence 'the photometric redshift estimates for the reddest... has markedly improved' contains a subject-verb agreement error; 'estimates' is plural and should take 'have'. The same issue appears in the abstract.
  2. [Section 2] The phrase 'These data product derive' should be 'These data products derive'.
  3. [Figure 2] The color bar on the right side of the figure is labeled 'Log(M/M_sun)' but it is not immediately clear that this color coding applies to the plotted points; please clarify in the caption.
  4. [Section 1, footnote 1] The footnote on the origin of the term 'quenching' is interesting but tangential; consider moving it to the main text or removing it, as it interrupts the flow of the introduction.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the reported colors and AV values are SED-fit outputs, but the central color-evolution claim is independently supported by spec-z, sub-mm, and a separate SED code.

full rationale

The paper is an observational analysis of DJA value-added products, not a first-principles derivation. Rest-frame V-J and AV are both outputs of the same SED-fitting pipeline, so a model-imposed correlation is conceivable; however, the paper does not define one in terms of the other or fit a parameter and then rename it as a prediction. The V-J redshift evolution is validated against 25 spectroscopic redshifts, the reddest objects overlap with ALMA sub-mm detections, and AV for the extreme tail is re-derived with bagpipes, yielding consistent values. The admitted open question of whether improved photo-zs are due to better photometry or better templates is an explicit limitation, not a circular reduction. Self-citations (Martis et al. 2016/2019, Gebek et al. 2025, van der Wel et al. 2014) provide context and prior support rather than load-bearing uniqueness arguments. No equation equates a predicted quantity to a fitted input, so no specific circular step can be exhibited.

Assumptions & free parameters 0 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new physical entities or free parameters. Its conclusions inherit the assumptions of the public SED fitting products, which include the cosmology, IMF, template set, and dust attenuation model. No ad hoc parameters are fitted in this paper itself.

assumptions (4)
  • domain assumption Flat Lambda CDM cosmology with H0 = 70 km/s/Mpc and Omega_m = 0.3.
    Stated in the Introduction/Section 2; used for distance and stellar mass estimates from the DJA catalog.
  • domain assumption Chabrier (2003) initial mass function.
    Stated in Section 2; affects stellar mass estimates.
  • domain assumption The DJA SED templates (agn_blue_sfhz_13) and the dust attenuation model in the EAZY fitting code produce unbiased rest-frame colors, M_star, and A_V for red galaxies.
    The paper relies on these value-added products; the A_V values and rest-frame colors are not measured directly but derived from the SED fitting.
  • domain assumption Quiescent galaxies have V-J < 1.2 in rest-frame, so V-J > 2 necessarily implies dust attenuation.
    Used in Section 3.1 to argue that red V-J colors cannot be explained by old stellar populations alone, citing spectroscopic studies of quiescent galaxies.

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Cite this review

Pith. "Pith review of Even redder than we knew: color and $A_{\mathrm{V}}$ evolution up to $z=2.5$ from JWST/NIRCam photometry." pith.science (2026). https://pith.science/paper/EYD4XX6N

@misc{pith2026250623669,
  author       = {Pith},
  title        = {Pith review of: Even redder than we knew: color and $A_\mathrmV$ evolution up to $z=2.5$ from JWST/NIRCam photometry},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/EYD4XX6N}},
  note         = {Machine review of arXiv:2506.23669}
}
abstract

JWST/NIRCam provides rest-frame near-IR photometry of galaxies up to $z=2.5$ with exquisite depth and accuracy. This affords an unprecedented view of the evolution of the UV-optical-near-IR color distribution and its interpretation in terms of the evolving dust attenuation, $A_{\mathrm{V}}$. We use the value-added data products (photometric redshift, stellar mass, rest-frame $U-V$ and $V-J$ colors, and $A_{\rm V}$) provided by the public DAWN JWST Archive. This data product derives from fitting the spectral energy distributions obtained from multiple NIRCam imaging surveys, augmented with pre-existing HST imaging data. Our sample consists of a stellar mass complete sample of $\approx 28,000$ $M_\star> 10^{9}~M_\odot$ galaxies in the redshift range $0.5<z<2.5$. The $V-J$ color distribution of star-forming galaxies evolves strongly, in particular for high-mass galaxies ($M_\star>3\times 10^{10}~M_\odot$), which have a pronounced tail of very red galaxies reaching $V-J> 2.5$ at $z>1.5$ that does not exist at $z<1$. Such red $V-J$ can only be explained by dust attenuation, with typical values for $M_\star \approx 10^{11}~M_\odot$ galaxies in the range $A_{\mathrm{V}}\approx 1.5-3.5$ at $z\approx 2$. This redshift evolution went largely unnoticed before because the photometric redshift estimates for the reddest ($V-J>2.5$), most attenuated galaxies has markedly improved thanks to the new, precise photometry. Despite the increased attenuation, $U-V$ colors across the entire mass range are slightly bluer at higher $z$. In conclusion, whereas the rest-frame UV-optical color distribution evolves remarkably little from $z=0.5$ to $z=2.5$, the rest-frame optical-near-IR color distribution evolves strongly, primarily due to a very substantial increase with redshift in dust attenuation for massive galaxies. (Abbr.)

Figures

Figures reproduced from arXiv: 2506.23669 by the authors.

Figure 1
Figure 1. Rest-frame U-V (upper panels) and V-J (lower panels) colors versus stellar mass in four redshift bins. Star-forming galaxies are shown in blue; quiescent in red, as separated by their location in the V − J vs. U − V color-color diagram as defined by Muzzin et al. (2013) and shown here in [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Rest-frame U-V vs. V-J diagram in four redshift bins, showcasing the rise of very red galaxies at higher z and indicating the separation between star-forming and quiescent galaxies. match the JWST/NIRSpec spectrum of a z = 4.5 source which is thought to host an obscured AGN (Killi et al. 2024). As input all available HST and JWST imaging datasets were used. For a detailed, field-by-field list we refer to [PITH_FULL… view at source ↗
Figure 3
Figure 3. AV vs. M⋆ for star-forming galaxies in four redshift bins. Points are color-coded with V − J color. White squares show the median in stellar mass bins and errorbars the statistical uncertainty (σ/ √ N, mostly smaller than the data points themselves). The solid black lines show the spline-percentile regression while the dashed lines show the 16-84 percentiles of the distribution. The error bars are the median uncerta… view at source ↗

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Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.