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Unveiling the Dark Side of UV/Optical Bright Galaxies: Optically Thick Dust Absorption

T0 review · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read One-third of massive galaxies at z~3 host optically thick dust substructures that hide 10-20% of their stellar mass and star formation rate.

desk verdict First census of patchy optically thick dust at z~3 with a clean out-of-sample F444W detection, but the mass/SFR fractions are model-dependent and the claimed lower-limit direction is not safe. read the letter →

arxiv 2411.08100 v1 pith:TPQ3QKM5 submitted 2024-11-12 astro-ph.GA

Yingjie Cheng , Mauro Giavalisco , Bren E. Backhaus , Rachana Bhatawdekar , Nikko J. Cleri , Luca Costantin , Emanuele Daddi , Mark Dickinson
show 16 more authors
Steven L. Finkelstein Michaela Hirschmann Benne W. Holwerda Anton M. Koekemoer Ray A. Lucas Fabio Pacucci Pablo G. Pérez-González Giulia Rodighiero Lise-Marie Seillé Katherine E. Whitaker L. Y. Aaron Yung Pablo Arrabal Haro Micaela B. Bagley Jeyhan S. Kartaltepe Casey Papovich Nor Pirzkal
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classification astro-ph.GA
keywords galaxiesopticallythickdarksubstructuresdustmassiveobscured
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 authors searched for galaxies at redshift 2.5 to 3.5 that are bright in UV and optical light but contain small regions where dust is so thick that it completely blocks the starlight behind it. Using JWST's near-infrared camera, they selected 486 massive galaxies from two surveys and fit each galaxy's light with a model, deliberately leaving out the reddest filter (F444W). They then compared the model's prediction for that filter to the actual observed flux. In 162 galaxies (about one-third), the red filter was much brighter than predicted, a sign that hidden regions of dense dust are blocking shorter-wavelength light while letting the red light through.

For those candidate galaxies, the authors subtracted the model image from the observed image to locate the dusty patches, then fit the light of each patch separately. They estimate that these patches contain about 10-20% of the stars and star formation in these galaxies, and that the obscured fraction does not depend strongly on galaxy mass or star formation rate. The patches are often off-center and irregular, and galaxies with a recent burst of star formation in the last 100 million years tend to have more hidden light. The main caveat is that the conversion from extra red light to hidden mass assumes the hidden regions emit like the rest of the galaxy, and any contribution from black holes (AGN) is ignored, so the true numbers could be lower or higher.

Extended reading notes

Core claim

Around one-third of the massive galaxies at z~3 show evidence of optically thick dust obscuration, which segregates on average ~10-20% of the stellar mass and SFR, i.e. they are invisible to UV/optical observations (Section 7). If correct, standard SED-based mass and SFR estimates for massive galaxies at cosmic noon are systematically low by this amount in a third of the population.

Load-bearing premise

The assumption, stated in Section 2 and used in Section 5.1, that the intrinsic spectral shapes of the optically thin and optically thick components are identical. Under this assumption, the F444W excess directly maps to obscured stellar mass and SFR using the same mass-to-light ratio as the rest of the galaxy. If the hidden regions are actually younger (as the burstiness correlation suggests) or contain AGN light, the mass-to-light ratio differs and the quoted 10-20% obscured fractions shift. The paper acknowledges this and calls its estimates lower limits.

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Editorial analysis

A structured set of objections, weighed in public.

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

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central quantitative claim (10-20% obscured mass/SFR in one-third of massive galaxies) rests on a small number of modeling assumptions: identical intrinsic SEDs for thin and thick components, no AGN contribution, a fixed attenuation law, and optically thin F444W. These are not fitted to the target result, but they are unverified and would shift the quoted fractions if wrong. The 15-sigma candidate threshold and the SFH binning are analyst choices that also influence the results.

free parameters (2)
  • Candidate selection threshold in F444W excess = 15 sigma
    Chosen in Section 3.1 and Appendix A; determines the 162-galaxy candidate sample and hence the one-third fraction. A lower threshold would increase the candidate fraction; the paper presents the obscured fractions as lower limits.
  • SFH binning and continuity prior = 7 lookback bins, reduced to 5 for substructures
    Modeling choice in Sections 3.1 and 4.2 that shapes the derived burstiness indices R1 and R2, which feed the starburst correlation claim.
assumptions (5)
  • ad hoc to paper Intrinsic spectral shapes of optically thin and optically thick components are identical
    Stated in Section 2 (last paragraph) and Section 5.1; the conversion of F444W excess into obscured mass and SFR assumes the same mass-to-light ratio in both components.
  • ad hoc to paper The F444W excess is entirely attributed to dust-obscured star formation, not AGN
    Section 5.1 paragraph 2 explicitly neglects obscured AGN emission; Section 5.4 argues against AGN from centroid offsets but cannot fully exclude it.
  • domain assumption Calzetti et al. (2000) attenuation law applies to all galaxies and substructures
    Adopted in Section 3.1; the redshift choice reduces attenuation-law degeneracy in F444W, but the law affects the model prediction of F444W flux.
  • domain assumption F444W-band dust optical depth is less than unity for the searched regions
    Section 2 and Figure 1; this restricts the search to dust that becomes thin in F444W, making the measured obscured fractions lower limits.
  • domain assumption Parent sample selection via EAZY photo-z and stellar mass is accurate enough
    Section 2; 25 galaxies have spec-z with Delta z <0.1 for 18 galaxies, supporting the photo-z, but the whole sample depends on photometric redshifts.

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Pith. "Pith review of Unveiling the Dark Side of UV/Optical Bright Galaxies: Optically Thick Dust Absorption." pith.science (2026). https://pith.science/paper/TPQ3QKM5

@misc{pith2026241108100,
  author       = {Pith},
  title        = {Pith review of: Unveiling the Dark Side of UV/Optical Bright Galaxies: Optically Thick Dust Absorption},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TPQ3QKM5}},
  note         = {Machine review of arXiv:2411.08100}
}
read the original abstract

Over the past decades, a population of galaxies invisible in optical/near-infrared, but bright at longer wavelengths, have been identified through color selections. These so-called optically faint/dark galaxies are considered to be massive quiescent galaxies or highly dust-attenuated galaxies. Having the entire galaxy obscured by dust, however, is likely an extreme case of the much more common occurrence of optically thin and thick absorption coexisting in the same system. With the power of JWST imaging, we are able to spatially resolve massive galaxies at z~3, accurately model their spectral energy distributions, and identify candidate optically thick substructures. We target galaxies with log(M*/Msun)>10.3 and 2.5<z<3.5, and get 486 galaxies in CEERS and PRIMER fields. Based on excess NIR luminosity, we identify 162 galaxies (~33\% of the parent sample) as candidate hosts of optically thick substructures. We then carry out spatially resolved SED modeling to explore the physical properties of those dark substructures and estimate the amount of optically thick obscuration. We find that optically thick dust is ubiquitous in normal massive galaxies with a wide variety of SFR and morphology. 10-20\% of the stellar mass/SFR are unaccounted for in our selected galaxies, and the fraction is insensitive to stellar mass or SFR. The dark substructures are generally dustier than the rest of the galaxies and are irregularly distributed, arguing against an obscured AGN as the source of the NIR excess. A correlation between the obscured luminosity and the presence of a recent starburst in the past <100 Myr is also observed.

Figures

Figures reproduced from arXiv: 2411.08100 by the authors.

Figure 1
Figure 1. The optical depths as a function of wavelengths for different amounts of dust attenuation. The black dashed line (τ=1) shows the optically thin and thick threshold. The throughput of five NIRCam broadband filters (F150W, F200W, F277W, F356W, and F444W) are plotted in gray curves at the bottom. 1 when the dust attenuation gets sufficiently high, in￾dicating that at least part of the absorption becomes optically thick… view at source ↗
Figure 2
Figure 2. The SED modeling for a candidate CEERS galaxy with MIRI data coverage. The best-fit SED for the identified dark substructure is shown with lower transparency. RGB images of the galaxies are shown in the upper left corner, with the F444W for red, the F277W for green, and the F150W for blue. tion of our candidate and non-candidate galaxies on the rest-frame UVJ diagram (left) and the star-formation main sequence (righ… view at source ↗
Figure 3
Figure 3. The distribution of candidate (orange) and non-candidate (blue) galaxies within our parent sample. The left panel shows the rest-frame UVJ diagram, where the black curve indicates the threshold to separate quiescent and star-forming galaxies given by Whitaker et al. (2011). The right panel shows the SFR as a function of stellar mass, with the star formation main sequence (Whitaker et al. 2014) marked in a black dash… view at source ↗
Figures from the paper (15 more)
Figure 4
Figure 4. Figure 4: Examples of RGB image stamps for three candidate galaxies, with F444W in red, F277W in green, and F150W in blue. The first column shows the observed F444W band image, while the second column shows the model-predicted F444W image. the third column is the residual image …
Figure 5
Figure 5. Figure 5: The stellar mass, SFR, and dust attenuation of the integrated galaxies (blue) compared with those of the dark substructures therein (orange). The one-to-one relations are plotted in black dashed lines. The number distributions and median values are shown in histograms …
Figure 6
Figure 6. Figure 6: The non-parametric morphology measurements of the integrated galaxy and the identified dark substructures. The scatter plot displays color-coded centroid offsets between the two populations, with the black dashed line indicating the one-to￾one relation. The number dist…
Figure 7
Figure 7. Figure 7: Row 1: Comparing the stellar mass (left) and SFR (right) obscured and unobscured by optically thick dust. Blue scattered and binned points represent the integrated candidate galaxies, and orange points represent the identified dark substructures within those galaxies. …
Figure 8
Figure 8. Figure 8: The fraction of stellar mass (left) and SFR (right) obscured by optically thick dust. Blue points represent the integrated galaxies, and orange points represent the dark substructures therein. The number distributions and median values are shown in histograms on both a…
Figure 9
Figure 9. Figure 9: The fraction of stellar mass (left) and SFR (right) obscured by optically thick dust as a function of the specific star formation rate (sSFR). The typical relative uncertainties for individual data points are δx = 2.2% and δy = 51.4% for the left panel, δx = 2.2% and δ…
Figure 10
Figure 10. Figure 10: The fraction of stellar mass (left) and SFR (right) obscured by optically thick dust as a function of the mass￾weighted age (tmw). The typical relative uncertainties for individual data points are δx = 64.9% and δy = 51.4% for the left panel, δx = 64.9% and δy = 36.9%…
Figure 11
Figure 11. Figure 11: The scatter plot and running average of the in￾clination angles as a function of the F444W band flux excess. The typical error bar of individual data points is shown at the bottom right corner. The vertical dashed line marks our threshold cut for candidate selection. …
Figure 12
Figure 12. Figure 12: The central stellar mass surface density (left) and the normalized central stellar mass (right) as a function of the F444W band flux excess. The typical error bar of individual data points is shown at the bottom right corner for each panel. The vertical line marks the…
Figure 13
Figure 13. Figure 13: The UV spectral slope as a function of the F444W band flux excess. The vertical line marks the thresh￾old cut for candidate selection. For all the candidate galaxies (right to the vertical line), we also plot the UV spectral slopes of the dark substructures in orange,…
Figure 14
Figure 14. Figure 14: The burstiness of the recent SFH as a function of the observed flux excess in F444W (top), and the fraction of stellar mass (left) and SFR (right) obscured by optically thick dust. The two SFR ratios of different timescales are shown in different symbols. The ratio on…
Figure 15
Figure 15. Figure 15: The same as [PITH_FULL_IMAGE:figures/full_fig_p017_15.png]
Figure 16
Figure 16. Figure 16: Left: the number fraction of candidates as a function of the observed F444W band flux excess. The blue line refers to SED fittings without the F444W band photometry, while the orange line refers to fittings with the F444W band photometry. The final selection of σ thre…
Figure 17
Figure 17. Figure 17: The identification of dark substructures based on different decomposition methods for CEERS9-6044. Line 1: The red ellipse shows the bulge-disk decomposition given by Galfit. The F277W-F150W color map is shown in the middle panel, with the red ellipse overlaid to demo…
Figure 18
Figure 18. Figure 18: Here we show a few examples of the SFHs given by Prospector fit with different burstiness measurements. The burstiness is defined by the SFR ratio in certain timescales, where R1 = SF R0−30 Myr SF R30−80 Myr , and R2 = SF R0−80 Myr SF R80−180 Myr . The SFH of the inte…

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Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. The Cosmic Evolution Early Release Science Survey (CEERS)

    astro-ph.GA 2025-01 conditional novelty 5.0 of 10

    The CEERS survey overview shows that coordinated parallel JWST observations in the EGS field work as designed and have generated a public legacy dataset that enabled extensive early-universe science.

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Pith tools

Reviewed August 12, 2026 · model on record in the stance chip above.