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The Identification of Two JWST/NIRCam-Dark Starburst Galaxies at $z=6.6$ with ALMA

T0 review · 3 major / 4 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Two galaxies at z=6.6 hide from JWST but blaze in ALMA, forming 80–250 solar masses per year behind thick dust.

desk verdict Two robust NIRCam-dark starbursts at z=6.6, with the number-density claim honestly framed as an upper envelope rather than a measurement. read the letter →

arxiv 2506.06418 v1 pith:3DYXGQ47 submitted 2025-06-06 astro-ph.GA

Fengwu Sun , Jinyi Yang , Feige Wang , Daniel J. Eisenstein , Roberto Decarli , Xiaohui Fan , George H. Rieke , Eduardo Bañados
show 15 more authors
Sarah E. I. Bosman Zheng Cai Jaclyn B. Champagne Luis Colina Francesco D'Eugenio Yoshinobu Fudamoto Mingyu Li Xiaojing Lin Weizhe Liu Jianwei Lyu Chiara Mazzucchelli Xiangyu Jin Hyunsung D. Jun Yunjing Wu Huanian Zhang
This is my paper
classification astro-ph.GA
keywords high-redshiftgalaxiesdustystar-formingsubmillimeterstarburstquasarcompanionsJWSTNIRCamALMAgalaxyevolution
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 reports the discovery of two galaxies at redshift $z=6.6$ that are robustly detected in ALMA millimeter continuum and [C II] line emission, yet are extraordinarily faint or undetected in deep JWST/NIRCam imaging. These 'NIRCam-dark' starbursts have inferred star formation rates of $80\!-\!250\,M_\odot\,\mathrm{yr}^{-1}$ and are more obscured than the well-known local ultraluminous galaxy Arp 220. The authors argue that such galaxies could be the missing link between ultra-luminous 'blue monster' galaxies at $z>10$ and the massive quiescent galaxies seen at $z\gtrsim4$. Their halo-occupation analysis suggests these hidden starbursts could be as numerous as $n\sim10^{-5.5}\,\mathrm{Mpc}^{-3}$, about a third of the number density of either end of that evolutionary chain. If correct, current surveys are missing a substantial share of star formation during the epoch of reionization.

What carries the argument

The central object is the 'NIRCam-dark' starburst galaxy, defined by a rest-frame $3.6\,\mu\mathrm{m}$ to $1.2\,\mathrm{mm}$ flux ratio below $10^{-4}$, so optically faint that JWST/NIRCam cannot see it. The identification pipeline is an ALMA survey mapping the 1.2 mm continuum and [C II] line around 25 luminous quasars at $z\simeq6.5\!-\!6.8$, which produced multi-band ALMA detections for the two targets. The physical interpretation relies on energy-balance SED fitting with parametric star-formation histories, stellar population synthesis models, and a modified dust attenuation curve, combining NIRCam limits, ALMA photometry, and [C II] luminosities. The population estimate is carried by a Gaussian halo-occupation model, with a 'light model' assuming constant occupation above a halo-mass cutoff of $\log(M_{\mathrm{halo}}/M_\odot)\ge11.4$ inferred from simulations.

What would settle it

Deep JWST/NIRCam or MIRI observations that directly detect the stellar continuum of J1526m2050.C02 and J0305m3150.C05 would measure their stellar masses without SED priors; if these turn out to be below $\log(M_\star/M_\odot)\sim9.5$, the claim that they are progenitors of massive quiescent galaxies would be falsified. Alternatively, a blind ALMA survey covering several square degrees at $\sim0.3\,\mathrm{mJy}$ depth that finds far fewer than roughly one NIRCam-dark source per 100 arcmin$^2$ would rule out the light halo-occupation model's high number density.

Watch

Extended reading notes

Core claim

The central claim is that two ALMA-selected quasar companions, J0305m3150.C05 and J1526m2050.C02, are securely detected at $>8\sigma$ in the 1.2 mm dust continuum and in [C II] spectroscopy at $z\simeq6.6$, but are nearly invisible to JWST/NIRCam: J0305m3150.C05 is undetected (F356W $>28.0$ AB mag) and J1526m2050.C02 is only $26.5\pm0.1$ AB mag. Their spectral energy distributions imply dust-obscured starbursts with star formation rates of $80\!-\!250\,M_\odot\,\mathrm{yr}^{-1}$, infrared luminosities of $10^{11.9}\!-\!10^{12.4}\,L_\odot$, and stellar masses of $\log(M_\star/M_\odot)\simeq10.0\!-\!10.5$ with $0.5$ dex uncertainties. The paper shows these properties match the predicted descendants of UV-luminous 'blue monsters' at $z>10$ and the predicted progenitors of massive quiescent galaxies at $z\gtrsim4$. Using a light halo-occupation model calibrated to the detection of two such sources in 25 quasar fields, it infers a number density of $n=3^{+4}_{-2}\times10^{-6}\,\mathrm{Mpc}^{-3}$ at $z\sim6.6$, about 30% of the number densities of the two comparison populations.

Load-bearing premise

The stellar masses and star-formation rates of the two galaxies come from SED fitting in which the rest-frame optical is essentially undetected, so the derived values and the evolutionary link rest on priors in the fitting model rather than on direct measurements of starlight.

Editorial extensions

If this is right

  • NIRCam-dark galaxies at $z\sim7$ could be the direct ancestors of a substantial fraction of the massive quiescent galaxies seen at $z\gtrsim4$.
  • The light halo-occupation model implies these hidden starbursts account for roughly a third of the (U)LIRG population and the dust-obscured cosmic star-formation rate density at $z\sim7$.
  • The $z\sim8$ analogs predicted by the star-formation histories of early quiescent galaxies would fall below the detection limits of current wide JWST, ALMA, and single-dish surveys, remaining 'JWST-dark'.
  • The compact dust-continuum sizes of these galaxies, about 1 kpc in circularized effective radius, match the compact stellar sizes of $z\sim4$ quiescent galaxies, supporting a direct evolutionary link.
  • The occurrence rate of NIRCam-dark companions, two out of 25 quasar fields, implies a much higher duty cycle than that of UV-bright quasars, so these galaxies are not rare accidents of the quasar environment.

Reading between the lines

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

  • If the light halo-occupation model is correct, blank-field ALMA surveys of a few square degrees at the GOODS-ALMA depth should find roughly one such source per 100 arcmin$^2$; a null detection over a much larger area would directly falsify the high number density.
  • The stellar masses are effectively priors from the SED fit rather than direct measurements; deep MIRI or NIRSpec observations that detect the stellar continuum could confirm whether these galaxies are truly as massive as claimed, or whether the evolutionary link needs revision.
  • The proposed 'blue monster' to NIRCam-dark connection implies that very efficient dust production occurs within a few hundred million years; the measured dust-to-stellar mass ratio of about $10^{-2.3}$ is a direct test for dust-formation models at $z>6$.
  • The assumed independence of quasar and NIRCam-dark halo occupation may break down if the starbursts are triggered by the same large-scale environment that feeds the quasar; future clustering measurements of these hidden galaxies would test this directly.
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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. The paper reports the identification and characterization of two dusty star-forming galaxies at z~6.6 selected as companions to UV-luminous quasars in the ASPIRE survey. Both sources are robustly detected in ALMA 1.2 mm continuum (8.7 and 26.4 sigma) and spectroscopically confirmed via [C II] emission, yet they are extremely faint in JWST/NIRCam (F356W >28.0 AB mag for one, 26.5 mag for the other). The authors perform aperture photometry (including PSF subtraction for the quasar proximity), model the SEDs with CIGALE, and derive SFRs of 80-250 Msun/yr, large dust attenuation, and poorly constrained stellar masses around log(Mstar/Msun)~10.0-10.5. They argue these galaxies are viable progenitors of massive quiescent galaxies at z>=4 and descendants of z>10 'blue monsters'. Using a 2/25 occurrence rate among the ASPIRE quasar fields, they estimate a number density that could be as high as n~1e-5.5 Mpc^-3 under a 'light' halo-occupation model, about 30% of the quiescent and blue-monster densities, and predict that z~8 analogs may remain JWST-dark. The paper also discusses detectability in current and planned surveys.

Significance. If the population-level interpretation holds, these two objects are among the most extreme NIRCam-dark starbursts found at z>6 and would constitute an important missing link in massive galaxy evolution, bridging dust-obscured star formation in the EoR to early quiescent galaxies. The observational core is strong: the ALMA detections are multi-frequency and high-significance, the [C II] redshifts are secure, and the NIRCam photometry is carefully handled, including PSF subtraction for the quasar-contaminated source. The paper is also commendably explicit that the stellar masses are weakly constrained and that the number density is 'highly unconstrained' over two orders of magnitude. The value of the paper lies in demonstrating that such extreme systems exist and in framing testable predictions for wide-field surveys.

major comments (3)
  1. [§4.2, Eq. (1)] The conversion from the observed 2/25 occurrence rate to a halo-occupation fraction f=0.08 silently assumes uniform ALMA sensitivity and complete NIRCam companion identification across all 25 fields, but the paper does not demonstrate that the two detection fields have representative rms and depth, nor that the search for NIRCam-dark companions is complete in separation, primary-beam response, and velocity offset. The quoted Poisson uncertainty (0.08+0.10-0.05) is not propagated into the light-model density; the number density should either include field-by-field completeness corrections or be explicitly presented as an upper envelope conditional on ideal sensitivity.
  2. [§4.2, light model] The light-model cutoff log(M_halo/Msun)>=11.4 is taken from TNG100 galaxies with SFR>50 Msun/yr, but the observed targets are quasar companions with SFR~80-250 Msun/yr and are likely hosted by halos of log(M_halo/Msun)~12.3, so applying the same constant occupation fraction to all halos above 11.4 maximizes the density without direct justification. The text notes that quasar and NIRCam-dark occupations are assumed independent, but the selection of both sources as companions in quasar environments implies a positive environmental correlation; this should be folded into the uncertainty budget or discussed quantitatively.
  3. [§3.2 and Table 1] The stellar masses (log(Mstar/Msun)=10.0±0.5 and 10.5±0.5) are essentially unconstrained by the F115W/F200W upper limits and the marginal F356W detection, so the 'viable progenitors' argument in §4.1 is driven by the CIGALE prior rather than by data. The paper acknowledges the 0.5-dex errors, but Figure 3 compares these prior-influenced masses and SFRs with SFHs derived from JWST spectrophotometry, which themselves assume delayed-tau parameterizations; the evolutionary connection should be framed as a consistency check with a prior-dependent outcome, not as an independent confirmation.
minor comments (4)
  1. [Figure 1 caption] The caption contains a typo: 'J1526m2020.C02' should be 'J1526m2050.C02'.
  2. [§3.1] The definition 'NIRCam-dark (S_3.6µm/S_1.2mm <10^-4)' is ambiguous: F356W is 3.56 µm observed, not rest-frame 3.6 µm at z=6.6; please clarify whether the ratio uses observed-frame or rest-frame quantities and define the bands explicitly.
  3. [§4.3] The statement that the z=8 template 'is not far from the current detection limits' in F444W, MIRI F1000W-F1500W, and ALMA Band 6/7 seems in tension with the figure, which shows the template below the 5-sigma limits of those surveys; please clarify whether 'not far' refers to a factor of a few rather than detectability.
  4. [Abstract and §4.1] The phrase 'we show that the NIRCam-dark galaxies are viable progenitors' overstates the evidence; 'we argue' or 'we suggest' would be more appropriate given the degenerate SED modeling.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the ALMA/NIRCam identifications and SED characterization are self-contained, and the population-density claim is explicitly a conditional model extrapolation.

full rationale

The paper's central observational claims -- two z=6.6 ALMA-detected, [C II]-confirmed companions that are faint or undetected in NIRCam -- rest on direct ALMA and JWST measurements and on prior independent detections by Venemans et al. (2019, 2020), Decarli et al. (2017), Mazzucchelli et al. (2019), Pensabene et al. (2021), and Li et al. (2022). The new SED modeling uses standard external tools (CIGALE, Bruzual & Charlot 2003, Calzetti et al. 2000, Casey 2012) and is transparent about the weak stellar-mass constraint: 'the constraints on their stellar mass are rather poor ... large errors are natural consequence of poor constraints in the rest-frame UV/optical through Bayesian inference.' The evolutionary connection to z~4 quiescent galaxies and z>10 'blue monsters' is interpretive: it compares IR-luminosity SFRs and poorly constrained stellar masses with published SFH tracks; no equation in the paper makes that match a logical necessity. The number-density estimate is explicitly a conditional scaling, not a hidden prediction: the paper states 'the number density of NIRCam-dark galaxies at z~7 remains highly unconstrained: it may be as low as n~1e-8.1 Mpc^-3, but could also be as high as ~1e-5.5 Mpc^-3,' and the 'light model' sets the occupation fraction equal to the observed 2/25 occurrence rate ('The halo occupation fraction is therefore the observed NIRCam-dark occurrence rate'). This is an openly stated model assumption, and the paper cautions that 'our models assume independent halo occupations for quasars and NIRCam-dark galaxies.' Self-citations (Sun et al. 2025a for the ALMA catalog; Wang et al. 2023/in prep. for ASPIRE) are data/method references rather than load-bearing theoretical results, and the two galaxies were previously reported by external teams. No step reduces by construction to its own inputs.

Assumptions & free parameters 6 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new physical entities. The main burden rests on the choice of SED-fitting priors and on the halo-occupation models, both of which are standard tools but are not independently verified for this population. The number-density range is dominated by the two halo-occupation models, which bracket the uncertainty.

free parameters (6)
  • P_max for quasar host occupation = 0.02
    Fitted to reproduce the observed quasar number density at z~6.6 in Section 4.2.
  • log(Mc/Msun) for quasar host occupation = 12.73
    Characteristic halo mass chosen to match quasar clustering and number density.
  • sigma_m for quasar host occupation = 0.22
    Mass dispersion of the Gaussian halo-occupation model, taken from EIGER.
  • P_max for NIRCam-dark galaxies, heavy model = 0.37 (+0.46, -0.23)
    Fitted to match the observed occurrence rate of 2/25 NIRCam-dark galaxies.
  • Halo mass cutoff for light model = log(Mhalo/Msun) >= 11.4
    Chosen based on TNG100 simulations of halos hosting SFR>50 Msun/yr galaxies.
  • SFE and dust parameters in CIGALE = Tdust 30-60 K, beta 1.6-2.0, AV 0-15, age 20-500 Myr, tau 20-2000 Myr
    These are the standard CIGALE priors, but the stellar mass and SFR values are strongly prior-dependent.
assumptions (4)
  • domain assumption CIGALE energy-balance SED fitting with delayed-tau SFH, Bruzual and Charlot 2003 stellar population models, and Calzetti attenuation
    The derived stellar masses and SFRs assume this specific modeling framework (Section 3.2).
  • domain assumption The halo-occupation model of quasars follows a Gaussian P(Mhalo) with parameters from EIGER and Pizzati+24
    The number-density estimates depend on this empirical model (Section 4.2, Eq. 1).
  • domain assumption Independent halo occupation of quasars and NIRCam-dark galaxies
    Explicitly stated in Section 4.2. If the two populations are correlated, the number density estimates change.
  • domain assumption TNG100-based cutoff of log(Mhalo/Msun) >= 11.4 for NIRCam-dark hosting halos
    Used to define the light model, deriving from simulation rather than direct observation.

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Cite this review

Pith. "Pith review of The Identification of Two JWST/NIRCam-Dark Starburst Galaxies at $z=6.6$ with ALMA." pith.science (2026). https://pith.science/paper/3DYXGQ47

@misc{pith2026250606418,
  author       = {Pith},
  title        = {Pith review of: The Identification of Two JWST/NIRCam-Dark Starburst Galaxies at $z=6.6$ with ALMA},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3DYXGQ47}},
  note         = {Machine review of arXiv:2506.06418}
}
abstract

We analyze two dusty star-forming galaxies at $z=6.6$. These galaxies are selected from the ASPIRE survey, a JWST Cycle-1 medium and ALMA Cycle-9 large program targeting 25 quasars and their environments at $z\simeq6.5 - 6.8$. These galaxies are identified as companions to UV-luminous quasars and robustly detected in ALMA continuum and [C II] emission, yet they are extraordinarily faint at the NIRCam wavelengths (down to $>28.0$ AB mag in the F356W band). They are more obscured than galaxies like Arp220, and thus we refer to them as "NIRCam-dark" starburst galaxies (star formation rate $\simeq 80 - 250\,\mathrm{M}_{\odot}\,\mathrm{yr}^{-1}$). Such galaxies are typically missed by (sub)-millimeter blank-field surveys. From the star-formation history (SFH), we show that the NIRCam-dark galaxies are viable progenitors of massive quiescent galaxies at $z\gtrsim4$ and descendants of UV-luminous galaxies at $z>10$. Although it is hard to constrain their number density from a quasar survey, we conclude that NIRCam-dark galaxies can be as abundant as $n\sim10^{-5.5}$ Mpc$^{-3}$ assuming a light halo occupation model. If true, this would equal to $\sim$30% of the number densities of both the quiescent galaxies at $z\gtrsim4$ and UV-luminous galaxies at $z>10$. We further predict that analogs at $z\sim8$ should exist according to the SFH of early massive quiescent galaxies. However, they may fall below the current detection limits of wide JWST and ALMA surveys, thus remaining "JWST-dark". To fully trace the evolution of massive galaxies and dust-obscured cosmic star formation at $z\gtrsim8$, wide-field JWST/NIRCam imaging and slitless spectroscopic surveys of early protoclusters are essential.

Figures

Figures reproduced from arXiv: 2506.06418 by the authors.

Figure 1
Figure 1. JWST NIRCam images (F115W, F200W, F356W), ALMA 1.2 mm continuum images and [C II] 158 µm spectra of two NIRCam-dark galaxies at zspec ∼ 6.6. Because the luminous quasar J1526–2050 is visible to the northwest of J1526m2050.C02 (1. ′′6 separation), we also show the quasar-subtracted F200W and F356W image of J1526m2020.C02 in the third row, with ALMA continuum contours (purple) at 10 and 20σ overlaid. Image size is 4′′… view at source ↗
Figure 2
Figure 2. SEDs of the two NIRCam-dark galaxies (red circles). The best-fit SED models obtained by CIGALE are shown in the black lines. The SED templates of Haro 11 (nearby starburst galaxy, blue; J. Lyu et al. 2016), Arp 220 (nearby ULIRG, orange; L. Silva et al. 1998) and ALESS optically faint DSFGs at z ∼ 3 (purple; E. da Cunha et al. 2015), all redshifted and scaled to the ALMA 1.2-mm flux densities, are shown for comparis… view at source ↗
Figure 3
Figure 3. Stellar mass (left) and SFR (right) versus redshift for NIRCam-dark dusty starburst galaxies (red diamonds) in the context of massive galaxy evolution. For comparison we show the star-formation histories of massive quiescent galaxies at z ∼ 4 confirmed with JWST spectroscopy (gray circle: K. Glazebrook et al. 2024 but using the SFH from C. Turner et al. 2025; diamond: A. de Graaff et al. 2025 with solar-metallicity … view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: The number density constraint of NIRCam-dark galaxies. Left: The host halo mass function models of NIRCam-dark starburst galaxies at z = 6.6. We consider two models for their host mass distribution, including a light model (dashed orange line) and a heavy model (dashed…
Figure 5
Figure 5. Figure 5: The best-fit SED model of J0305m3150.C05 but redshifted to z = 8 and scaled to a SFR of 60 M⊙ yr−1 (solid black lines). Left: the near-to-mid-infrared SED compared with the 5σ detection limits of representative JWST NIRCam and MIRI imaging surveys, including JADES-medi…

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