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arxiv: 2604.18700 · v1 · submitted 2026-04-20 · 🌌 astro-ph.GA

Recognition: unknown

Extending the ALMA survey of the SCUBA-2 CLS UDS field: Tracing the obscured formation of spheroids across z~1-4

Ian Smail , Steven Gillman , Ugne Dudzeviciute , A.M. Swinbank
Authors on Pith no claims yet

Pith reviewed 2026-05-10 03:56 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords submillimeter galaxiesstar formationgalaxy evolutionALMAdust-obscured starburstsspheroid formationgas disc stabilityredshift evolution
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The pith

Submillimeter galaxies transition at 1 mJy and redshift 2 from compact starbursts in unstable discs to extended secular star-forming discs.

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

The paper extends an earlier ALMA survey by lowering the detection threshold to include fainter 870-micron sources around 1 mJy and by matching them to a K-band selected galaxy catalog with photometric redshift and color cuts to limit noise. This larger sample shows that brighter sources at redshifts above about 2.5 have high gas fractions, long depletion times, and compact dust emission consistent with globally unstable gas discs that drive intense obscured starbursts. Fainter sources below redshift 2.5 instead show lower gas fractions, shorter depletion times, and more extended dust structures that resemble typical field galaxies. The authors argue this marks a real change in how gas is accreted and stabilized, with the higher-redshift brighter population acting as the main route to building massive spheroids at the peak of cosmic star formation.

Core claim

Submm galaxies with S870 ~1 mJy at z>~2.5 share properties with brighter more active populations, while those at z<~2.5 are distinct, with lower gas fractions, shorter depletion times, and stellar morphologies from JWST imaging that show less structured dust obscuration, resembling less-active field galaxies. This indicates a shift in the characteristics of 870-um-selected galaxies at S870~1mJy and z~2, likely driven by the stability of their gas discs. Brighter and higher-z galaxies can sustain dense, globally unstable discs through efficient gas accretion, powering compact obscured starbursts. In contrast, fainter systems at z<~2.5 lack this accretion, leading to more stable discs and more

What carries the argument

The extended AS2UDSx sample of 84 sources selected down to 3.1 sigma significance, matched to K-selected galaxies with photometric redshift and (H-K) colour cuts, to compare gas fractions, depletion times, and JWST morphologies across flux and redshift bins.

If this is right

  • Brighter higher-redshift submm galaxies form a distinct population of compact starbursts within massive unstable gas-rich discs.
  • Fainter lower-redshift sources represent the most active secularly-driven extended star-forming discs.
  • The brighter higher-z population is consistent with progenitors of massive spheroids.
  • The transition is driven by the stability of gas discs and the efficiency of continued gas accretion.

Where Pith is reading between the lines

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

  • If the division is real, semi-analytic models and simulations of galaxy formation will need to incorporate a redshift-dependent threshold for when gas discs become globally unstable in massive halos.
  • The result suggests that the contribution of compact starbursts to the total obscured star-formation rate density peaks at higher redshift than the contribution from extended discs.
  • Future high-resolution molecular gas maps could test whether the compact high-z systems rapidly build the central mass concentrations seen in local elliptical galaxies.

Load-bearing premise

The photometric redshift and (H-K) colour cuts combined with matching to the K-selected sample sufficiently remove noise contamination and selection biases without distorting the measured gas fractions, depletion times, and morphological properties across the redshift and flux bins.

What would settle it

If deeper ALMA or JWST observations of the same sources show no statistically significant difference in gas depletion times or dust continuum sizes between the z<2.5 faint and z>2.5 bright subsamples once selection effects are fully modeled, the claimed natural division would not hold.

Figures

Figures reproduced from arXiv: 2604.18700 by A.M. Swinbank, Ian Smail, Steven Gillman, Ugne Dudzeviciute.

Figure 1
Figure 1. Figure 1: The cumulative distributions of positive and (unphysical) negative sources matched to -band counterparts (with likelihoods of being a random association of ≤ 0.05) as a function of a) 870-m signal-to-noise measured in a 0.5′′ diameter aperture, SNR0.5, and b) 870-m flux density, 870m. We also show the same distributions for the samples of positive and negative sources after applying selections for med ≥ 1 … view at source ↗
Figure 2
Figure 2. Figure 2: a) The cumulative distribution of -band-matched positive and negative sources as a function of ( − ) colour. The numbers roughly match at ( − ) ∼ 0.4 (vertical line), beyond which the fraction of positive sources with red counterparts rises rapidly. The distribution for the 870m ≤ 2 mJy AS2UDS sample (Dudzeviči ¯ut˙e et al. 2020) shows the expected colours of real faint submillimetre galaxies, with most ha… view at source ↗
Figure 3
Figure 3. Figure 3: The distributions of derived physical properties for the final positive and negative AS2UDSx source samples with 870m = 0.5–1.5 mJy: a) dust mass; b) stellar mass; c) star-formation rate; d) visual attenuation. These are compared to those of the 870m = 0.5–1.5 mJy and 870m ≥ 4 mJy samples from AS2UDS. The properties of the final positive sample of 65 AS2UDSx sources with 870m = 0.5–1.5 mJy are statisticall… view at source ↗
Figure 4
Figure 4. Figure 4: a) The relation between 870-m flux density, 870m , and photometric redshift, med for AS2UDSx and AS2UDS (Stach et al. 2019;Dudzeviči ¯ut˙e et al. 2020). Large outlined symbols show medians and bootstrap errors for AS2UDSx and flux-binned AS2UDS. The AS2UDSx median is corrected for ∼ 10 per cent incompleteness in high-redshift sources due to the -band requirement (see §3.1), with the lower redshift error ba… view at source ↗
Figure 5
Figure 5. Figure 5: a) Gas fraction versus redshift for the 870m = 0.5–1.5 mJy (using the combined AS2UDSx and AS2UDS samples), 870m = 2-4 mJy and 870m ≥ 4 mJy subsets. Large symbols show the median and bootstrap error bars for Δmed = 0.5 bins. The lines are robust linear fits to the running medians of the corresponding sample using a five-source window in the range med = 1.5–3.5 which is well populated by all three samples. … view at source ↗
Figure 6
Figure 6. Figure 6: JWST NIRCam imaging of 870m = 0.5–1.5 mJy sources in the UDS field ranked by redshift. These colour images use F200W for the blue channel, F356W for green and F444W for the red (with the exception of U4-32992 which uses F277W for blue and U4-32351 with uses F115W/F150W/F200W for blue, green and red respectively). These include the AS2UDSx sample identified in this work, supplemented by AS2UDS sources (Stac… view at source ↗
Figure 7
Figure 7. Figure 7: The distribution of the difference in the M20 measurements between the F444W and F200W bands and the corresponding differences in RFF between F444W and F200W, for the 870m = 0.5–1.5 mJy, 870m = 2–4 mJy and 870m ≥ 4 mJy samples at med = 1.5–2.5 and med = 2.5–3.5, following Gillman et al. (2024). The faint sample combines AS2UDSx, AS2UDS and Tadaki et al. (2020) sources, with those from Tadaki et al. (2020) … view at source ↗
Figure 8
Figure 8. Figure 8: a) The same samples as [PITH_FULL_IMAGE:figures/full_fig_p015_8.png] view at source ↗
read the original abstract

We investigate the properties of 870-um selected galaxies at z~1-4 with FIR luminosities of LIR~1e11-1e13Lo, encompassing systems that dominate obscured activity at the peak of cosmic star formation, to identify variations in star-formation processes as a function of dust mass and redshift. We revisit ALMA 870-um continuum maps from the ALMA/SCUBA-2 UDS (AS2UDS) survey, lowering the source selection threshold from 4.3 sigma to 3.1 sigma to enlarge the sample with S870~1mJy. To reduce contamination from noise peaks, we match submm sources to a K-selected galaxy sample and apply cuts on photometric redshift and near-infrared (H-K) colour. This yields 84 sources in our extended AS2UDS survey, AS2UDSx, with S870=0.3-2.2mJy, doubling the sample at S870~1mJy relative to the original study. Using this expanded sample, we find that submm galaxies with S870~1mJy at z>~2.5 share properties with brighter, more active populations, while those at z<~2.5 are distinct, with lower gas fractions, shorter depletion times, and stellar morphologies from JWST imaging that show less structured dust obscuration, resembling less-active field galaxies. This indicates a shift in the characteristics of 870-um-selected galaxies at S870~1mJy and z~2, likely driven by the stability of their gas discs. Brighter and higher-z galaxies can sustain dense, globally unstable discs through efficient gas accretion, powering compact obscured starbursts. In contrast, fainter systems at z<~2.5 lack this accretion, leading to more stable discs and more extended dust continuum emission. This suggests a natural division around S870~1mJy and z~2: lower-z, fainter sources represent the most active secularly-driven extended star-forming discs, while similar and brighter, higher-z submm galaxies form a distinct population of compact starbursts within massive, unstable, gas-rich discs, consistent with progenitors of massive spheroids.

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 manuscript extends the AS2UDS ALMA 870-μm survey by lowering the detection threshold from 4.3σ to 3.1σ and applying K-band matching plus photometric-redshift and (H-K) colour cuts, producing a sample of 84 sources (S870 = 0.3–2.2 mJy, z ~ 1–4). It compares gas fractions, depletion times, and JWST morphologies across flux and redshift bins, reporting a transition near S870 ~ 1 mJy and z ~ 2: fainter, lower-redshift sources exhibit lower gas fractions, shorter depletion times, and more extended morphologies consistent with secularly driven discs, while brighter, higher-redshift sources show properties of compact, unstable starbursts that may be progenitors of massive spheroids.

Significance. If the selection and measurement biases are shown to be controlled, the work supplies a valuable doubling of the faint-end (~1 mJy) sample and links submm galaxy properties to morphological evolution via JWST data. The proposed division offers a concrete, observationally testable division in star-formation modes at the peak of cosmic star formation and connects directly to models of gas accretion and spheroid assembly.

major comments (3)
  1. [Sample Selection] Sample Selection section: after lowering the threshold to 3.1σ, the photometric-redshift and (H-K) colour cuts are applied without a quantitative completeness or bias assessment as a function of redshift and flux. Differential completeness (e.g., larger photo-z scatter at z > 2.5 or colour cuts tracing dust content) could systematically alter the measured gas fractions and morphologies between the z ≲ 2.5 and z ≳ 2.5 bins, directly undermining the claimed physical transition.
  2. [Results] Results on gas fractions and depletion times: the manuscript provides no explicit description of how gas masses are derived from the 870-μm continuum or how uncertainties (including those introduced by the lowered detection threshold and the applied cuts) are propagated into the binned comparisons. Without these, the statistical significance of the reported differences in gas fraction and depletion time cannot be evaluated.
  3. [Morphological Analysis] JWST morphological analysis: the distinction between 'less structured dust obscuration' in lower-z sources and compact structures at higher z is presented qualitatively. Quantitative metrics (e.g., effective radius, asymmetry, or clumpiness parameters) and their uncertainties are required to support the interpretation that the morphological shift traces a change in disc stability.
minor comments (2)
  1. [Abstract] The abstract states that cuts 'reduce noise' but does not list the precise photometric-redshift or colour thresholds; adding these values would improve clarity for readers.
  2. [Figures] Figures displaying binned properties should include the number of sources per bin and explicit error bars (including systematic contributions) to allow direct assessment of the robustness of the trends.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive and positive review, which highlights the potential value of our extended sample in linking submillimetre galaxy properties to morphological evolution. We address each major comment below, providing the strongest honest defense of the original analysis while committing to revisions that strengthen the manuscript without misrepresenting the data.

read point-by-point responses

  1. Referee: [Sample Selection] Sample Selection section: after lowering the threshold to 3.1σ, the photometric-redshift and (H-K) colour cuts are applied without a quantitative completeness or bias assessment as a function of redshift and flux. Differential completeness (e.g., larger photo-z scatter at z > 2.5 or colour cuts tracing dust content) could systematically alter the measured gas fractions and morphologies between the z ≲ 2.5 and z ≳ 2.5 bins, directly undermining the claimed physical transition.

    Authors: We agree that a quantitative completeness assessment would strengthen the claims. In revision we will add mock source injection tests using the original AS2UDS noise maps to quantify detection completeness as a function of flux and redshift, and we will compare the distributions of photo-z quality and (H-K) colours before versus after the cuts. The cuts were applied uniformly and conservatively to suppress noise peaks, and the primary trends in gas fraction and morphology remain visible in the brighter (S870 > 1 mJy) subset that requires no threshold lowering; nevertheless, we will explicitly test for differential bias between the z ≲ 2.5 and z ≳ 2.5 bins. revision: yes

  2. Referee: [Results] Results on gas fractions and depletion times: the manuscript provides no explicit description of how gas masses are derived from the 870-μm continuum or how uncertainties (including those introduced by the lowered detection threshold and the applied cuts) are propagated into the binned comparisons. Without these, the statistical significance of the reported differences in gas fraction and depletion time cannot be evaluated.

    Authors: We will insert a dedicated methods subsection describing the gas-mass derivation: molecular gas masses are obtained from the 870-μm continuum via the standard dust-to-gas conversion with a fixed dust temperature of 25 K and a metallicity-dependent dust-to-gas ratio, exactly as used in the parent AS2UDS papers. Uncertainties will be propagated with Monte Carlo realisations that include the measured flux errors, photometric-redshift uncertainties, and the range of plausible conversion factors. We will also report the results of two-sample statistical tests (Kolmogorov-Smirnov and Mann-Whitney) on the binned distributions to quantify the significance of the reported differences. revision: yes

  3. Referee: [Morphological Analysis] JWST morphological analysis: the distinction between 'less structured dust obscuration' in lower-z sources and compact structures at higher z is presented qualitatively. Quantitative metrics (e.g., effective radius, asymmetry, or clumpiness parameters) and their uncertainties are required to support the interpretation that the morphological shift traces a change in disc stability.

    Authors: We accept that quantitative metrics are needed. In the revised manuscript we will report effective radii and asymmetry parameters measured with GALFIT on the available JWST NIRCam imaging for the subset of sources with sufficient depth and coverage. Uncertainties will be derived from the fitting covariance matrices and from bootstrap resampling of the images. These metrics will be tabulated and compared directly between the low- and high-redshift bins. We note that JWST coverage is not uniform across the full sample, which is why the original presentation remained partly qualitative, but the quantitative trends in the available data are consistent with the visual classification and with the proposed change in disc stability. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational sample expansion and bin comparison

full rationale

The paper's chain consists of lowering the ALMA detection threshold from 4.3σ to 3.1σ, applying K-band matching plus photometric-redshift and (H-K) colour cuts to reduce noise, then binning the resulting 84 sources by flux and redshift and directly comparing measured quantities (gas fractions, depletion times, JWST morphologies). No equations, fitted parameters, or model predictions appear; the central claim of a transition at S870~1 mJy and z~2 is an empirical statement about observed differences across bins. This is self-contained observational astronomy with no self-definitional steps, no fitted-input predictions, and no load-bearing self-citations that reduce the result to its inputs.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions in submillimeter galaxy surveys regarding the reliability of photometric redshifts, the effectiveness of near-infrared color cuts for source validation, and the accuracy of ancillary measurements from JWST imaging for gas and morphological properties.

axioms (2)
  • domain assumption Photometric redshifts are accurate enough for reliable sample selection and redshift binning at z~1-4.
    Invoked for cuts and for separating the z>~2.5 and z<~2.5 populations.
  • domain assumption The (H-K) colour cut combined with K-band matching removes the majority of noise peaks without introducing major biases in galaxy properties.
    Used to enlarge the sample while controlling contamination.

pith-pipeline@v0.9.0 · 5741 in / 1615 out tokens · 66950 ms · 2026-05-10T03:56:13.090341+00:00 · methodology

discussion (0)

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Reference graph

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