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REVIEW 4 major objections 6 minor 131 references

Determining Total Infrared Luminosities from Submm Measurements of High Redshift Galaxies

T0 review · 4 major / 6 minor · reviewed 2026-08-03 · deepseek-v4-flash

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Pith's one-line read A single parameter—luminosity density—governs the infrared spectra of high-redshift galaxies, requiring a 1.6–2× correction to ALMA-derived luminosities.

desk verdict A useful, honest calibration paper whose typical-z correction factors are solid but whose z>4 'up to 2' factor rests on a single-galaxy template extrapolation that the data do not actually constrain. read the letter →

arxiv 2607.28875 v1 pith:MPLCFLL7 submitted 2026-07-30 astro-ph.GA

Maria Emilia De Rossi , George H. Rieke , Christina C. Williams , Volker Bromm , Jianwei Lyu , Meredith A. Stone , Yang Sun , Christopher N. A. Willmer
show 1 more author
Yongda Zhu
This is my paper
classification astro-ph.GA
keywords infraredluminositystarformationratesubmillimetergalaxieshighredshiftspectralenergydistributionmodifiedblackbodydensitydustemission
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

This paper aims to fix a systematic bias in how astronomers measure the total infrared luminosity, and hence the star formation rate, of dusty galaxies at redshifts above two. Because ALMA observes only the long-wavelength side of a galaxy's infrared spectrum, luminosities are usually obtained by fitting a modified blackbody, which ignores the warm-dust mid-infrared emission. The authors argue, using models tuned to high-redshift conditions and a set of local calibrator galaxies, that the relevant shape of the infrared spectrum is controlled almost entirely by one number: the luminosity density, or how much infrared light is packed into a cubic parsec of star-forming gas. If that is right, modified-blackbody luminosities for typical z>2 galaxies must be multiplied by roughly 1.6–1.7, and by up to ~2 for the most luminous z>4 sources, meaning past ALMA-based star formation rates are low by 0.2–0.3 dex in those regimes.

What carries the argument

Luminosity density (Lsun pc^-3) is the organizing variable: the paper shows that the peak temperature and the width of the infrared SED scale with this single quantity. The quantitative tool is a correction factor, defined as the ratio of the integral of a full template SED from 8 to 1000 µm to the integral of a modified blackbody fitted to it over 70–1000 µm. The Haro 11 SED—a local galaxy with extreme luminosity density (~1.5e4 Lsun pc^-3) and a broad, warm infrared spectrum—serves as the reference shape for the most luminous high-redshift sources. A set of radiative-transfer models for early-Universe galaxies (fixed radius 1.5 kpc, varying SFR from 5 to 30 Msun/yr, optically thin dust) re

What would settle it

Measure rest-frame 20–50 µm fluxes for a statistically complete sample of z>4, >1e12 Lsun galaxies (e.g., with JWST/MIRI or ALMA Band 8/9). If the average SED matches narrower low-luminosity-density templates rather than the broad Haro 11-like shape, the required correction reverts to ~1.6 and the paper's headline z>4 result (~2) is an overestimate. Alternatively, comparing ALMA 1 mm continuum with total IR luminosity from full SED decomposition would settle the correction directly.

Watch

Extended reading notes

Core claim

The paper establishes that variations in the far-infrared spectral energy distributions of high-redshift galaxies—both the shift of the peak to warmer temperatures and the broadening of the SED—are dominated by a single physical parameter, the luminosity density of the star-forming regions. Using radiative transfer models of early-Universe galaxies with a fixed ISM radius of 1.5 kpc and varying star formation rate, the authors show that higher luminosity density produces warmer and broader SEDs, while metallicity, gas fraction, and extinction have at most secondary effects. Consequently, the missing mid-infrared luminosity not captured by modified blackbody fits can be estimated in a general

Load-bearing premise

The largest corrections (up to ~2) assume that the most luminous z>4 ALMA galaxies have SEDs shaped like Haro 11, the local extreme-density reference; the paper states this incidence is 'high enough' to matter but does not quantify it, and the supporting composite rests on 18 galaxies with sparse wavelength coverage.

Editorial extensions

If this is right

  • Typical dusty galaxies at z>2: multiply modified-blackbody IR luminosities by ~1.6–1.7; published SFRs are low by ~0.2 dex.
  • Most luminous z>4 sources (L>1e12 Lsun): correction up to ~2 (0.3 dex), so their SFRs are underestimated the most.
  • Because the driver is a single parameter, the same correction framework applies without needing full SED coverage—one can use luminosity density (or its proxy, SFR surface density) to pick the appropriate factor.
  • The general increase in dust temperature with redshift found in earlier studies is explained as a luminosity-density effect, not a metallicity effect; metallicity plays little role.
  • Cosmic star formation rate density and the bright end of the galaxy luminosity function at z>2 shift upward once corrections are applied.

Reading between the lines

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

  • If luminosity density is the controlling parameter, JWST/ALMA high-resolution imaging that resolves star-forming clumps should predict which galaxies need the largest corrections—compact clumps imply Haro 11-like SEDs; this is testable with existing data.
  • The paper models only silicate+carbon dust continuum and omits PAH emission and stochastically heated very small grains; real galaxies with strong PAH features may have even more mid-IR emission, possibly requiring larger corrections than 2 in specific cases, or smaller if PAHs are weak.
  • The Eddington-limit argument implies an upper bound on SED broadening: the most compact, luminous starbursts should sit near the limit, so the correction factor should saturate around 2 rather than growing without bound—an observable prediction.
  • Since the models assume optically thin dust and a fixed ISM radius of 1.5 kpc, the correction factors may not transfer directly to lower-mass JWST-discovered galaxies with smaller effective radii; if such galaxies are detected by ALMA, their corrections could differ.
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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

4 major / 6 minor

Summary. The paper addresses how to convert ALMA submm photometry of high-redshift galaxies into total 8–1000 µm infrared luminosities. It argues that the shape of the infrared SED is controlled primarily by the luminosity density of the star-forming ISM, and that luminous z>4 galaxies frequently have broad, Haro 11-like SEDs rather than narrower local templates. On this basis it recommends multiplying modified-blackbody luminosities by ~1.6–1.7 in most circumstances, rising to ~1.75–2 for z>4 galaxies with L_IR > 10^12 L_sun. The paper combines a radiative-transfer model tuned to early-Universe conditions, local high-luminosity-density analogs, a z~2.5 lensed-galaxy template check, and template-integral corrections tabulated in Table 4.

Significance. If the central claim holds, the paper provides a useful and quantitative prescription for an important practical problem: deriving total infrared luminosities and obscured star formation rates from sparse ALMA data. The physical argument that luminosity density drives SED broadening is plausible and supported by local examples and by the model. The z~2.5 check with lensed galaxies is a genuinely valuable addition, and the paper is unusually honest about degeneracies and the template-dependent nature of the corrections. The weakest link is the high-redshift, high-luminosity tail of the prescription, where the evidence for Haro 11-like SEDs is indirect and where the recommended correction is largest. The paper is therefore worth publishing after the high-z claim is re-scoped or strengthened with quantitative support.

major comments (4)
  1. [§6.2, Table 4 (Haro 11 row) and Fig. 5] The headline z>4 correction 'up to ~2' rests on the assumption that luminous z>4 galaxies have Haro 11-like SEDs. The supporting composite of 18 galaxies (De Rossi et al. 2018) and Fig. 5 do not constrain rest-frame 8–50 µm: the ALMA points extend only to ~50 µm, and the Herschel/SPT points are longward. This is exactly the wavelength range that contributes the extra ~0.3 dex of luminosity in the Haro 11 template. Moreover, the theoretical model in §3.3 explicitly omits stochastically heated grains and PAHs and falls far below the data at λ≤15 µm, so the model cannot predict the mid-IR excess that drives the larger correction. Please either present the z>4 correction as an explicitly conditional upper end with a realistic uncertainty, or provide direct evidence (e.g., MIRI or stacking) that the 8–50 µm excess is present in the z>4 population.
  2. [§5, Table 2] The statement that the incidence of Haro 11-like behavior 'is high enough that it should be taken into account' is not quantified. Table 2 is a partial, non-statistical list of high-luminosity-density galaxies; there is no denominator, selection function, or uncertainty. Since the recommended correction factor depends directly on how common this SED shape is among ALMA-detected galaxies, the paper should either quote a measured incidence with errors from a well-defined sample, or explicitly state that the z>4 correction applies only to the subset known to have very high luminosity density.
  3. [§6.2, Fig. 7 and Table 4] The z~2.5 reference correction (1.74) is not measured directly: it is computed from a constructed hybrid template that joins the log(L)=10.85 Rieke template shortward of 50 µm to the log(L)=11.25 template, with the join point and normalization chosen to minimize χ² in the 6–11 µm range. This is a reasonable empirical procedure, but the resulting correction inherits the assumptions of that interpolation. Please report the sensitivity of the correction to the join wavelength (e.g., 40/60 µm) and to the choice of the low-luminosity template, and propagate this into the uncertainty quoted for the 'typical' 1.6–1.7 factor.
  4. [§3.4, Fig. 6] The central claim that SED behavior is dominated by a single physical parameter, luminosity density, is demonstrated mainly by varying SFR at fixed R=1.5 kpc. The top-right panel shows that varying R alone also changes the SED substantially at λ≲50 µm. Since R and SFR both enter luminosity density, a more direct test would be to show that arbitrary combinations of R, SFR, and Mgas with the same luminosity density produce approximately the same SED. Without such a one-parameter collapse test, the generality of the correction factors as functions of luminosity density alone is not fully established.
minor comments (6)
  1. [Throughout] Typos: 'difficult', 'sufficient', 'similiar', 'correponds', 'an Haro 11 model' should be 'a Haro 11 model'.
  2. [Fig. 7 caption] The caption refers to 'A1385a and A2128a', while the text and Table 3 discuss A1835a and A2218a. Correct the figure caption.
  3. [Table 4] The row labeled 'z = 6' cites Schreiber et al. (2018) as the template, but the text says the correction is for a modified template with T=47 K and β=1.6. Clarify whether this is the unmodified Schreiber template, a modified template, or a modified blackbody with those parameters.
  4. [Table 1] For clarity, add a dash or '—' in the Haro 11 row under z=2–4, as was done for the Kirkpatrick row under z=5–7, so that the table does not appear to have a missing entry.
  5. [§3.1.5, Eq. (7)] The choice β=0.57 for λ>150 µm is stated without uncertainty or discussion of how it affects the derived corrections. Since the correction factors involve integrating the SED, a sentence quantifying the sensitivity of Table 4 to β would be useful.
  6. [Table 2] Several entries give only a single value for r_eff with no error bar (e.g., ALMACAL-1, ALMACAL-2). State whether these are upper limits, characteristic values, or formal measurements.

Circularity Check

0 steps flagged · score 1.0 of 10

No demonstration of circularity: the correction factors are explicitly defined as template-to-modified-blackbody ratios, and the luminosity-density driver is an independent forward model; the z>4 Haro-11-based factor is an extrapolation risk, not a circular reduction.

full rationale

The quantitative corrections in Table 4 are, by the paper's own definition in Section 6.2 and footnote 6, ratios of the integral of a chosen template (8-1000 um) to the integral of a modified blackbody fitted to that same template; the text calls these 'examples to illustrate the size of the missing flux.' Thus the Haro 11 row yielding '~2' is the Haro 11 template's own conversion factor by construction, not a claim that the model independently predicts that number. The paper's substantive physical result - that SED broadening tracks luminosity density - is produced by the forward model of Section 3 for a fixed R=1.5 kpc and varying SFR, and is cross-checked against local galaxies in Section 2; it does not depend on the correction factors. The z>4, up-to-2 recommendation does rest on the premise that the most luminous high-z galaxies are Haro 11-like, supported by the De Rossi et al. (2018) composite and the non-statistical Table 2, with the paper itself acknowledging 'Although they are a minority of all high-z galaxies observed with ALMA, the incidence of this behavior is high enough' (Section 5). The model also explicitly omits PAHs/small grains and 'falls far below the measurements at lambda <= 15 um' (Section 3.3), so the extra mid-IR luminosity in the Haro 11 template is not physically modeled. These are real limitations and a load-bearing self-citation, but De Rossi et al. (2018) is an external published data analysis, and the paper also invokes Mitsuhashi et al. (2024a) for the luminosity-density prevalence. No fitted parameter is renamed as a prediction, and no uniqueness theorem is imported. The concern is therefore an extrapolation/template-selection risk, not a reduction of the result to its own inputs.

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

The central claim (correction factors) rests on a chain of modeling choices: the representative templates (Haro 11), empirical scaling relations extrapolated to z~5, and a fixed fiducial radius. None of these is independently validated for the target population; the correction factors are integrals over these chosen templates.

free parameters (6)
  • ISM radius R = 1.5 kpc
    Fiducial radius of the ISM component (Section 3.2); maps SFR to luminosity density. The paper notes smaller radii (0.5 kpc) produce >10x higher mid-IR luminosity (Section 3.5) but argues such compact systems are Eddington-limited.
  • long-wavelength emissivity index beta = 0.57
    Eq. 7: model SED multiplied by (150µm/λ)^β for λ>150 µm to improve fit to long-wavelength observations; a tuning parameter.
  • star formation period T = 67 Myr
    Chosen to make the SFR=30 Msun/yr model match Haro 11's stellar mass (Section 3.1.1); affects stellar population age and thus dust heating.
  • reference redshift z_ref = 5
    Fiducial redshift for model outputs; paper claims general trends do not depend on this choice.
  • dust composition (carbon fraction) = 20%
    Chosen to match Haro 11's silicate features (Section 3.1.5); model is degenerate to such choices.
  • template join luminosity = log(L)=10.85 shortward of 50µm
    Section 6.2: the z=2.5 reference SED is built by replacing the log(L)=11.25 template shortward of 50 µm with an interpolated log(L)=10.85 template and minimizing χ² in the 6–11 µm range — a fit that determines the 1.74 correction factor.
assumptions (4)
  • domain assumption Empirical scaling relations (Eqs. 3-6) for metallicity, dust-to-metal ratio, and gas mass, calibrated at low/intermediate z, hold at z~5.
    Used to set Zgas, D/M, Mgas for model galaxies; extrapolation of Tremonti et al. (2004), Sarkar et al. (2025), Popping & Péroux (2022), Scoville et al. (2016) to high z.
  • domain assumption Infrared luminosity is a direct proxy for UV luminosity absorbed by dust in heavily obscured regions.
    Section 2: used to estimate luminosity densities for local galaxies and to map SFR to luminosity density.
  • domain assumption Eddington star formation limit suppresses the most compact, highest luminosity-density configurations.
    Section 3.5: invoked to justify excluding smaller R cases that would otherwise break the 'single parameter dominates' claim.
  • domain assumption Yggdrasil population synthesis outputs and adopted dust opacities (including private communication from K. Misselt) are correct.
    Underlies the stellar SEDs and dust emission calculations (Sections 3.1.1, 3.1.5).

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Cite this review

Pith. "Pith review of Determining Total Infrared Luminosities from Submm Measurements of High Redshift Galaxies." pith.science (2026). https://pith.science/paper/MPLCFLL7

@misc{pith2026260728875,
  author       = {Pith},
  title        = {Pith review of: Determining Total Infrared Luminosities from Submm Measurements of High Redshift Galaxies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MPLCFLL7}},
  note         = {Machine review of arXiv:2607.28875}
}
read the original abstract

Determining total infrared luminosities for very high redshift galaxies is important to estimate the rate of star formation in heavily dust-embedded environments. It is also challenging because the most sensitive far infrared observatory, Herschel, was limited in sensitivity and its deepest measurements are subject to confusion noise. Thus, these determinations largely depend on ALMA, observing in the mm- and/or submm-wavelengths, which sample only the long-wavelength part of the spectral energy distributions (SEDs). Luminosities are conventionally estimated with modified blackbody fits to these measurements, but do not include the emission in the mid-infrared by warmer dust; there is evidence that this mid-IR component may be relatively strong in very high-redshift galaxies compared with local ones. A correction factor must be applied to the modified black body luminosities to derive the total infrared luminosity. We study infrared SEDs using simulations tuned to galactic conditions typical of high-z galaxies. We find that the different behaviors of infrared SEDs are dominated by a single key physical parameter, the luminosity density. This allows us to estimate the corrections for the missing mid-infrared luminosity in a general way. We find that a factor of ~ 1.6 - 1.7 (0.2 dex) is appropriate in most circumstances, with a larger factor of ~ 1.75 - 1.85 (~ 0.25 dex) up to 2 (0.3 dex) necessary for high redshift (z > 4) galaxies at the highest luminosities, > 10^{12} Lsun. These corrections are needed to estimate star formation rates based on total infrared luminosity.

Figures

Figures reproduced from arXiv: 2607.28875 by the authors.

Figure 1
Figure 1. The trend of temperature corresponding to the peak of the far infrared SED vs. galaxy metallicity, from Rémy-Ruyer et al. (2015). As usual, the oxygen abundance, 12+log(O/H), is used as a proxy for a galaxy’s ISM metal￾licity. The line is fitted to all points except the two at the lowest metallicity. Further details can be found in Rémy￾Ruyer et al. (2015) and references therein. De Rossi et al. (2018) concluded tha… view at source ↗
Figure 4
Figure 4. Similar to [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Far infrared SED summary. The figure is based on [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figures from the paper (2 more)
Figure 6
Figure 6. Figure 6: Comparison between the default model SED (blue solid line), corresponding to a compact stellar source, a radius R = 1.5 kpc for the ISM component, a gas fraction based on main-sequence galaxies, and no extinction effects (Section 3.2), and model SEDs derived when assum…
Figure 7
Figure 7. Figure 7: Photometry and spectroscopy of A1385a and A2128a merged, together with a customized template fit (the “z = 2.5 template”). See text for details. magnification of ∼ 22 (Rigby et al. 2008). For A1835a, the intrinsic Ltot ∼ 4×1012 L⊙ at z = 2.56 with a mag￾nification7 of …

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Pith tools

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