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ALMA observations of pre-JWST z ~ 10 galaxy candidates: A CO(J = 9-8) line from a ULIRG at z = 2.54 and revisit of the photometric redshifts with JWST photometry

T0 review · 4 major / 4 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read ALMA and JWST show that UDS_18697, once thought to be a galaxy at $z\sim10$, is a dusty ultra-luminous infrared galaxy at $z=2.54$ with a CO($J=9-8$) line, and that most of the paper's pre-JWST $z\sim10$ candidates are low-redshift…

desk verdict A useful cautionary tale with a robust interloper conclusion, but the CO(9-8)/ULIRG headline needs the unpublished NIRSpec data to stand. read the letter →

arxiv 2608.12708 v1 pith:ILWRP3UT submitted 2026-08-13 astro-ph.GA

Suzuka Arai , Yuma Sugahara , Akio K. Inoue , Takuya Hashimoto , Ken Mawatari , Yi W. Ren , Steven L. Finkelstein , John R. Weaver
show 10 more authors
Rebecca L. Larson Seiji Fujimoto Yuichi Harikane Takahiro Morishita Yoichi Tamura Andreas Faisst Charles Steinhardt Nima Chartab Larry D. Bradley David B. Sanders
This is my paper · ORCID
classification astro-ph.GA
keywords high-redshiftgalaxiesLymanbreakselectionphotometricredshiftALMACO(9-8)lineultraluminousinfraredgalaxyJWST/NIRCamcontaminants
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 establish that UDS_18697, a galaxy previously selected from HST and Spitzer photometry as a $z\sim10$ candidate, is actually an ultra-luminous infrared galaxy at $z=2.54$ that emits a CO($J=9-8$) line, and that five of the six $z\sim10$ candidates in the ALMA sample are low-redshift interlopers once JWST/NIRCam photometry and NIRSpec spectroscopy are folded in. The finding matters because pre-JWST Lyman-break selections of the earliest galaxies can be severely contaminated by dusty star-forming and Balmer-break galaxies at $z\sim2$–3, and the paper offers a quantitative remedy: raising the Lyman-break colour threshold from $F115W-F150W>0.5$ to $F115W-F150W>1.0$ raises the purity of a $z>8.5$ sample from roughly 45% to roughly 75%, at some cost in completeness. If the result holds, current and future wide-area surveys such as the Euclid Deep Fields and the Roman High-Latitude Wide-Area Survey should adopt stringent colour cuts and deep short-wavelength coverage to avoid being dominated by interloping bright galaxies.

What carries the argument

The argument runs through a short chain of identifications and measurements. (1) The ALMA line at 293.27 GHz, co-spatial with UDS_18697, is identified as CO($J=9-8$) because the NIRSpec redshift $z=2.54$ places that transition at the observed frequency; the clump search gives a 4.5% false-positive probability for the line. (2) The $29.9\sigma$ dust continuum at $368\pm19\,\mu$Jy is modelled as a single-temperature modified blackbody with emissivity index $\beta=2.0$ and a dust temperature $T_{\rm d}$ from the Sommovigo et al. (2022) relation, giving $L_{\rm FIR}\approx1.1\times10^{12}\,L_\odot$. (3) The source is placed on the $L_{\rm FIR}$–$L'_{\rm CO(9-8)}$ diagram against local and $z>2$ samples. (4) The colour–colour criterion $F115W-F150W>0.5$ with $F150W-F356W<1.4$, applied to spectroscopically confirmed galaxies from the JADES and CANUCS catalogues, yields the purity estimate, and the stricter $F115W-F150W>1.0$ threshold raises purity from $\sim45\%$ to $\sim75\%$ for $z>8.5$.

What would settle it

Inspect the NIRSpec PRISM spectrum of UDS_18697: if it does not show multiple optical lines (e.g., H$\alpha$, [OIII], H$\beta$) at a common redshift $z=2.54$, or if the ALMA line frequency does not match CO($J=9-8$) at that redshift, the identification fails. Alternatively, re-observing the target with ALMA at higher sensitivity and resolution would settle the marginal $4.46\sigma$ detection: a genuine CO($J=9-8$) line should reproduce at $>5\sigma$, remain co-spatial with the $29.9\sigma$ dust continuum, and show a velocity width matching the NIRSpec lines.

Watch

Extended reading notes

Core claim

The central discovery is that the ALMA line at 293.27 GHz with significance $4.46\sigma$ toward UDS_18697 is not the targeted [OIII] 88$\mu$m line at $z\sim10$ but rather CO($J=9-8$) at $z=2.5356$, making the source a ULIRG with $L_{\rm FIR}\approx1.1\times10^{12}\,L_\odot$ and a dust temperature $T_{\rm d}\approx42.8$ K, and placing it slightly below, yet consistent with, the local $L_{\rm FIR}$–$L'_{\rm CO}$ relation while being among the faintest CO($J=9-8$) emitters at $z>2$. This identification is anchored by JWST/NIRSpec PRISM spectroscopy that fixes the redshift at $z=2.54$ (R. Larson et al., in prep.), and it is corroborated by SED fitting with JWST/NIRCam photometry that revises all three NIRCam-observed targets to $z\sim2$–2.5. The paper further claims, on the basis of spectroscopically confirmed galaxies from the JADES and CANUCS catalogues, that a stricter Lyman-break colour criterion substantially reduces low-$z$ contamination in high-$z$ samples.

Load-bearing premise

The load-bearing premise is that the unpublished JWST/NIRSpec PRISM redshift from R. Larson et al. (in prep.) is correct at $z=2.54$; every identification of the ALMA line as CO($J=9-8$), and therefore the ULIRG classification, the luminosity estimates, and the placement on the $L_{\rm FIR}$–$L'_{\rm CO}$ relation, collapses if that redshift is wrong.

Editorial extensions

If this is right

  • UDS_18697 becomes one of the faintest $z>2$ sources detected in CO($J=9-8$), extending the $L_{\rm FIR}$–$L'_{\rm CO}$ relation an order of magnitude downward in luminosity; more such serendipitous ALMA detections can populate the gap between local ULIRGs and high-$z$ DSFGs.
  • Pre-JWST $z\sim10$ candidates selected from HST+Spitzer photometry should be re-fitted with NIRCam photometry before being used to constrain luminosity functions or reionisation; this paper shows three targets that previously had $z_{\rm phot}\sim10$ collapse to $z\sim2$–2.5.
  • Euclid Deep Fields and Roman HLWAS should adopt a stringent Lyman-break colour threshold (equivalent to $F115W-F150W>1.0$) plus deep observations blueward of the break; otherwise bright low-$z$ interlopers will outnumber true $z>8.5$ galaxies.
  • Balmer-break galaxies at $z\sim2$ can mimic Lyman-break dropouts; requiring a non-detection in F090W ($S/N<2$) alongside the colour cut removes this class of contaminant.

Reading between the lines

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

  • If the unpublished NIRSpec redshift is independently confirmed, the CO($J=9-8$) identification makes UDS_18697 a benchmark for CO excitation in a moderately luminous ULIRG at cosmic noon; a direct test would be ALMA observations of lower-$J$ CO lines (e.g., CO(4-3) or CO(7-6)) at the same redshift, which should yield a consistent dynamical mass and line width.
  • The reported $\sim4.5\%$ and $\sim10\%$ false-positive probabilities for the two marginal ALMA lines suggest that comparable line searches should routinely report both positive and negative clump counts in their fields; without such statistics, marginal detections are hard to evaluate.
  • The purity jump from $\sim45\%$ to $\sim75\%$ is measured on the JADES/CANUCS spectroscopic sample, which may be biased toward blue continua or strong emission-line galaxies; applying the same colour cut to a completeness-corrected spectroscopic survey would sharpen the quantitative claim.
  • Because the magnification factor $\mu=1.35$ for UDS_18697 is not corrected, the intrinsic $L_{\rm FIR}$ and $L'_{\rm CO}$ could be $\sim35\%$ lower, moving the source closer to the local relation; correcting it tests whether the slight CO-bright offset is real.
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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 / 4 minor

Summary. The paper reports ALMA Band 7 observations of six pre-JWST z~10 galaxy candidates, targeting the [OIII] 88 micron line. A 4.5-sigma line and a 29.9-sigma dust continuum are detected in UDS_18697; the line is identified as CO(J=9-8) at z=2.5356 because unpublished JWST/NIRSpec PRISM observations reportedly give z=2.54. The authors classify UDS_18697 as a ULIRG with L_FIR=1.1e12 L_sun, using a dust temperature from Sommovigo et al. (2022) and a fixed beta=2.0, and place it on the L_FIR-L'_CO relation. SED fitting with new NIRCam photometry gives z~2-2.5 for three objects, and NIRSpec results (in prep.) indicate low redshifts for two more; J2140+0241 remains unidentified. Finally, using JADES and CANUCS spectroscopic catalogues, the authors propose that raising the Lyman-break colour threshold F115W-F150W from 0.5 to 1.0 increases the purity of z>8.5 samples from ~45% to ~75%, with implications for Euclid, Roman, and GREX-PLUS.

Significance. If the results hold, the paper provides a quantitative, empirically grounded caution about contamination in wide-field high-redshift galaxy surveys and a concrete selection guideline. The use of independent spectroscopic catalogues for the colour-purity analysis and the explicit clump-search false-positive estimate are strengths. However, the headline CO(J=9-8) identification and the consequent ULIRG classification rest entirely on an unpublished NIRSpec spectrum; the ALMA detection alone is marginal. The magnification-uncorrected luminosities further weaken the ULIRG classification. These issues affect the central claims and must be addressed before the paper can be considered archival.

major comments (4)
  1. [Section 3.2.1 and 3.3; Eq. (1)] The identification of the 293.27 GHz line as CO(J=9-8) rests entirely on the unpublished JWST/NIRSpec redshift of z=2.54 (R. Larson et al., in prep.). The ALMA data alone are marginal: peak S/N of 4.46, line-flux S/N of ~2.9, a 0.16 arcsec offset versus the expected 0.10 arcsec astrometric accuracy, and a 4.5% false-positive probability from the clump search in Appendix B. Without the NIRSpec data, the line could be a noise fluctuation or a different transition. The manuscript should include the NIRSpec redshift information (line list, signal-to-noise, or spectrum) or, failing that, explicitly state that the CO(9-8) identification and all derived quantities (L'_CO, L_FIR-based ULIRG classification, position on the L_FIR-L'_CO diagram) are tentative pending publication of the NIRSpec results.
  2. [Table 1 and Section 3.3] The ULIRG classification is not robust against the uncorrected magnification factor mu=1.35 listed in Table 1. The paper quotes L_FIR=1.1e12 L_sun with mu uncorrected; dividing by mu=1.35 gives about 0.8e12 L_sun, below the conventional 1e12 L_sun ULIRG threshold. Moreover, the reported 1-sigma range (L_FIR=1.1+1.0-0.3 x 10^12 L_sun) already extends below 1e12 L_sun. The authors should either correct the luminosities for magnification (quantifying the uncertainty in mu) or restate the ULIRG classification as conditional on mu<1.35, and should adjust the abstract and conclusion accordingly.
  3. [Section 3.3, after Eq. (1)] The quoted CO line luminosity, L'_CO(J=9-8) = 1.53 ± 0.54 K km s^-1 pc^2, is missing a factor of 10^9. Using Eq. (1) with the listed line flux (0.397 Jy km/s), D_L at z=2.536, and nu_obs=293.27 GHz gives L'_CO ~ 1.5e9 K km s^-1 pc^2, consistent with the axis range in Figure 3. The text should read (1.53 ± 0.54) x 10^9 K km s^-1 pc^2. This is a numerical error in the central measurement of the paper and must be corrected.
  4. [Section 3.3, dust temperature and beta] The L_FIR estimate is derived from a single continuum measurement with a fixed emissivity index beta=2.0 and a dust temperature assigned from the Sommovigo et al. (2022) relation with a uniform metallicity prior of Z=0-2 Z_sun. The resulting L_FIR has an asymmetry (1.1+1.0-0.3 x 10^12 L_sun) that spans below the ULIRG threshold even before magnification correction, and the central value is largely set by the assumed T_d. The authors should discuss the sensitivity of the ULIRG classification to the choice of beta and to the T_d relation, and ideally provide a table of L_FIR for a grid of T_d and beta values.
minor comments (4)
  1. [Section 3.2.2 vs Table 4] The line properties for COSMOS-z10-2 are inconsistent between the text and Table 4: the text gives line flux 0.475±0.169 Jy km/s, central frequency 334.66±0.07 GHz, and FWHM 463.06±73.77 km/s, while Table 4 lists 0.439±0.157 Jy km/s, 334.67±0.06 GHz, and 415.42±63.16 km/s. Please reconcile these values.
  2. [Section 5.2.1] The purity estimates of ~45% and ~75% are quoted without the number of galaxies in the respective redshift bins. Since the underlying JADES/CANUCS sample is incomplete and may be biased toward strong breaks, it would be helpful to state the sample sizes (N_z>8.5 and N_interloper) and the exact cuts used (including S/N_F090W<2 and S/N_F150W>5) so that readers can assess the statistical weight of the proposed F115W-F150W>1.0 threshold.
  3. [Appendix B] The false-positive probability for UDS_18697 uses the number of clumps on the inverted map (N_neg) as the background estimate, but N_pos and N_neg differ by a factor of about 2.5 in the 1-arcsec aperture. The authors note this may be statistical fluctuation, but a bootstrap or Monte Carlo estimate of the false-positive rate would be more robust; currently the 4.5% probability is tied to a single noisy measurement of N_neg.
  4. [Section 3.2.1] The statement that the line is 'co-spatial with the position of UDS_18697' is in tension with the reported 0.16 arcsec offset, which is larger than the expected 0.10 arcsec astrometric accuracy. Please clarify the positional tolerance used in this assessment.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity found: empirical inputs (ALMA line/continuum, JWST photometry, JADES/CANUCS spectra) are independent, with no fitted parameter renamed as a prediction.

full rationale

The paper is an empirical observational study. The central claims are: (1) UDS_18697 hosts a CO(J=9-8) line at z~2.54; (2) it is a ULIRG with L_FIR~1.1e12 L_sun; and (3) a brighter Lyman-break colour threshold improves z>8.5 sample purity. None of these claims reduces to its own input. The CO(J=9-8) assignment uses the ALMA line frequency (293.27 GHz) combined with the external JWST/NIRSpec redshift z=2.54 from R. Larson et al. in prep.; the redshift is not derived from the ALMA line, and the ALMA line is not fitted to the redshift. L'_CO is computed directly from the measured line flux via the standard Solomon et al. (1992) formula. L_FIR is computed from the measured 30-sigma continuum plus a dust temperature T_d=42.8 K obtained from the published Sommovigo et al. (2022) relation with fixed beta=2.0; T_d is not fit to this target's SED, and the luminosity is not adjusted to force any correlation. The L_FIR versus L'_CO(9-8) comparison uses independent literature samples (Rosenberg et al. 2015; Liu et al. 2015; Riechers et al. 2021; Butler et al. 2023), so that statement is not circular. The photometric-redshift revisit uses JWST/NIRCam photometry from the ASTRODEEP-JWST catalogue and bagpipes fitting, independently of the ALMA data. The colour-selection purity analysis is based on independent JADES and CANUCS spectroscopic catalogues, not on the paper's own targets; the estimated purity increase from ~45% to ~75% when raising F115W-F150W from 0.5 to 1.0 is therefore an empirical benchmark test, not a construction. The only caveat is that the NIRSpec redshift anchoring the CO identification is cited as in-preparation work by co-authors and is not shown; this is a verifiability gap, not circularity, because the spectrum is an external observation that does not depend on the ALMA measurements or on any parameter fitted in this paper. No equation in the paper is equivalent by construction to its inputs, and no fitted parameter is relabelled as a prediction. Score 0 is therefore appropriate.

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

No new physical entities are introduced. The key free parameters are the dust temperature model inputs and the magnification correction, all acknowledged. The colour-threshold analysis rests on standard photometric selection assumptions.

free parameters (4)
  • Dust temperature T_d = 42.8 +8.7 -3.5 K
    Derived from the single-band continuum using the Sommovigo et al. (2022) physical model with random metallicity (0-2 Zsun) and beta=2.0; L_FIR scales strongly with this value.
  • Emissivity index beta = 2.0
    Assumed fixed for the modified blackbody in the L_FIR calculation; a different beta would change the total luminosity.
  • Metallicity prior Z = random uniform in 0-2 Zsun
    Randomly drawn in the Monte Carlo; dust temperature depends weakly on Z, but the prior is not data-driven for this object.
  • Magnification factor mu = 1.35
    Adopted from Finkelstein et al. (2022a) but not corrected for in the luminosities due to uncertainty; could shift L_FIR and L'_CO down by roughly 35 percent.
assumptions (4)
  • standard math Flat Lambda-CDM cosmology with Omega_M=0.310 and H0=67.7 km/s/Mpc (Planck 2020)
    Used to compute luminosities and distances (Section 1).
  • domain assumption Calzetti et al. (2000) dust attenuation law and delayed-tau star formation history in SED fitting
    Adopted in bagpipes fitting (Section 4); alternative SFH/attenuation assumptions could shift the inferred redshifts.
  • domain assumption Single-temperature modified blackbody with beta=2.0 represents the FIR SED
    Used to derive L_FIR from one continuum point (Section 3.3); multi-component dust could change the result.
  • domain assumption The JADES/CANUCS spectroscopic sample is representative enough to measure purity fractions
    Purity numbers in Section 5.2 rely on secure-redshift samples that the authors note are incomplete and potentially biased (footnote 13).

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Cite this review

Pith. "Pith review of ALMA observations of pre-JWST z ~ 10 galaxy candidates: A CO(J = 9-8) line from a ULIRG at z = 2.54 and revisit of the photometric redshifts with JWST photometry." pith.science (2026). https://pith.science/paper/ILWRP3UT

@misc{pith2026260812708,
  author       = {Pith},
  title        = {Pith review of: ALMA observations of pre-JWST z ~ 10 galaxy candidates: A CO(J = 9-8) line from a ULIRG at z = 2.54 and revisit of the photometric redshifts with JWST photometry},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/ILWRP3UT}},
  note         = {Machine review of arXiv:2608.12708}
}
abstract

We present Atacama Large Millimetre/submillimetre Array (ALMA) observations targeting the [OIII]$88\,\mu$m line for six $z\sim10$ galaxy candidates selected with the Hubble Space Telescope and the Spitzer Space Telescope. We detect a line ($4.5\sigma$) and dust continuum emission ($30\sigma$) in UDS_18697, while detecting neither robust line nor continuum emission in the remaining five objects. The detected line in UDS_18697 is identified as CO($J=9-8$), because follow-up James Webb Space Telescope (JWST) NIRSpec observations have confirmed the redshift as $z=2.54$. UDS_18697 is classified as an ultra luminous infrared galaxy (ULIRG) with far-infrared (FIR) luminosity of $L_\mathrm{FIR}\approx1.1\times10^{12}\,L_\odot$, assuming a dust temperature of $T_\mathrm{d}\approx42\,$K, estimated using a physically-motivated method. We find that UDS_18697 follows the $L_\mathrm{FIR}-L'_\mathrm{CO}$ relation for local and $z>2$ galaxies, albeit being slightly brighter in CO($J=9-8$). Also, based on the follow-up NIRSpec observations and spectral energy distribution fitting using JWST/NIRCam photometry, we found that most of our targets are suggested to be low-$z$ interlopers. Motivated by these redshift misclassifications, we investigate colour--colour selection criteria for high-$z$ galaxies using JWST spectroscopic survey catalogues. We find that elevating a colour threshold tracing the Lyman break is crucial for constructing a robust high-$z$ sample, particularly for wide field surveys such as Euclid Deep Fields and Roman High-Latitude Wide-Area Survey.

Figures

Figures reproduced from arXiv: 2608.12708 by the authors.

Figure 2
Figure 2. Extracted line spectra of UDS_18697 (top panel) and COSMOS￾z10-2 (bottom panel) along with the best-fit Gaussian functions (solid line). The rms levels are shown in the dotted lines. 3.2.3 Other targets For the remaining four objects, neither line nor continuum emis￾sion was detected. We put 3𝜎 upper limits on the line fluxes and continuum flux densities ( [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. The FIR luminosity 𝐿FIR and CO line luminosity 𝐿 ′ CO correlation. The value of UDS_18697 is shown in the blue diamond. Green squares are DSFGs at 𝑧 ∼ 2–6 taken from Cañameras et al. (2018), Riechers et al. (2021) and Riechers (2025). Red diamonds indicate QSOs at 𝑧 ∼ 2–4 shown in Butler et al. (2023). Grey circles are local galaxies presented in Rosenberg et al. (2015). The dashed line shows the best-fit line for 1… view at source ↗
Figure 4
Figure 4. SEDs of UDS_18697 (top), COSMOS_20646 (middle), and UDS_7815 (bottom), together with the redshift probability distribution (top left in each panel). Blue lines and circles show the model spectrum and pho￾tometry, respectively, while blue squares indicate the measured photometry of the NIRCam+HST photometry. The grey lines and open markers present the result of the fittings using the Spitzer+HST photometry (symbols a… view at source ↗
Figures from the paper (1 more)
Figure 5
Figure 5. Figure 5: Left: A colour–colour diagram showing the distribution of galaxies from the JADES and CANUCS spectroscopic catalogues, and our sample galaxies with NIRCam photometry. The spectroscopically confirmed galaxies in different redshift ranges are shown in different colours a…

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