Pith. sign in

REVIEW 3 major objections 5 minor 7 cited by

The first systematic study of [OIII] 88µm at z>8 finds two luminous oxygen lines and a candidate powerful ionized outflow in UNCOVER-10646, with a mass outflow rate that exceeds the galaxy's star formation rate.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-03 16:01 UTC pith:MI3TVHVF

load-bearing objection Two solid new [OIII]88 detections at z>8, plus a plausible but unproven outflow whose statistical support depends on the extraction. the 3 major comments →

arxiv 2512.14486 v2 pith:MI3TVHVF submitted 2025-12-16 astro-ph.GA

A first systematic study of [OIII] 88μm at z>8: two luminous oxygen lines and a powerful ionized outflow in the first 600 million years

Hiddo S. B. Algera , John R. Weaver , Tom J. L. C. Bakx , Manuel Aravena , Rychard J. Bouwens , Karin Cescon , Chian-Chou Chen , Elisabete da Cunha
show 30 more authors
Pratika Dayal Andreas Faisst Andrea Ferrara Seiji Fujimoto Takuya Hashimoto Kasper Heintz Rodrigo Herrera-Camus Jacqueline Hodge Hanae Inami Akio K. Inoue Jorryt Matthee Romain Meyer Shoichiro Mizukoshi Chayan Mondal Themiya Nanayakkara Pascal A. Oesch Andrea Pallottini Huub R\"ottgering Lucie E. Rowland Sander Schouws Renske Smit Laura Sommovigo Daniel P. Stark Yuma Sugahara Livia Vallini Bovornpratch Vijarnwannaluk Paul van der Werf Norbert Werner Joris Witstok Mengyuan Xiao
This is my paper
classification astro-ph.GA
keywords [OIII] 88 µmhigh-redshift galaxiesEpoch of Reionizationionized outflowsALMAstar formationgravitational lensingmass loading factor
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper tries to establish that the far-infrared [OIII] 88µm line can be used systematically to find and characterize galaxies in the first 600 million years of cosmic history, and that at least one such galaxy hosts a powerful ionized outflow. Using ALMA to target four UV-luminous, gravitationally lensed galaxies at z=8.5–10.3, it detects the line in two sources, UNCOVER-10646 at z=8.51 and DHZ1 at z=9.31, and shows that their intrinsic luminosities (roughly 1–2×10^9 Lsun) follow the local [OIII]-SFR relation for dwarf galaxies. The central new claim is that the [OIII]88 line in UNCOVER-10646 is better described by a narrow plus a broad component, with the broad component having FWHM≈1370 km/s and carrying about twice the flux of the narrow one. Interpreted as a compact ionized outflow, this implies a mass outflow rate of about 130 solar masses per year and a mass loading factor of about three, meaning the galaxy expels ionized gas faster than it forms stars, at a speed that likely exceeds its escape velocity. If correct, this is the earliest ionized outflow yet measured through this line, showing that feedback-driven gas ejection was already underway within 600 million years of the Big Bang.

Core claim

On its own terms, the paper's central discovery is that the [OIII] 88µm line in the z=8.51 galaxy UNCOVER-10646 is not a single Gaussian: its high signal-to-noise peak-pixel spectrum is significantly better fit by a narrow plus a broad component (ΔBIC≈20), with the broad component having FWHM = 1366 km/s. Under the interpretation that this broad component is an ionized outflow, the inferred outflow mass is ~1.4×10^8 M_sun, the mass outflow rate is 128 M_sun/yr, and the mass loading factor η = 2.9, exceeding the galaxy's own star formation rate and exceeding its estimated escape velocity. The paper further establishes that the two detected sources have intrinsic [OIII]88 luminosities of (1.1–

What carries the argument

The central object is the [OIII] 88µm far-infrared fine-structure line, observed with ALMA at ~30–50 km/s spectral resolution; it traces the low-density ionized ISM and is typically brighter than [CII] at z>6. The kinematic argument is carried by a dual-Gaussian decomposition of the line profile with Bayesian model comparison (ΔBIC), applied to a peak-pixel spectrum to maximize signal-to-noise on a compact, unresolved component. Outflow properties are derived from the broad Gaussian's flux, width, and assumed size (0.3″), using the standard ionized-outflow mass and mass-outflow-rate formalism.

Load-bearing premise

The broad, high-velocity wings in UNCOVER-10646's [OIII]88 line are a real, compact ionized outflow rather than an artifact of the peak-pixel extraction or the kinematics of the unresolved merger of two AGN; the evidence is strong only in the peak-pixel spectrum (ΔBIC≈20), the source is not spatially resolved, and the 0.8″-aperture spectrum prefers the two-component fit only marginally (ΔBIC≈2.7).

What would settle it

A high-resolution ALMA observation that spatially resolves [OIII]88 in UNCOVER-10646 and finds the high-velocity emission either disappears or is not spatially coincident with a compact outflow; or JWST/NIRSpec high-resolution spectroscopy showing no broad component in [OIII]5007; either would overturn the outflow interpretation.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • The [OIII]88 line can spectroscopically confirm and kinematically characterize z>8 galaxies efficiently, even in 2–4.5 hours of ALMA time, including for sources at z>9.
  • Luminous [OIII]88 emitters at z>8 follow the local [OIII]-SFR relation for dwarf galaxies, reinforcing [OIII]88 as a star-formation tracer in the Epoch of Reionization.
  • Powerful ionized outflows with mass loading factor η≈3 exist in the first 600 million years; if real, the outflow's velocity exceeds the galaxy's escape velocity, so it will enrich the circumgalactic and intergalactic medium.
  • The deep [OIII]88 upper limit for the z=10.07 X-ray AGN UHZ1 implies the AGN's obscuration is not due to galaxy-wide dust; the line non-detections and stringent dust limits indicate subdued dust production in these early systems.
  • Higher-resolution ALMA follow-up is explicitly required to confirm and spatially resolve the outflow, and JWST/NIRSpec high-resolution spectroscopy should reveal a corresponding broad component in rest-optical [OIII] lines.

Where Pith is reading between the lines

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

  • If outflows like this are common at z>8, they could explain the puzzling UV brightness of early galaxies by clearing dust on short timescales; the tentative ~2σ extended dust continuum co-spatial with UNCOVER-10646 is a direct, testable symptom of this dust-clearing scenario.
  • Because the target is a late-stage merger of two AGN, the outflow may be partly AGN-driven; a clean test is to compare the broad-component flux and velocity in [OIII]88 with future high-resolution [OIII]5007 mapping of each merger component.
  • The large difference in ΔBIC between peak-pixel (20) and aperture (2.7) extractions is a cautionary lesson: for unresolved sources, tests for broad-line outflows should be reported for both extraction methods, since aperture dilution can mask otherwise strong evidence.
  • If confirmed, this sets a quantitative benchmark at z~8.5 for simulations of feedback-regulated galaxy formation, which currently predict mass loading factors of order unity to a few at these stellar masses.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper presents the first systematic ALMA Band 7 study of [OIII] 88 μm emission and dust continuum in four gravitationally lensed, JWST-selected galaxies at z = 8.5–10.3. [OIII] 88 is robustly detected in UNCOVER-10646 at z = 8.5080 ± 0.0011 (15σ) and in DHZ1 at z = 9.3113 ± 0.0006 (6σ), with intrinsic luminosities L ≈ (1.1–1.6)×10^9 L_sun that place them on the local [OIII]-SFR relation; neither of the two z > 10 targets is detected, yielding deep limits. The central novel claim is that the high-S/N detection in UNCOVER-10646 shows a broad line component (FWHM ≈ 1366 km/s) interpreted as a powerful ionized outflow, with inferred Mdot_out ≈ 128 M_sun/yr and mass-loading factor η ≈ 2.9. The authors extensively caveat that this outflow signature is statistically strong only in a peak-pixel extraction (ΔBIC ≈ 20) and weak in the fiducial 0.8 arcsec aperture (ΔBIC = 2.7), and that the source is an unresolved, likely merging pair of AGN.

Significance. If the outflow interpretation is confirmed, this would be the earliest ionized outflow measured through [OIII] 88, with a mass-loading factor exceeding the galaxy's SFR and plausibly escaping the galaxy. The paper's strengths include robust 15σ and 6σ line detections with verified redshifts, a first systematic multi-target sample at z > 8, careful checks against cleaning artifacts (including a dirty-cube comparison), transparent presentation of the statistical evidence for both extraction choices, and comparison of the derived quantities to established local relations and external simulations. The deep upper limits for the z > 10 targets, especially UHZ1, are also valuable. However, the headline outflow claim rests on a single unresolved peak-pixel feature whose statistical significance drops to marginal in the fiducial aperture, and the source's likely merger nature provides a plausible alternative explanation. The paper is honest about these caveats, but the abstract and summary overstate the robustness of the outflow discovery.

major comments (3)
  1. [Section 4.3.1 / Appendix D, Fig. 13] The statistical evidence for the broad component is extraction-dependent. The 'very strong evidence' (ΔBIC ≈ 20) is obtained only for the peak-pixel spectrum (Section 4.3.1), while the fiducial 0.8''-aperture extraction defined in Section 2.3 yields ΔBIC = 2.7, i.e., only 'positive evidence' per the Raftery scale (Appendix D, Fig. 13). The authors acknowledge this in Section 4.3.5, but the abstract and summary present the outflow as 'uniquely revealed.' Because the outflow mass, rate, and mass-loading factor in Section 4.3.2 are derived entirely from the broad component, the central claim should either be reframed as a candidate outflow pending the fiducial-aperture evidence, or the paper should justify why the peak-pixel extraction is the appropriate measurement and quantify the selection effect. As it stands, the discovery claim is not supported by the paper's own fiducial measurement.
  2. [Section 2.1.1 / Section 4.3.5] UNCOVER-10646 is described as a likely late-stage merger of two AGN, unresolved in the ALMA observations (Appendix D: beam-deconvolved size <0.36'' × <0.22''). A superposition of kinematically distinct components from the merging galaxies can produce broad, symmetric line wings without a single physical outflow. The paper's arguments against this — the apparent symmetry of the profile and the lack of evidence for a third component — reduce the likelihood of a two-component merger signature but do not exclude it. This is load-bearing for the physical interpretation. The abstract's 'uniquely reveals ... an ionized outflow' should be softened to 'candidate ionized outflow' unless the authors present additional kinematic modeling (e.g., a two-component merger model) that can be compared to the observed profile.
  3. [Section 4.3.2, Eq. (1)] The outflow mass and rate depend crucially on quantities taken from 'Weaver et al. (in preparation)': SFR = 45.4 ± 1.7 M_sun/yr, stellar mass, metallicity 12+log(O/H) = 8.12, and the AGN identification. If this companion paper is not publicly available at the time of review, the outflow properties are not independently checkable. Please include the relevant values (or an explicit tabulation) in the present paper, or provide a public version of the companion analysis. This is not a fatal flaw, but it is necessary for reproducibility of the paper's quantitative claims.
minor comments (5)
  1. [Section 3.2] The quoted significances of 15σ and 6σ refer to the peak pixel S/N in the moment-0 maps. Please state this explicitly in the text and figure captions, as the line-flux S/N may differ and the reader could otherwise misinterpret the detection significance.
  2. [Figure 6] In the bottom panels, the two fits are shown in separate panels without repeated y-axis labels. Consider aligning the panels or adding common axis labels to facilitate direct visual comparison.
  3. [Section 4.2] The statement that all currently detected z > 8 galaxies fall within ~0.3 dex of the local [OIII]-SFR relation would benefit from specifying whether that scatter is the intrinsic scatter of the De Looze et al. (2014) relation or the observed scatter of the plotted sample.
  4. [Section 2.3, footnote 1] The footnote appears to contain a formatting error: '1 A range of 1.2×FWHM ...' should read 'A range of 1.2×FWHM ...'.
  5. [References] Several crucial inputs rely on 'Weaver et al. (in preparation)' and other in-press/arXiv-only references. Please update all such references to their published/arXiv versions, or note that the companion values are available in the present paper's appendix.

Circularity Check

0 steps flagged

No circularity found; the paper's measurements are compared against external calibrations and simulations, and no target-derived quantity is fed back into the relations being tested.

full rationale

The derivation chain is self-contained. [OIII] 88 line fluxes are measured directly from ALMA data (Section 3.2) and converted to luminosities using lensing magnifications from independent models (Furtak et al. 2023). The comparison to the local [OIII]-SFR relation uses the external De Looze et al. (2014) calibration and SFRs from JWST/NIRSpec SED fitting (Sections 2.1 and 4.2), not SFRs derived from [OIII] 88 itself. The outflow mass (Equation 1) is the standard Carniani et al. (2015) formula applied to the measured broad-component luminosity, with a PyNeb emissivity and adopted Te/ne, plus a metallicity taken from a co-authored companion paper (Weaver et al., in preparation). The mass outflow rate combines this mass with the fitted broad-line width and a fiducial assumed size; none of these inputs is the theory being tested. The comparison of the resulting eta to FIRE-2 and ASTRAEUS uses external simulation predictions (Pandya et al. 2021; Ucci et al. 2023), not predictions calibrated on this target. The paper explicitly discloses the aperture-dependence of the broad-component significance (Appendix D, Figure 13: DeltaBIC=2.7 in the fiducial 0.8" aperture) and discusses merger alternatives (Section 4.3.5); this is an honest robustness caveat, not circularity. The only self-references provide SFR, stellar mass, metallicity, and measurement methodology, all independent of the ALMA [OIII] 88 data, so they do not make the argument circular.

Axiom & Free-Parameter Ledger

6 free parameters · 6 axioms · 0 invented entities

The central measurements (line fluxes, redshifts) rest only on standard ALMA calibration and Gaussian fitting. The headline outflow numbers, however, rest on several unconstrained microphysical choices (ne, C, Rout) and an interpretive assumption that the broad component is an outflow. The dust and SFR comparisons rely on SED assumptions and external SED fits, one unpublished (Weaver et al., in preparation). No new physical entities are introduced.

free parameters (6)
  • Outflow radius Rout = 0.3″ ± 0.1″ (≈1.4 kpc at z=8.51)
    Adopted from unresolved beam-deconvolved size; Mdot_out ∝ 1/Rout, so it directly sets the quoted 128 Msun/yr rate.
  • Electron density ne = 300 cm^-3
    Unconstrained by the ALMA data; Mout ∝ 1/ne, so the outflow mass scales inversely with this choice.
  • Clumping factor C = 1
    Assumed; true outflow mass would be lower by C if the gas is clumpy.
  • Electron temperature Te = 1.5×10^4 K
    Used for the [OIII]88 emissivity; claimed <10% effect over 1–2×10^4 K.
  • Dust temperature Tdust = 50 K
    Adopted for the modified-blackbody dust SED; sets all dust mass and obscured-SFR upper limits.
  • Assumed line FWHM for non-detections = 200 km/s
    Used to convert 3σ flux limits into luminosity limits for UHZ1 and UNCOVER-37126; broader lines would weaken the limits.
axioms (6)
  • standard math Standard ΛCDM cosmology with H0=70, Ωm=0.30, ΩΛ=0.70
    Adopted throughout for luminosity distances and angular scales; Section 1.
  • domain assumption [OIII]88 emissivity from PyNeb and outflow mass formula of Carniani et al. (2015) apply at z=8.5
    Used to convert broad-component luminosity into outflow mass; Section 4.3.2, Eq. 1.
  • domain assumption The local [OIII]88-SFR relation for dwarf galaxies (De Looze et al. 2014) is applicable at z>8
    Central comparison in Section 4.2; assumes no strong evolution in the line-to-SFR calibration.
  • domain assumption Modified blackbody dust SED with Tdust=50 K, β=2.0, κ0=10.41 cm^2/g at 1900 GHz, and CMB heating/contrast
    Converts continuum upper limits into dust masses, LIR, and obscured fractions; Section 4.1.
  • ad hoc to paper Broad [OIII]88 wing emission traces a compact ionized outflow rather than merger kinematics or an artifact
    Interpretive assumption for the paper's headline claim; Section 4.3.5 acknowledges the merger alternative.
  • domain assumption Lensing magnifications from Furtak et al. (2023) and adopted SED-fit SFRs/stellar masses are accurate
    All intrinsic luminosities and mass-loading factors divide by these external estimates; Section 2.1.

pith-pipeline@v1.3.0-alltime-deepseek · 35735 in / 14087 out tokens · 116274 ms · 2026-08-03T16:01:02.858588+00:00 · methodology

0 comments
read the original abstract

We present deep ALMA Band 7 observations of the [OIII] $88\mu$m line and underlying dust continuum emission in four UV-bright, gravitationally lensed (magnification $\mu = 1.4-3.8$), JWST-selected galaxies at $z = 8.5 - 10.3$, with observed magnitudes $-22.5 \lesssim M_\mathrm{UV} \lesssim -20.5$. [OIII] $88\mu$m is confidently detected in UNCOVER-10646 at $z=8.5080 \pm 0.0011$ ($15\sigma$) and DHZ1 at $z=9.3113 \pm 0.0006$ ($6\sigma$), with both being intrinsically luminous systems [$L_\text{[OIII]} = (1.1 - 1.6) \times 10^9\,L_\odot$] that follow the local [OIII]-SFR relation. [OIII] $88\mu$m remains undetected in the two $z>10$ targets, including in the $z=10.07$ X-ray AGN UHZ1, where we obtain a deep limit of $L_\text{[OIII]} < 6 \times 10^7\,L_\odot$. Dust emission is not detected in any individual source nor in a stack ($<3\sigma$). The high S/N [OIII] $88\mu$m detection in UNCOVER-10646 uniquely reveals an additional broad component ($\mathrm{FWHM} = 1366_{-329}^{+473}\,\mathrm{km/s}$; $\Delta\mathrm{BIC}\approx20$) indicative of an ionized outflow. We infer a high outflow rate of $\dot{M}_\mathrm{out} = 128_{-46}^{+80}\,M_\odot\,\mathrm{yr}^{-1}$, corresponding to a mass loading factor $\eta = \dot{M}_\mathrm{out}/\mathrm{SFR} = 2.9_{-1.0}^{+1.8}$ that matches or exceeds theoretical predictions and JWST-based studies of ionized outflows at high redshift. While high-resolution ALMA follow-up is required to confirm and spatially resolve the outflow, this first systematic study at $z>8$ highlights the unique diagnostic power of [OIII] $88\mu$m in characterizing galaxies in the early Universe.

Figures

Figures reproduced from arXiv: 2512.14486 by Akio K. Inoue, Andrea Ferrara, Andrea Pallottini, Andreas Faisst, Bovornpratch Vijarnwannaluk, Chayan Mondal, Chian-Chou Chen, Daniel P. Stark, Elisabete da Cunha, Hanae Inami, Hiddo S. B. Algera, Huub R\"ottgering, Jacqueline Hodge, John R. Weaver, Joris Witstok, Jorryt Matthee, Karin Cescon, Kasper Heintz, Laura Sommovigo, Livia Vallini, Lucie E. Rowland, Manuel Aravena, Mengyuan Xiao, Norbert Werner, Pascal A. Oesch, Paul van der Werf, Pratika Dayal, Renske Smit, Rodrigo Herrera-Camus, Romain Meyer, Rychard J. Bouwens, Sander Schouws, Seiji Fujimoto, Shoichiro Mizukoshi, Takuya Hashimoto, Themiya Nanayakkara, Tom J. L. C. Bakx, Yuma Sugahara.

Figure 1
Figure 1. Figure 1: — Absolute UV magnitude versus redshift (bottom x-axis) and Cosmic time (top axis) for our targets (large, colored mark￾ers) and other z > 8 galaxies targeted in [O iii]88 in the literature (white squares; Hashimoto et al. 2018; Tamura et al. 2019; Fuji￾moto et al. 2024a; Zavala et al. 2024; Carniani et al. 2025; Schouws et al. 2025b; Witstok et al. 2025). The larger, opaque markers show the apparent brigh… view at source ↗
Figure 2
Figure 2. Figure 2: — Naturally-weighted ALMA Band 7 dust continuum cutouts (3′′ × 3 ′′) of our four targets, overplotted on JWST/NIRCam F150W imaging. Contours are drawn at ±2, 3, 4, . . . × σ intervals, where σ is the continuum RMS. Negative contours are dashed. None of the sources are convincingly dust-detected, although UNCOVER-10646 shows a ∼ 2σ continuum signal in tapered imaging ( [PITH_FULL_IMAGE:figures/full_fig_p00… view at source ↗
Figure 3
Figure 3. Figure 3: — ALMA [O iii]88 cutouts (4′′ × 4 ′′) of our four targets, overplotted on JWST/NIRCam F444W imaging. For UNCOVER-10646 and DHZ1, where [O iii]88 emission is robustly detected, the moment-0 map spans all channels within 1.2× the line FWHM. No line emission is detected in UHZ1 and UNCOVER-37126, and the moment-0 map is collapsed across 200 km/s centered on the fiducial redshifts of z = 10.073 and z = 10.255,… view at source ↗
Figure 4
Figure 4. Figure 4: — Extracted 1D spectra showing the [O iii]88 detections for UNCOVER-10646 at z = 8.51 (left) and DHZ1 at z = 9.31 (right). A Gaussian fit to the spectra is shown through the red lines. The vertical shading shows the channels across which the moment-0 maps in [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: — Left: The [O iii]88-SFR relation of z > 6 galaxies. Our four z > 8.5 targets are overplotted as the colored symbols, while z > 8 (6 ≲ z < 8) galaxies compiled from the literature by Algera et al. (2025a) are shown as white (grey) squares. We show UNCOVER￾37126 as a semi-transparent symbol, given that its [O iii]88 line is possibly missed by our ALMA observations as a result of its uncertain, Lyman-break-… view at source ↗
Figure 6
Figure 6. Figure 6: — Naturally-weighted (top row) and briggs-weighted (middle row) moment-0 maps extracted across the shaded regions shown in the 1D spectra (bottom row). Contours are drawn at ±2, 3, 4, . . . × σ intervals, and the aperture (black circle) has a radius of 0.8 ′′. The grey and colored maps correspond to a region of (undetected) continuum emission and the [O iii]88 line, respectively. The orange shading represe… view at source ↗
Figure 7
Figure 7. Figure 7: — The mass loading factor η = M˙ out/SFR as a function of stellar mass. UNCOVER-10646, whose mass loading factor is de￾rived from the [O iii] 88 µm line, is shown as the large blue marker, and is compared to [O iii]5007-derived outflow rates at z ≈ 2 − 8 (Llerena et al. 2023; Carniani et al. 2024b; Xu et al. 2025). We also explicitly compare to the ALMA-detected z = 7.21 galaxy SXDF-NB1006-2, for which Ren… view at source ↗
Figure 8
Figure 8. Figure 8: — 1D spectra of UHZ1 (top) and UNCOVER-37126 (middle and bottom), extracted in 0.8 ′′ and 0.5 ′′-radii apertures, respectively. The expected location of the (undetected) [O iii]88 line based on the JWST/NIRSpec redshift of UHZ1 (z = 10.07; [PITH_FULL_IMAGE:figures/full_fig_p018_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: — ALMA dust continuum image (3′′ ×3 ′′) of UNCOVER-10646, tapered to ∼ 1.3 ′′ resolution. The tapered map shows a ∼ 2σ dust continuum signal co-spatial with the NIRCam F150W emission of the z = 8.51 galaxy (background greyscale). Given that UNCOVER￾10646 appears to host a powerful outflow (Section 4.3), its dust may be also efficiently expelled from the galaxy resulting in an extended dust reservoir that i… view at source ↗
Figure 10
Figure 10. Figure 10: — An alternative [O iii]88-SFR relation for our sample. Instead of showing the SFRs obtained from SED fitting as in [PITH_FULL_IMAGE:figures/full_fig_p020_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: — Moment-0 maps (left), CASA imfit Gaussian models (middle) and residuals (right) of the naturally-weighted (top) and Briggs-weighted (bottom) [O iii]88 emission of UNCOVER-10646. The cutouts span a 3′′ × 3 ′′ area and contours show emission at the ±2, 3, 4, . . .×σ level. The [O iii]88 line is not confidently resolved in the natural- and Briggs-weighted maps, suggesting the putative outflow in the 1D spe… view at source ↗
Figure 12
Figure 12. Figure 12: — Peak-pixel (blue) and aperture spectra of UNCOVER-10646, extracted from the cleaned (left) and dirty datacubes (right). Spectra are offset in steps of 2.5 mJy for visual clarity. The frequency ranges of the two concatenated spectral windows in the ALMA baseband containing the emission line are shown through the background grey and purple shading, respectively. High-velocity [O iii]88 emission is clearly… view at source ↗
Figure 13
Figure 13. Figure 13: — Single (left) and dual (right) Gaussian fits to the fiducial aperture-extracted spectrum of UNCOVER-10646 ( [PITH_FULL_IMAGE:figures/full_fig_p022_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: — Channel maps for the naturally-weighted, clean datacube of UNCOVER-10646, spanning a broad velocity range across its narrow and putative broad [O iii]88 emission in 50 km/s channels. Cutouts are 4′′ × 4 ′′, and our fiducial 0.8 ′′-radius extraction aperture is overplotted in white. The colorscale runs linearly between 0 − 5σ where σ is the RMS for a given channel. The contours start at ±1σ and increase … view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 7 Pith papers

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

  1. Multiphase images of a powerful supernova-driven wind in the early Universe

    astro-ph.GA 2026-06 unverdicted novelty 7.0

    Resolved multiphase observations reveal a supernova-driven wind in a z=5.3 galaxy removing gas at twice the star-formation rate, potentially quenching it within 100 Myr and matching local superwind properties.

  2. JWST absorption line spectroscopy with SPURS: ISM covering fractions and kinematics in individual galaxies at $z=5-9$

    astro-ph.GA 2026-06 unverdicted novelty 7.0

    JWST spectra of six z=5-9 galaxies show low-ionization covering fractions of 0.2-0.9 and diverse kinematics including blueshifted outflows, indicating heterogeneous multiphase ISM.

  3. Spatially resolved metallicity and ionization in the merging system Gz9p3 at z=9.3

    astro-ph.GA 2026-04 unverdicted novelty 7.0

    JWST data on Gz9p3 at z=9.3 reveal strong spatial variations in star formation rate, metallicity, ionization, and physical conditions between the central clump and tail of this merging system.

  4. A Massive Galaxy at the Edge of Feedback-Free Efficiency

    astro-ph.GA 2026-07 conditional novelty 6.0

    UNCOVER 3686 at z = 9.31 has a star-formation efficiency of 20–60%, 2–6 times above empirical models and consistent with the feedback-free starburst scenario.

  5. Chemical signatures from the first stars embedded in metal-poor gas in galaxies at cosmic dawn

    astro-ph.GA 2026-06 unverdicted novelty 6.0

    JWST absorption spectra of galaxies at z~8-9 show metal-poor gas with high [C/O] suggesting enrichment by Population III supernovae.

  6. PRISMS. U37126, a very blue, ISM-naked starburst at z=10.255 with nearly 100% Lyman continuum escape fraction

    astro-ph.GA 2026-02 conditional novelty 6.0

    U37126, a z=10.255 compact starburst, shows no optical nebular lines and a very blue UV slope, implying a Lyman-continuum escape fraction of ~94%.

  7. Grain-size evolution and rapid dust growth in high-redshift galaxies

    astro-ph.GA 2026-06 conditional novelty 5.0

    A multiphase ISM grain-size model with low supernova dust yield reproduces observed dust-to-stellar mass ratios and UV luminosity functions at z=7-12 by letting small grains seed rapid metal accretion.

Reference graph

Works this paper leans on

5 extracted references · cited by 7 Pith papers

  1. [1]

    Adams N. J. et al., 2024, ApJ, 965, 169 Aird J., Coil A. L., Georgakakis A., Nandra K., Barro G., P´ erez-Gonz´ alez P. G., 2015, MNRAS, 451, 1892 Akins H. B. et al., 2022, ApJ, 934, 64 Algera H. et al., 2025a, arXiv e-prints, arXiv:2509.16071 Algera H. S. B. et al., 2025b, arXiv e-prints, arXiv:2512.02320 Algera H. S. B. et al., 2024a, MNRAS, 533, 3098 A...

    arXiv 2024

  2. [2]

    plus a width of ±100 km/s is indicated through the vertical shading. The redshift of UNCOVER-37126 is less certain due to a lack of confident emission line detections in NIRSpec, and therefore we show the spectra extracted in both basebands, coveringz= 10.22−10.36 andz= 10.68−10.83, respectively. No high-significance feature likely to correspond to the [O...

    2025

  3. [5]

    If these slightly larger aperture 22 Fig

    This analysis reveals that for the Briggs-weighted (naturally-weighted) moment-0 map, an aperture extraction yields a higher line flux by a factor of 1.25±0.18 (1.32±0.15) compared to the peak-pixel flux. If these slightly larger aperture 22 Fig. 13.—Single (left) and dual (right) Gaussian fits to the fiducial aperture-extracted spectrum of UNCOVER-10646 ...

    1995

  4. [8]

    For the latter, we show both redshift intervals covered by the ALMA Band 7 observations, given that its spectroscopic redshift currently remains uncertain as no emission lines have been confidently detected in itsJWST/NIRSpec prism spectrum. 19 Fig. 9.—ALMA dust continuum image (3′′ ×3 ′′) of UNCOVER-10646, tapered to∼1.3 ′′ resolution. The tapered map sh...

    2023

  5. [11]

    This too suggests that UNCOVER-10646 is, at best, marginally resolved along the beam major axis

    This yields a size of (0.74 ′′ ±0.06 ′′)×(0.65 ′′ ±0.05 ′′), which corresponds to a beam-deconvolved extent of (0.37 ′′ ±0.14 ′′)× (0.31′′ ±0.21 ′′). This too suggests that UNCOVER-10646 is, at best, marginally resolved along the beam major axis. However, we deem the upper limit obtained from the Briggs-weighted map to be more robust, given its higher ang...

    2022