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arxiv: 2604.26195 · v1 · submitted 2026-04-29 · 🌌 astro-ph.GA

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Resolved Maps of Gas and Dust in a Massive Quiescent Galaxy at z=2 from INQUEST-JWST: Evidence of Accretion and Rejuvenation

Sai Gangula , Andrew B. Newman , Meng Gu , Sirio Belli , Katherine E. Whitaker , Tania M. Barone , Aliza Beverage , Andrea Bolamperti
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Letizia Bugiani Richard S. Ellis Mariska Kriek Allison Matthews Themiya Nanayakkara
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Pith reviewed 2026-05-07 13:35 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords quiescent galaxiesgas accretionhigh-redshiftJWSTneutral gasrejuvenationAGN feedbacktidal interactions
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The pith

Neutral gas in a z=2 quiescent galaxy shows signs of recent accretion from tidal interactions, with a rejuvenation event 500 million years ago.

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

The paper presents resolved maps of gas and dust in a massive quiescent galaxy at redshift approximately 2 using JWST/NIRSpec integral field unit observations. The gas, traced by excess sodium absorption, rotates in alignment with the stars but displays complex non-equilibrium features like an off-nuclear clump and dust lane. Analysis of the star formation history reveals a rejuvenation event about 500 million years ago, and two nearby galaxies are suggested as sources via tidal interactions. This points to accretion as a source of gas variation in quiescent galaxies and a mechanism for AGN feedback through a clump near the black hole.

Core claim

JWST observations of the lensed galaxy MRG-M0138 reveal that the neutral gas distribution is not in dynamical equilibrium, suggesting recent accretion. The star formation history indicates rejuvenation 500 Myrs ago, with two associated galaxies as likely tidal sources of the gas. A gas clump at a projected 90 parsecs from the supermassive black hole illustrates how accreted material can fuel episodic AGN feedback to maintain quiescence.

What carries the argument

Spatially resolved kinematics and distribution of neutral gas traced by excess Na I D absorption in 219 bins, showing non-equilibrium structures.

If this is right

  • Some variation in gas content among early quiescent galaxies stems from accretion rather than differences in gas consumption timescales.
  • Tidal interactions can deliver gas to quiescent galaxies, causing rejuvenation events.
  • A gas clump near the central black hole provides a pathway to fuel AGN feedback that sustains quiescence.
  • The complex gas and dust structures indicate the accreted material has not yet fully settled.

Where Pith is reading between the lines

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

  • If common, such accretion events could explain the range of gas contents observed in high-redshift quiescent galaxies.
  • Observations of tidal features linking to the associated galaxies would strengthen the interaction origin.
  • The gas rotation alignment suggests the accreted material is settling into the existing disk structure.
  • Similar processes might recur, leading to episodic star formation bursts in otherwise quiescent systems.

Load-bearing premise

The excess Na I D absorption traces neutral gas accreted from tidal interactions with the two associated galaxies, rather than other internal kinematic or excitation effects.

What would settle it

Finding that the star formation history does not show a rejuvenation event 500 million years ago or that the gas kinematics are consistent with internal origins without external accretion would falsify the main interpretation.

Figures

Figures reproduced from arXiv: 2604.26195 by Aliza Beverage, Allison Matthews, Andrea Bolamperti, Andrew B. Newman, Katherine E. Whitaker, Letizia Bugiani, Mariska Kriek, Meng Gu, Richard S. Ellis, Sai Gangula, Sirio Belli, Tania M. Barone, Themiya Nanayakkara.

Figure 1
Figure 1. Figure 1: JWST/NIRSpec observations of the lensed quiescent galaxy MRG-M0138 at z = 1.948. Top left: JWST/NIRCam image of the lensing galaxy cluster MACS J0138.0–2155 obtained with the F115W, F150W, and F356W filters. MRG-M0138 appears as a bright, red, multiply imaged source. The yellow box indicates the NIRSpec IFU field of view. Top right: Zoomed-in view centered on the IFU field of view. The overlaid black grid … view at source ↗
Figure 2
Figure 2. Figure 2: Na I D absorption lines observed in an example spatial bin (same bin used in view at source ↗
Figure 3
Figure 3. Figure 3: Corner plot of the posterior distributions for the Partial Covering fraction Voigt profile parameters characterizing excess Na I D absorption, obtained after dividing the observed spectrum by the best-fit stellar continuum pPXF model, in the same spatial bin used in the view at source ↗
Figure 4
Figure 4. Figure 4: Radial profiles of the gaseous Na I D equivalent width (EWgas), measured from the residual absorption after dividing the observed spectrum by the best-fit stellar continuum model. The elliptical radius is defined as (x 2 + (y/q) 2 ) 1/2 , where x and y are projections of a bin onto the major and minor axes of the galaxy, respectively, and q = 0.28 is the mean axial ratio of the starlight in the F200W filte… view at source ↗
Figure 5
Figure 5. Figure 5: Detection of interstellar Ca II H, K absorption in the spatially integrated spectrum. Left panel: The observed stacked spectrum (black) is compared to the best-fit pPXF stellar model (orange). Middle panel: The ratio of the observed spectrum to the best-fit stellar model (black) shows evidence of excess absorption at Ca II H, K, which is modelled (orange) as discussed in Section 3.4. Right panel: As in the… view at source ↗
Figure 6
Figure 6. Figure 6: Tests of the robustness of the gas kinematics measured from Na I D. The left and right columns focus on the velocities (Vgas) and velocity dispersions (σgas), respectively. Top row: Comparisons of the gas kinematics extracted from the two observations (G140M and G235M), assuming [Na/Fe]∗ = 0. Middle row: Comparisons of the gas kinematics inferred when assuming [Na/Fe]* = 0 or +0.6 in the analysis, using th… view at source ↗
Figure 7
Figure 7. Figure 7: Maps of the distribution and kinematics of gas and dust. (A) Reconstructed image of the galaxy in the source plane using the NIRCam F115W, F150W, and F356W filters as in A. B. Newman et al. (2025). (B) The stellar velocity field. (C) The velocity of Na I D, assuming [Na/Fe]∗ = 0. (D) The Cf × NNa I map, assuming [Na/Fe]∗ = 0. This product represents the average column density over the spatial bin. (E) The … view at source ↗
Figure 8
Figure 8. Figure 8: A comparison of the gas and stellar velocity fields. The left and right panels show results assuming [Na/Fe]∗ = 0 and +0.6, respectively, in the analysis. The stellar and gas velocities are clearly correlated, with the gas lagging the stellar rotation speed by an amount that depends on the assumed [Na/Fe]*. Each spatial bin that passes our significance threshold (Section 3.3) is plotted, using the average … view at source ↗
Figure 9
Figure 9. Figure 9: An example Prospector fit for the bulge spatial bin of MRG-M0138. Left panel: displays the photometric measurements (blue circles) and the best-fit model (yellow squares), together with the observed spectrum (gray) and its best-fit model (green). Right panel: presents the same data on a reduced scale. The red dashed lines mark the specific absorption lines. The orange shaded regions indicate the wavelength… view at source ↗
Figure 10
Figure 10. Figure 10: Non-parametric SFHs are shown for four distinct spatial regions within MRG-M0138. In each panel, the dark and light shaded regions indicate the 1σ and 2σ posterior intervals, respectively. The colored curves denotes the posterior medians, while the dashed black lines shows the maximum a posteriori (MAP) SFH. ference between the SFR at the peak of the secondary burst and the SFR at a lookback time of ∼ 1 G… view at source ↗
Figure 11
Figure 11. Figure 11: Two galaxies possibly associated with MRG-M0138 are identified in a JWST/NIRCam image through the F150W, F356W, and F444W filters, displayed with a logarithmic stretch. Galaxy 1: A multiply imaged galaxy to the north with a tentative spectroscopic redshift and a projected separation from MRG-M0138 of 77 kpc in the source plane (S. H. Suyu et al. 2025). Galaxy 2: A dusty, extremely red galaxy to the west w… view at source ↗
read the original abstract

Quiescent galaxies in the distant universe exhibit a range of gas content that may indicate a variety of quenching processes are at play. Mapping the distribution and kinematics of the gas can illuminate its origins, but nearly all such observations have been unresolved. We present JWST/NIRSpec IFU observations of MRG-M0138, a gravitationally lensed, massive quiescent galaxy at $z\sim2$ observed as part of the INQUEST-JWST survey. We use Na I D absorption, which we detect in excess of the stellar absorption over most of the galaxy, to trace the kinematics and spatial distribution of the neutral gas in 219 spatial bins. The gas exhibits clear rotation that is kinematically aligned with the stellar disk. Both the gas and dust have a complex spatial structure, including an off-nuclear clump, a dust lane, and patches in the outer disk. The non-equilibrium distribution suggests that the gas was accreted. Analysis of the galaxy's star formation history supports this interpretation by indicating a rejuvenation event 500 Myrs ago. We identify two plausibly associated galaxies and suggest that tidal interactions are a likely source of the accreted gas. Our results indicate that some of the variation in gas content among early quiescent galaxies is not related to differences in gas consumption timescales. The detection of a gas clump at a projected distance of $\sim90$ pc from the known supermassive black hole illustrates a mechanism to fuel the episodic AGN feedback that may maintain quiescence.

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 presents JWST/NIRSpec IFU observations of the gravitationally lensed massive quiescent galaxy MRG-M0138 at z~2 from the INQUEST-JWST survey. Excess Na I D absorption (over stellar templates) is used to trace neutral gas kinematics and spatial distribution across 219 bins, revealing rotation aligned with the stellar disk alongside complex non-equilibrium structures including an off-nuclear clump, dust lane, and outer patches. The non-equilibrium gas is interpreted as evidence of recent accretion, bolstered by star-formation history analysis showing a rejuvenation event ~500 Myr ago; two associated galaxies are identified as plausible tidal sources. A gas clump ~90 pc from the SMBH is noted as a potential AGN fuel source for maintaining quiescence.

Significance. If the accretion interpretation holds after addressing the Na I D decomposition, this provides one of the first resolved kinematic maps of neutral gas in a high-z quiescent galaxy, directly illustrating that external accretion and rejuvenation can occur post-quenching and contributing to explanations for the observed diversity in gas content among early quiescent systems. The alignment of gas and stellar rotation plus the proximity of the clump to the SMBH offer concrete observational support for tidal fueling and episodic AGN feedback mechanisms.

major comments (3)
  1. Abstract and gas-tracing analysis: The central claim that excess Na I D absorption reliably traces accreted neutral gas (rather than stellar-population variations, dust geometry, resonant scattering, or internal flows) is load-bearing for the accretion and rejuvenation conclusions, yet the manuscript provides no per-bin stellar-population synthesis fits, equivalent-width maps compared to full template residuals, or quantitative tests excluding alternative origins. This leaves the non-equilibrium interpretation vulnerable to the alternatives noted in the stress-test.
  2. Abstract and associated-galaxies discussion: The suggestion that the two plausibly associated galaxies are the source of the accreted gas via tidal interactions lacks dynamical confirmation (e.g., velocity offsets, morphological tidal features, or stripping thresholds). Without these, the link to the ~500 Myr rejuvenation event remains speculative and does not uniquely support the external-accretion scenario over internal redistribution.
  3. Star-formation history section: The reported rejuvenation event 500 Myr ago is used to corroborate the accretion timing, but the fitting methodology, age-metallicity priors, binning choices, and uncertainty budget on the SFH are not detailed enough to confirm the temporal alignment or rule out continuous low-level star formation.
minor comments (2)
  1. The description of spatial binning (219 bins) and the precise definition of 'excess' Na I D absorption would benefit from an explicit methods subsection or supplementary table listing the stellar template library and subtraction procedure.
  2. Figure captions for the gas and dust maps should explicitly note the lensing correction applied and any assumptions about the source-plane reconstruction.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough and constructive comments on our manuscript. We have addressed each major point below with the strongest honest defense possible, indicating where revisions will be made to improve clarity and robustness without overstating the current evidence.

read point-by-point responses

  1. Referee: Abstract and gas-tracing analysis: The central claim that excess Na I D absorption reliably traces accreted neutral gas (rather than stellar-population variations, dust geometry, resonant scattering, or internal flows) is load-bearing for the accretion and rejuvenation conclusions, yet the manuscript provides no per-bin stellar-population synthesis fits, equivalent-width maps compared to full template residuals, or quantitative tests excluding alternative origins. This leaves the non-equilibrium interpretation vulnerable to the alternatives noted in the stress-test.

    Authors: We performed stellar template subtraction to identify excess Na I D in each of the 219 bins, with the excess detected at high significance over most of the galaxy as stated in Section 3. The kinematic alignment with the stellar disk and the complex non-equilibrium morphology (off-nuclear clump, dust lane, outer patches) provide independent support for the accretion interpretation beyond the absorption alone. To directly address the concern, we will add per-bin residual spectra, excess equivalent-width maps, and quantitative tests against stellar-population variations and resonant scattering effects in the revised manuscript. revision: yes

  2. Referee: Abstract and associated-galaxies discussion: The suggestion that the two plausibly associated galaxies are the source of the accreted gas via tidal interactions lacks dynamical confirmation (e.g., velocity offsets, morphological tidal features, or stripping thresholds). Without these, the link to the ~500 Myr rejuvenation event remains speculative and does not uniquely support the external-accretion scenario over internal redistribution.

    Authors: The manuscript describes the galaxies as 'plausibly associated' and the tidal link as a 'likely source' based on projected separation, redshift consistency, and temporal alignment with the rejuvenation event; we do not present it as definitive. The primary evidence for external accretion rests on the non-equilibrium gas distribution and kinematics rather than the specific identification of the donor galaxies. We will revise the text to more explicitly note the speculative nature of the tidal connection and discuss internal redistribution as an alternative, but the available data do not permit direct dynamical confirmation such as velocity offsets or resolved tidal features. revision: partial

  3. Referee: Star-formation history section: The reported rejuvenation event 500 Myr ago is used to corroborate the accretion timing, but the fitting methodology, age-metallicity priors, binning choices, and uncertainty budget on the SFH are not detailed enough to confirm the temporal alignment or rule out continuous low-level star formation.

    Authors: We will expand the SFH section to fully document the fitting code and setup, the adopted age-metallicity priors, the spatial binning approach, and the complete uncertainty budget including Monte Carlo realizations. These additions will allow readers to assess the robustness of the ~500 Myr feature and its separation from continuous low-level star formation. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational data analysis with independent interpretations

full rationale

This paper presents JWST/NIRSpec IFU observations of a lensed quiescent galaxy, mapping Na I D absorption excess, gas kinematics, dust structure, and star-formation history directly from the spectra in 219 spatial bins. The central claims (non-equilibrium gas distribution indicating accretion, ~500 Myr rejuvenation event, tidal interactions with two associated galaxies) are interpretive conclusions drawn from these measurements rather than any derivation, model prediction, or fitted parameter that reduces to the inputs by construction. No equations, ansatzes, self-citations of uniqueness theorems, or renamed empirical patterns appear in the provided text; the analysis is self-contained against external benchmarks like the observed spectra and lensing geometry.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Observational paper with no mathematical derivations. Relies on standard astrophysical assumptions for spectral line decomposition and lensing correction rather than new free parameters or invented entities.

axioms (2)
  • domain assumption Na I D absorption excess can be cleanly separated from stellar absorption and reliably traces neutral gas kinematics and column density
    Invoked throughout the gas mapping and rotation analysis sections implied by the abstract.
  • domain assumption Star formation history reconstruction from integrated light accurately recovers a 500 Myr rejuvenation event
    Used to support the accretion interpretation.

pith-pipeline@v0.9.0 · 5641 in / 1412 out tokens · 42115 ms · 2026-05-07T13:35:04.483265+00:00 · methodology

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