A model to mini-quench early galaxies by balancing stellar feedback and gas accretion

Judah Luberto; Steven R. Furlanetto

REVIEW

A model to mini-quench early galaxies by balancing stellar feedback and gas accretion

Judah Luberto, Steven R. Furlanetto

Astrophysics of Galaxies · Submitted 16 Sep 2026 · 101 references

Pith's verdict: Novel inclusion of accretion blocking by outflow shell, but the mechanism's feasibility hinges on an unverified premise about shell formation that the paper does not quantify.

T0 · AI review

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arXiv ID2609.19265 (version 1)

Pith IDLH6U6XZG, Pith's permanent record of this paper and its review

CitationJudah Luberto, Steven R. Furlanetto. "A model to mini-quench early galaxies by balancing stellar feedback and gas accretion." arXiv:2609.19265 (2026). https://pith.science/paper/LH6U6XZG

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Editor's note

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This paper does one genuinely new thing: it lets the outflowing shell physically block accreting gas from reaching the star-forming region, and works through the consequences analytically. Previous models treated the shell as independent of accretion, so this is a clear step forward. The derivation is clean, the assumptions are stated, and the match to observed quenching masses and timescales is plausible over a range of parameters.

The soft spot is the one the stress-test flags. The whole mechanism depends on feedback assembling the ISM into a thin, coherent shell at R0 with f_cover=1 before Eq. 2.21 can act as an accretion barrier. The authors acknowledge that the diffuse gas 'will take time to evolve' into such a shell (Sec. 2.9), but the only parameter absorbing that assembly cost is epsilon_k, which they set to 1. That means every supernova contributes fully to driving exactly the shell the model needs. If shell assembly is inefficient, or if RT/KH instabilities (Sec. 5.1, tau_RT ~ 60 Myr) disrupt it before t_quench elapses, the mechanism fails. This matters because the mass limit (Eq. 3.13), quenching-time curves (Fig. 5), and duty-cycle fractions (Fig. 9) all inherit this assumed initial condition. The authors discuss instabilities as a possible ceiling on t_quench, but that discussion is qualitative—it does not protect the central claim that feedback can create such a shell in the first place.

That said, the paper is transparent about its limitations. It does not overclaim. The parameter study is honest, and the filamentary accretion section shows when the model breaks down. The core idea is worth taking seriously, even if the missing step (shell formation) is load-bearing.

Who is this for? Theorists working on bursty star formation and early galaxy quenching. It deserves a serious referee because it presents a testable framework that sharpens the debate—even if the referee ends up demanding a demonstration that shells actually form. I would accept review on this. I would not cite it for my own work yet (I'd want to see the shell formation question addressed), but I'd bring it to reading group to discuss that exact issue.

Referee report

Significance

If the central claim holds, the paper provides a physically motivated explanation for the population of low-mass, temporarily quiescent galaxies discovered by JWST at z~4–8. The novel element is the explicit coupling between the outflowing shell and the accreting gas, which earlier analytic models neglected. The model successfully reproduces the observed stellar masses and quenching timescales of a few galaxies with plausible parameter values. However, because the model is highly simplified (thin shell, spherical symmetry, instantaneous shell formation), its predictive power is limited; a rigorous test would require hydrodynamical simulations. Nevertheless, the work identifies key parameters that govern mini-quenching and makes falsifiable predictions about the covering fraction of accreting gas and the redshift dependence of quenching times. It is a useful step toward understanding episodic star formation at high redshift.

Major objections (3)

[Section 2.9, Eq. (2.21)] The model assumes that the galaxy's gas reservoir instantaneously forms a thin, coherent spherical shell at radius R0 = kappa r_vir and that this shell interacts perfectly with all accreting gas (f_cover = 1 for isotropic accretion). The authors acknowledge in Section 2.9 that 'the gas reservoir will take time to evolve from its diffuse state... into a thin shell,' but the only allowance for the energy spent during this assembly is the parameter epsilon_k, which is set to 1 (i.e., all SN energy is available to drive the already-formed shell). No estimate is provided for the assembly timescale or the energy losses incurred while gathering the diffuse ISM into a shell. If assembly is slow or inefficient, the effective feedback momentum available to halt accretion may be much smaller than assumed. This is a load-bearing assumption for the entire quenching picture. The authors should either estimate the shell-formation timescale and show it is shorter than the star-formation and accretion timescales, or treat the assembly efficiency as an additional free parameter and explore its sensitivity.
[Section 5.1, Eq. (5.1)] The discussion of Rayleigh-Taylor and Kelvin-Helmholtz instabilities estimates an instability growth timescale tau_RT ~ 60 Myr at z=6, which is comparable to or shorter than the predicted quenching times in many models (e.g., t_quench > 100 Myr for low-mass halos in Fig. 5). The authors note that instabilities 'can help limit the extremely long quenching periods' but do not incorporate any disruption into the model's predictions. The central claim that feedback can prevent accretion relies on the shell remaining intact over the quenching interval. If instabilities fragment the shell on a timescale << t_quench, accreting gas could reach the star-forming region and resume star formation, invalidating the quenching mechanism. The paper should at minimum quantify how the quenching times and mass limits would change if the shell disrupts after tau_RT, or provide a stronger argument (e.g., based on simulations or specific timescale comparisons) that the shell survives.
[Section 4.1, Fig. 5; Section 2.7] The star-formation efficiency f* and the wind efficiency epsilon_k are degenerate in the feedback force (both scale linearly in the supernova pressure term). The paper sets epsilon_k = 1 and explores f* = 0.001–0.1, but notes in Section 4.1 that 'if epsilon_k = 0.1, the required f* values would be 10 times larger.' Since epsilon_k is observationally unconstrained and likely much less than unity (some SN energy is radiated or lost to turbulence), the plausible range for the effective feedback strength is wide. The paper should systematically explore the (f*, epsilon_k) plane and show contours of quenching mass and timescale, rather than only varying f* with epsilon_k fixed. This would give a more honest assessment of the model's predictive power.

Minor objections (5)

[General] The notation m* for the stellar mass formed in a single episode and m_{*,tot} for the total stellar mass is potentially confusing, especially in the abstract and introduction. Consider using a subscript (e.g., m*_ep, m*_tot) consistently.
[Figure 5, caption and text] The right panels convert halo mass to stellar mass using a range of ~f* = [0.01, 0.1], but the text (Section 4.1) says 'We plot each curve (except f* = 0.1) with a range of ~f* = [0.01,0.1].' The figure shows bands for only the f*=0.001 and f*=0.01 curves; the f*=0.1 curve appears as a single line. Clarify whether the f*=0.1 curve also has a range, and explain the choice of ~f* relative to the instantaneous f*.
[Section 3.3, Eq. (3.12)] The analytic expression for m_h,max is derived for z=6 and a Chabrier-like IMF. The text should explicitly state the redshift and IMF assumed, and note that Figure 4 shows numerical results for other redshifts. The range of validity of Eq. (3.12) should be given (e.g., t_SF < t_SN or > t_SN).
[Section 4.4, Fig. 8] The figure shows that for f_cover = 0.005, the quenching timescale is zero (no quenching) for all halo masses. The text (Section 4.4) says 'mini-quenching becomes impossible.' This is an important result but it depends on the assumed filament radius (0.08 r_vir from Mandelker+2018). The uncertainty in the filament opening angle should be discussed: e.g., would a less conservative estimate (larger solid angle) allow quenching?
[Section 2.6.1, Eq. (2.9)] The UV luminosity per stellar mass is computed using a simple stellar model. The authors note that their model produces about half the ionizing photons of starburst99 for a Chabrier-like IMF. This discrepancy should be quantified further: if the UV feedback is subdominant anyway (Fig. 3), the impact on the results is minor, but a brief mention of the uncertainty in stellar models would be helpful.

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The paper

The paper claims

Stellar feedback can drive mini-quenching in early galaxies by blocking gas accretion, a model shows.

The reading

This paper presents a model to explain the surprising population of 'mini-quenched' galaxies discovered by JWST at redshifts 3–9. These galaxies show extremely low star formation over tens of millions of years, but are not permanently quenched. The model shows that stellar feedback, primarily from supernovae, can drive a thin shell of gas outward from the star-forming region. The key novelty is that this shell intercepts and prevents incoming accreting gas from reaching the galaxy, choking off the fuel supply. With plausible parameters, the model reproduces observed stellar masses up to about $10^{10}$ solar masses and quenching timescales of tens of Myr, though it predicts overly long quenching in low-mass halos unless accretion is filamentary or instabilities break the shell.

What carries the argument

The central object is a thin spherical shell of gas at the edge of the star-forming region, whose motion is governed by a force equation (Equation 2.21) that balances outward feedback forces (supernova pressure, radiation pressure from UV and Lyα) against inward gravitational and accretion-induced ram pressure forces. The key identity is that the shell both carries the outflowing gas and interacts with accreting gas through a covering fraction f_cover, linking feedback and accretion for the first time in an analytic model. The maximum halo mass for mini-quenching is derived by equating the dominant outward force (supernovae) to the dominant inward force (gravity for isotropic accretion, accretion ram pressure for filamentary accretion).

Extended reading notes

Core claim

The paper establishes that stellar feedback alone can cause temporary quenching episodes in early galaxies as massive as observed mini-quenched galaxies, provided that the outflowing gas shell physically blocks accreting gas. Using a thin-shell force equation that includes gravity, ram pressure from accretion, and feedback from supernovae (dominant), UV radiation, and Lyα photons, the model finds that galaxies with isotropic accretion and star-formation efficiencies near 0.01 can quench for tens of Myr in halos up to ~$10^{11}$–$10^{12}$ solar masses. This corresponds to total stellar masses up to ~$10^{10}$ solar masses, matching JWST detections. The paper further shows that filamentary accretion reduces both the maximum quenchable mass and the quenching timescale, potentially resolving the overly long quenching times predicted for low-mass halos, but very narrow filaments make mini-quenching impossible.

Load-bearing premise

The model assumes that the galaxy's gas reservoir instantly forms a thin spherical shell at the edge of the star-forming region, and that this shell perfectly covers all incoming gas (f_cover=1 for isotropic accretion).

Editorial extensions

If this is right

If correct, mini-quenching is a natural consequence of bursty star formation in early galaxies, not requiring AGN or environmental effects for masses up to ~10^10 M_sun.
The model predicts distinct quenching timescales for field galaxies (accreting isotropically, longer quenching) versus galaxies in the cosmic web (filamentary accretion, shorter quenching), which future surveys can test statistically.
The estimated fraction of galaxies undergoing mini-quenching becomes large (>50%) for isotropic accretion but drops sharply for narrow filaments, so observed quenching fractions will constrain the typical accretion geometry at z~6.
The model implies that metals from supernovae can escape the galaxy in halos below ~10^11 M_sun, enriching the intergalactic medium, but that the gas remains bound and will re-accrete, potentially triggering starbursts after quenching ends.

Reading between the lines

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

The paper’s result that mini-quenching requires relatively wide filaments (covering fractions >~0.05) suggests that if future observations show many mini-quenched galaxies in environments that simulations predict have narrow filaments, then either the feedback mechanism is stronger than modeled (e.g., AGN contribution) or the filament geometry is more complex.
The long quenching timescales for low-mass halos ( >100 Myr) in the isotropic case imply that such galaxies should be readily observable if they exist; the fact that few are seen may indicate that instabilities (Rayleigh-Taylor, as estimated in Section 5.1) limit quenching to ~30–60 Myr, providing an indirect test of shell stability.
The model can be extended to later redshifts (z~3) where quenching timescales are longer, potentially explaining the transition to permanent quenching as galaxies grow above the mass threshold where feedback no longer overcomes gravity and accretion.

Original abstract

The James Webb Space Telescope (JWST) has discovered a population of low-mass, early galaxies with very low levels of star formation over tens of Myr. These "mini-quenched" galaxies were one of the many surprises from JWST and still require a robust explanation. We seek to explain a few important properties of these galaxies, namely the timescales governing their star formation and quenching. We use a simple model that pairs stellar feedback with the forces binding gas to a $z \sim 6$ galaxy, and with plausible parameter choices, this model produces mini-quenching in galaxies approximately as large as observed mini-quenched galaxies -- up to total stellar masses of $\sim 10^{10} M_{\odot}$. In our model, the ejected interstellar gas forms into a spherical shell that expands outward during quenching. Our novel improvement is allowing this expanding shell to prevent accreting gas from falling in, in contrast to other models whose shells do not interact with accreting gas. Using our model, if a galaxy accretes isotropically, we find that stellar feedback can reproduce observed timescales of mini-quenching with plausible galaxy-formation parameter values. However, at low halo masses, the quenching timescale of our model is too long ($> 100$ Myr). A potential solution for a long quenching time is for the galaxy to accrete via filaments, in which case only a portion of the shell interacts with the accreting gas and the quenching timescale decreases to more accepted values. However, the ram pressure from feedback cannot stop filaments with very small opening angles, as occur in some halo formation models, making mini-quenching impossible. Finally, we use this model to estimate the fraction of galaxies undergoing mini-quenching, finding that it can be large.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 8,418 input tokens.

What the abstract itself states, as probabilities: claims first 0.09 · states limitation 0.98 · human participants 0.01 · controlled comparison 0.14 · randomized assignment 0.01 · states quantitative result 0.97 · compares with prior results 0.71 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

The James Webb Space Telescope (JWST) has discovered a population of low-mass, early galaxies with very low levels of star formation over tens of Myr. These "mini-quenched" galaxies were one of the many surprises from JWST and still require a robust explanation. We seek to explain a few important properties of these galaxies, namely the timescales governing their star formation and quenching. We use a simple model that pairs stellar feedback with the forces binding gas to a $z \sim 6$ galaxy, and with plausible parameter choices, this model produces mini-quenching in galaxies approximately as large as observed mini-quenched galaxies -- up to total stellar masses of $\sim 10^{10} M_{\odot}$. In our model, the ejected interstellar gas forms into a spherical shell that expands outward during quenching. Our novel improvement is allowing this expanding shell to prevent accreting gas from falling in, in contrast to other models whose shells do not interact with accreting gas. Using our model, if a galaxy accretes isotropically, we find that stellar feedback can reproduce observed timescales of mini-quenching with plausible galaxy-formation parameter values. However, at low halo masses, the quenching timescale of our model is too long ($> 100$ Myr). A potential solution for a long quenching time is for the galaxy to accrete via filaments, in which case only a portion of the shell interacts with the accreting gas and the quenching timescale decreases to more accepted values. However, the ram pressure from feedback cannot stop filaments with very small opening angles, as occur in some halo formation models, making mini-quenching impossible. Finally, we use this model to estimate the fraction of galaxies undergoing mini-quenching, finding that it can be large.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	The James Webb Space Telescope (JWST) has discovered a population of low-mass, early galaxies with very low levels of star formation over tens of Myr.	background 1.00	0.10	0.02	asserted 1.00
s1	These "mini-quenched" galaxies were one of the many surprises from JWST and still require a robust explanation.	background 0.61	0.05	0.02	asserted 0.99
s2	We seek to explain a few important properties of these galaxies, namely the timescales governing their star formation and quenching.	contribution 0.42	0.38	0.03	asserted 0.71
s3	We use a simple model that pairs stellar feedback with the forces binding gas to a $z \sim 6$ galaxy, and with plausible parameter choices, this model produces mini-quenching in galaxies approximately as large as observed mini-quenched galaxies -- up to total stellar masses of $\sim 10^{10} M_{\odot}$.	result 0.66	0.94	0.55	asserted 0.92
s4	In our model, the ejected interstellar gas forms into a spherical shell that expands outward during quenching.	method 0.98	0.69	0.04	asserted 1.00
s5	Our novel improvement is allowing this expanding shell to prevent accreting gas from falling in, in contrast to other models whose shells do not interact with accreting gas.	contribution 0.96	0.89	0.10	asserted 1.00
s6	Using our model, if a galaxy accretes isotropically, we find that stellar feedback can reproduce observed timescales of mini-quenching with plausible galaxy-formation parameter values.	result 1.00	0.96	0.40	asserted 1.00
s7	However, at low halo masses, the quenching timescale of our model is too long ($> 100$ Myr).	limitation 0.97	0.94	0.04	asserted 1.00
s8	A potential solution for a long quenching time is for the galaxy to accrete via filaments, in which case only a portion of the shell interacts with the accreting gas and the quenching timescale decreases to more accepted values.	interpretation 0.60	0.54	0.09	hedged possibility 0.96
s9	However, the ram pressure from feedback cannot stop filaments with very small opening angles, as occur in some halo formation models, making mini-quenching impossible.	limitation 0.93	0.66	0.06	asserted 0.98
s10	Finally, we use this model to estimate the fraction of galaxies undergoing mini-quenching, finding that it can be large.	result 1.00	0.95	0.21	asserted 0.70

What kind of paper the classifier reports this is: theoretical result 0.94 · evidence from simulation or computation 0.80.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

References

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Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

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