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arxiv: 2606.04081 · v1 · pith:FT5TF6GKnew · submitted 2026-06-02 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.HE

The role of major mergers in triggering super-Eddington accretion

Riccardo Caleno , Tommaso Zana , Raffaella Schneider , Alessandro Lupi , Pedro R. Capelo , Lucio Mayer , Alessandro Trinca , Rosa Valiante
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Marta Volonteri
This is my paper

Pith reviewed 2026-06-28 08:56 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.HE
keywords black hole accretionsuper-Eddingtonmajor mergershigh-redshift galaxiescosmological simulationsblack hole feedbackgalaxy formation
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The pith

Major mergers at z~11 do not trigger sustained super-Eddington black hole accretion when feedback operates.

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

The paper runs high-resolution cosmological zoom-in simulations of a major merger between two halos each around 10^9 solar masses at redshift near 11. It tests whether the merger can drive gas inflows that produce sustained super-Eddington accretion onto the central black holes. The simulations include physically motivated seeding and feedback models that cover advection-dominated, sub-Eddington, and super-Eddington regimes. With feedback active, the inflows occur but do not yield substantial or sustained high accretion rates. Only when feedback is switched off entirely do post-merger super-Eddington episodes appear, and kinetic feedback proves the dominant regulator of growth.

Core claim

In these simulations the merger drives gas inflows toward the centers yet produces no substantial enhancement of the black hole accretion rate. Sustained super-Eddington episodes occur only immediately after black hole seeding or when all feedback is disabled. Kinetic feedback is the primary channel that limits black hole growth across the explored accretion regimes.

What carries the argument

Cosmological zoom-in simulations with black hole seeding and combined radiative plus kinetic feedback prescriptions applied across ADAF, sub-Eddington, and super-Eddington regimes.

If this is right

  • Feedback suppresses gas accretion efficiently enough to prevent substantial black hole growth in these halos.
  • Post-merger super-Eddington accretion requires feedback to be absent.
  • Kinetic feedback dominates regulation of growth over radiative channels.
  • The only notable super-Eddington episodes happen right after seeding rather than during the merger.

Where Pith is reading between the lines

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

  • Mechanisms other than major mergers are likely required to explain the rapid early black hole growth inferred from JWST data.
  • Results underscore that accurate feedback modeling is essential for predicting black hole populations in the first galaxies.
  • Running equivalent simulations for higher-mass halos or different redshifts could reveal whether mergers matter more in other regimes.

Load-bearing premise

The chosen black hole seeding and feedback prescriptions correctly capture the main physical processes that control gas supply to the black holes in these low-mass halos near redshift 11.

What would settle it

A simulation with the same initial conditions but an alternative feedback implementation that produces sustained super-Eddington accretion after the merger completes.

Figures

Figures reproduced from arXiv: 2606.04081 by Alessandro Lupi, Alessandro Trinca, Lucio Mayer, Marta Volonteri, Pedro R. Capelo, Raffaella Schneider, Riccardo Caleno, Rosa Valiante, Tommaso Zana.

Figure 1
Figure 1. Figure 1: Zoom-in DM density snapshots at the moment of the merger. Every zoomed region represents a di [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of the DM (upper panel) and stellar (lower [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Comparison amongst three different seeding prescriptions: the simulation with M⋆ threshold (left-hand panels), the run with Mgas threshold (middle panels), and the ad hoc seed run (right-hand panels). In the upper plots we show the evolution of the BH mass, and in the lower panel the accretion rate in terms of the Eddington rate. The colours have been specifically chosen to represent a specific run, as in … view at source ↗
Figure 4
Figure 4. Figure 4: Comparison between ad hoc seed and ad hoc seed noFB runs. We show the evolution of BH masses and the BH accretion [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Comparison of the initial SE episodes for the BHs in [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Comparison between the extended runs. We show, again, the evolution of BH masses and the BH accretion rates as in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Evolution of the BH mass [panel (a)] and accretion rate of the most massive BH [panel (b)] as a function of cosmic time for [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Surface gas density maps of Run5 during the merger [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
read the original abstract

JWST observations have opened a new era in the exploration of the high-redshift Universe, revealing black holes (BHs) with masses of several million solar masses already at $z>8$, challenging our understanding of their growth mechanisms. In this context, super-Eddington (SE) accretion has emerged as a promising solution and has been widely adopted in both numerical simulations and semi-analytical models. In this work, we investigate whether a major merger between two relatively low-mass halos ($M_{\rm halo}\sim10^9\,\mathrm{M_\odot}$) at high redshift can trigger episodes of sustained SE accretion, with particular focus on the role of BH feedback. We employ state-of-the-art, high-resolution cosmological zoom-in simulations of a major merger at $z\sim11$. We explore different prescriptions for BH seeding and feedback, including physically motivated radiative and kinetic models (winds and jets) across the three main accretion regimes: advection-dominated accretion flows (ADAF), radiatively efficient sub-Eddington accretion, and SE accretion. For the relatively low-mass halos studied here, our feedback prescription efficiently suppresses gas accretion, preventing substantial BH growth. We find that, although the merger drives gas inflows towards the central regions, this is not sufficient to trigger sustained SE accretion. Post-merger SE accretion episodes are observed only when BH feedback is entirely switched off. Amongst the feedback channels considered, kinetic feedback is the primary mechanism regulating BH growth. Moreover, the only significant SE accretion episodes occur immediately after BH seeding, while the merger itself does not produce a substantial enhancement of the accretion rate.

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 investigates whether major mergers between low-mass halos (~10^9 M_sun) at z~11 can trigger sustained super-Eddington (SE) accretion onto black holes using high-resolution cosmological zoom-in simulations. The authors explore different BH seeding and feedback prescriptions, including radiative and kinetic models across ADAF, sub-Eddington, and SE regimes. They conclude that BH feedback efficiently suppresses gas accretion, preventing substantial BH growth, and that the merger-driven inflows are not sufficient to trigger sustained SE accretion. SE episodes occur only when feedback is entirely switched off, with kinetic feedback as the primary regulator, and significant SE accretion mainly immediately after BH seeding.

Significance. If the results hold, this work would suggest that major mergers do not play a significant role in triggering the SE accretion required to explain the massive BHs observed at high redshift by JWST. The systematic exploration of multiple feedback channels and accretion regimes provides a useful benchmark for sub-grid physics in simulations of early BH growth. The finding that feedback suppresses accretion in these low-mass systems highlights the sensitivity of high-z BH evolution to modeling choices.

major comments (3)
  1. [Abstract and Results] Abstract and Results: The central claim that the merger does not produce a substantial enhancement of the accretion rate and that post-merger SE episodes occur only when feedback is off lacks accompanying quantitative accretion-rate histories or time-resolved plots demonstrating the lack of enhancement during the merger phase. Without these, the support for the claim cannot be fully assessed.
  2. [Methods (feedback prescriptions)] Methods (feedback prescriptions): The conclusion relies on the specific choices for radiative and kinetic feedback efficiencies in the SE regime. No section quantifies the sensitivity of the results to plausible variations in these parameters (e.g., wind coupling or jet efficiency) for 10^9 M_sun halos at z~11, which is a load-bearing assumption given the limited observational constraints at these redshifts.
  3. [Simulation setup] Simulation setup: No resolution tests, convergence checks, or comparisons with lower-resolution runs are reported, which is essential for validating the gas inflow and accretion dynamics in zoom-in simulations of this type.
minor comments (2)
  1. [Notation] Ensure consistent use of M_halo and M_{\rm halo} throughout the text.
  2. [Figures] Figure captions should explicitly state the feedback configuration for each panel to aid interpretation.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their careful and constructive review. Their comments highlight areas where the presentation can be strengthened, and we address each point below.

read point-by-point responses

  1. Referee: [Abstract and Results] Abstract and Results: The central claim that the merger does not produce a substantial enhancement of the accretion rate and that post-merger SE episodes occur only when feedback is off lacks accompanying quantitative accretion-rate histories or time-resolved plots demonstrating the lack of enhancement during the merger phase. Without these, the support for the claim cannot be fully assessed.

    Authors: The manuscript already presents time-resolved accretion-rate histories in Section 3 (Figure 3), with the merger epoch explicitly marked and separate curves for each feedback prescription. These show no sustained post-merger enhancement when feedback is active. To address the concern directly, we will add an inset or supplementary panel quantifying the pre- versus post-merger accretion-rate ratio (averaged over 10 Myr windows) and will update the abstract to reference these figures explicitly. revision: yes

  2. Referee: [Methods (feedback prescriptions)] Methods (feedback prescriptions): The conclusion relies on the specific choices for radiative and kinetic feedback efficiencies in the SE regime. No section quantifies the sensitivity of the results to plausible variations in these parameters (e.g., wind coupling or jet efficiency) for 10^9 M_sun halos at z~11, which is a load-bearing assumption given the limited observational constraints at these redshifts.

    Authors: The efficiencies adopted are standard values drawn from the high-redshift simulation literature (cited in the Methods). We acknowledge that a systematic sensitivity study would be desirable. We will add a dedicated paragraph discussing the impact of plausible variations (within a factor of two) and note that the qualitative result—kinetic feedback as the dominant suppressor—remains unchanged. A full parameter exploration lies beyond the scope of the present work but is flagged as important future work. revision: partial

  3. Referee: [Simulation setup] Simulation setup: No resolution tests, convergence checks, or comparisons with lower-resolution runs are reported, which is essential for validating the gas inflow and accretion dynamics in zoom-in simulations of this type.

    Authors: The adopted gas mass resolution (~10^4 M_⊙) is among the highest used for z~11 zoom-ins. Dedicated convergence tests for this exact merger were not performed owing to computational cost. We will insert a new Methods paragraph that (i) states the resolution explicitly, (ii) notes consistency with our prior lower-resolution runs on analogous systems, and (iii) cites convergence studies from related high-z zoom-in literature to support the adopted resolution. revision: yes

Circularity Check

0 steps flagged

No circularity: simulation outcomes follow from sub-grid prescriptions without reduction to fitted inputs or self-citations

full rationale

The paper reports results from cosmological zoom-in simulations exploring BH seeding and feedback across ADAF/sub-Eddington/SE regimes. The central finding—that mergers do not trigger sustained SE accretion except when feedback is switched off—emerges directly from the simulation runs under the stated models. No equations or claims reduce a prediction to a parameter fitted from the target result itself, nor does any load-bearing step rely on a self-citation chain that is unverified or self-referential by construction. Model dependence on feedback efficiency is acknowledged as an assumption but does not constitute circularity per the defined patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract supplies no explicit list of fitted parameters or background assumptions; feedback efficiencies and seeding masses are implicitly present but not quantified.

pith-pipeline@v0.9.1-grok · 5854 in / 978 out tokens · 21676 ms · 2026-06-28T08:56:18.111931+00:00 · methodology

discussion (0)

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Reference graph

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