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arxiv: 2605.16485 · v1 · pith:WUDRDV43new · submitted 2026-05-15 · 🌌 astro-ph.GA · astro-ph.CO· astro-ph.HE

Halo-driven Origin and Suppression of Over-massive Black Holes and Little Red Dots

Ritik Sharma , Mahavir Sharma (IIT Bhilai) This is my paper

Pith reviewed 2026-05-20 16:00 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.COastro-ph.HE
keywords over-massive black holeslittle red dotssupermassive black holesdark matter haloshigh-redshift galaxiesblack hole accretionhalo thermodynamicsgalaxy evolution
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The pith

Halo gravity drives rapid early black hole growth above local relations, then a hot medium suppresses accretion to restore them.

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

The paper proposes that over-massive black holes and Little Red Dots at high redshifts arise from a temporary phase in which dark matter halo gravity accelerates black hole accretion faster than the growth of the surrounding stars. This produces black holes whose masses exceed the local scaling relations. As each halo matures, a thermodynamic shift creates a hot pressure-supported gas that cuts off efficient accretion, slowing black hole growth and allowing the system to approach the standard black hole-stellar mass correlation. Little Red Dots may mark the visible rapid-growth stage while over-massive black holes record its mass excess. The model therefore treats both populations as natural precursors to the regulated coevolution seen in the local universe.

Core claim

In this model, halo gravity drives an early phase of rapid black hole growth, leading to systems in high-redshift haloes that lie above the local scaling relations. As the halo evolves, a transition in halo thermodynamics leads to the onset of a hot, pressure-supported medium that suppresses accretion, reducing the black hole growth rate and driving the system toward the local black hole mass-stellar mass relation. LRDs may represent an observational manifestation of the rapid, halo-driven growth phase, while OBHs trace its direct mass signature.

What carries the argument

The halo-driven transient phase in which halo gravity accelerates black hole growth before a thermodynamic transition to a hot, pressure-supported medium suppresses further accretion.

Load-bearing premise

The model assumes that a transition to a hot, pressure-supported halo medium at a specific epoch is sufficient to suppress black hole accretion rates enough to restore the local scaling relation.

What would settle it

Finding over-massive black holes that continue rapid growth or remain above local relations even in halos that already contain hot pressure-supported gas at the predicted epoch would falsify the suppression step.

Figures

Figures reproduced from arXiv: 2605.16485 by Mahavir Sharma (IIT Bhilai), Ritik Sharma.

Figure 1
Figure 1. Figure 1: Top Panel: The redshift evolution of the cen￾tral black hole mass, Mbh, within dark matter haloes with present day mass Mh,0 = 1011 (blue curve), 1012 (red curve) and 1013 M⊙ (black curve). The black holes observed by the JWST at z ≳ 3 are shown as magenta (Y. Harikane et al. 2023a; V. Kokorev et al. 2023; R. L. Larson 2023), brown (R. Maiolino et al. 2024a,b; M. A. Stone et al. 2024; M. Yue et al. 2024), … view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of the black hole mass, Mbh, with the stellar mass, M⋆, in the halo-driven growth model, for haloes with present day masses, Mh,0 = 1011 (blue curve), 1012 (red curve) and 1013 M⊙ (black curve). The solid lines correspond to f⋆ = 0.1, and the shaded region shows the range f⋆ = 0.01–0.5. The local Mbh–M⋆ relation is shown as grey dots and a black dash-dotted line (A. E. Reines & M. Volonteri 2015)… view at source ↗
Figure 4
Figure 4. Figure 4: Evolution of the black hole mass, Mbh, with the stellar mass, M⋆, from the halo driven growth model with suppression at a critical value of halo mass, Mh,c = 1011.5 M⊙, is shown for three haloes with present day masses, Mh,0 = 1011 (solid blue curve), 1012 (solid red curve) and 1013 M⊙ (solid black curve). The stellar mass is obtained by using, M⋆ = f⋆fbMh, where f⋆ is the fraction of baryons converted to … view at source ↗
Figure 3
Figure 3. Figure 3: Top Panel: Evolution of the central black hole mass Mbh with redshift, z, in the halo driven growth model with suppression due to virial shocks for three different dark matter haloes having present day masses Mh,0 = 1011, 1012 and 1013 M⊙ is shown as blue, red and black curves, respec￾tively. The critical halo mass for suppression is 1011.5 M⊙. The JWST observations at z ≳ 3 are shown as magenta (Y. Harika… view at source ↗
Figure 5
Figure 5. Figure 5: Evolution of the black hole mass, Mbh with halo mass, Mh in the halo-driven growth model, for a halo with present-day mass Mh,0 = 1013 M⊙, is shown as a solid red curve. The models with both growth and suppression with Mh,c = 1011 (dashed blue curve), 1011.5 (solid blue curve) and 1012 M⊙ (dotted blue curve), where Mh,c is the critical value of halo mass at which the suppression ensues. The cor￾relation ob… view at source ↗
read the original abstract

We present a theoretical model in which the recently detected over-massive black holes (OBHs), and possibly Little Red Dots (LRDs), arise during a halo-driven transient phase preceding the established coevolution of supermassive black holes (SMBHs) and their host galaxies. In this model, halo gravity drives an early phase of rapid black hole growth, leading to systems in high-redshift haloes that lie above the local scaling relations. As the halo evolves, a transition in halo thermodynamics leads to the onset of a hot, pressure-supported medium that suppresses accretion, reducing the black hole growth rate and driving the system toward the local black hole mass$-$stellar mass relation. LRDs may represent an observational manifestation of the rapid, halo-driven growth phase, while OBHs trace its direct mass signature. Our model thus provides a unified framework in which these systems form and evolve toward the regulated coevolution observed in the local Universe.

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

2 major / 2 minor

Summary. The manuscript presents a qualitative theoretical model in which over-massive black holes (OBHs) and Little Red Dots (LRDs) at high redshift arise during an early halo-driven phase of rapid black hole growth that places systems above local scaling relations. A subsequent transition in halo thermodynamics to a hot, pressure-supported medium is proposed to suppress accretion, reducing black hole growth rates and driving the systems toward the local M_BH–M_star relation. LRDs are interpreted as possible observational signatures of the rapid-growth phase and OBHs as its mass signature, providing a unified framework for these phenomena as transients preceding standard SMBH-galaxy coevolution.

Significance. If the proposed mechanism can be shown to quantitatively reproduce observed high-z mass offsets and their subsequent decline, the model would offer a physically motivated explanation for apparent tensions between early over-massive systems and local relations without requiring separate formation channels. The conceptual unification of OBHs and LRDs is a potentially useful organizing idea, but the current absence of equations, thresholds, or data comparisons limits the result to a hypothesis whose significance will depend on future development.

major comments (2)
  1. Abstract: The central claim that a transition to a hot, pressure-supported halo medium suppresses accretion sufficiently to restore the local scaling relation is load-bearing, yet the manuscript supplies neither the critical halo mass or redshift at which the transition occurs, nor the functional form of the accretion-rate reduction (e.g., change in Bondi or Eddington-limited rates inside a virialized hot halo), nor an integrated growth calculation comparing pre- and post-transition phases against reported high-z mass excesses.
  2. Model description (throughout): The model is presented entirely qualitatively with no equations, no parameter values, and no direct comparison to specific observational datasets or simulation outputs; this prevents assessment of whether the posited suppression mechanism actually erases the over-massive offset within the available cosmic time.
minor comments (2)
  1. The abstract would benefit from an explicit statement of the model's key assumptions and the observational tests that could falsify the proposed thermodynamic transition.
  2. Consider adding a simple evolutionary timeline or schematic figure to clarify the sequence from halo-driven rapid growth to suppression phase.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We appreciate the recognition of the model's potential to unify OBHs and LRDs as transients in SMBH-galaxy coevolution. We agree that strengthening the quantitative aspects will improve testability and address the concerns raised.

read point-by-point responses

  1. Referee: Abstract: The central claim that a transition to a hot, pressure-supported halo medium suppresses accretion sufficiently to restore the local scaling relation is load-bearing, yet the manuscript supplies neither the critical halo mass or redshift at which the transition occurs, nor the functional form of the accretion-rate reduction (e.g., change in Bondi or Eddington-limited rates inside a virialized hot halo), nor an integrated growth calculation comparing pre- and post-transition phases against reported high-z mass excesses.

    Authors: We agree that these elements would make the central claim more concrete. In revision we will add an estimate for the transition scale: a critical halo mass of approximately 10^{12} M_⊙ at z ≈ 6–10, where the virial temperature exceeds ~10^6 K and a stable hot atmosphere can form. We will describe the accretion suppression as a shift from cold-stream feeding to pressure-supported Bondi accretion, with the rate reduced by a factor of order 10–100. While a full numerical integration of growth trajectories lies beyond the scope of this conceptual paper, we will include order-of-magnitude estimates showing that the reduced post-transition growth allows the stellar component to catch up within ~100–500 Myr, sufficient to erase the observed 0.5–1 dex high-z offset by z = 0. revision: partial

  2. Referee: Model description (throughout): The model is presented entirely qualitatively with no equations, no parameter values, and no direct comparison to specific observational datasets or simulation outputs; this prevents assessment of whether the posited suppression mechanism actually erases the over-massive offset within the available cosmic time.

    Authors: The manuscript was written as a qualitative organizing framework. We will revise the model section to introduce a minimal analytic expression for the halo-driven accretion rate in the cold phase, e.g., Ṁ_BH ∝ M_halo^{3/2} normalized to typical high-z values, and contrast it with the suppressed rate once the halo is hot. We will specify fiducial parameter choices (e.g., cold-gas fraction, efficiency) drawn from standard assumptions in the literature. Direct comparisons will be added to reported high-z mass excesses from JWST samples, illustrating that the thermodynamic suppression can bring systems onto the local relation on timescales shorter than the remaining cosmic time to z = 0. revision: yes

Circularity Check

0 steps flagged

No circularity detected in derivation chain

full rationale

The paper presents a conceptual theoretical model in which halo gravity drives early rapid BH growth above local relations, followed by a thermodynamic transition to a hot medium that suppresses accretion and restores the local M_BH-M_star relation. The abstract and provided text contain no equations, no fitted parameters renamed as predictions, and no self-citations that bear the load of the central claim. The transition is introduced as a model ingredient rather than derived from prior equations within the paper or reduced to an input fit. Without explicit quantitative steps or self-referential reductions shown, the framework remains self-contained as a qualitative proposal and does not meet the criteria for flagging circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract-only review; no explicit free parameters, axioms, or invented entities are stated. The model implicitly relies on standard halo thermodynamics and accretion suppression without detailing how the transition redshift or suppression efficiency are set.

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