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arxiv: 2312.04085 · v3 · submitted 2023-12-07 · 🌌 astro-ph.GA · astro-ph.CO

Impact of primordial black holes on the formation of the first stars and galaxies

Boyuan Liu , Volker Bromm This is my paper

Pith reviewed 2026-05-24 04:53 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords primordial black holesfirst starsgalaxy formationearly universecosmological simulationsstructure formationblack hole feedbackhigh-redshift galaxies
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The pith

Stellar-mass primordial black holes have only minor effects on the formation of the first stars, while supermassive ones seed the early massive galaxies seen in recent data.

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

The paper investigates how primordial black holes could shape the earliest stars and galaxies through two opposing influences: they speed up the collapse of cosmic structures, yet their accretion also heats surrounding gas and may suppress star formation. Semi-analytical models combined with cosmological simulations show that stellar-mass black holes, at fractions allowed by current limits, produce only small changes to overall star formation rates even though they modify the density and temperature profiles of the first halos and clouds. Supermassive primordial black holes, by contrast, act as ready-made seeds that accelerate the growth of large structures, offering a possible account for the unexpectedly massive galaxies detected at high redshift.

Core claim

The impact of stellar-mass PBHs (allowed by existing observational constraints) on primordial star formation is likely minor, although they do alter the properties of the first star-forming halos/clouds and can potentially trigger the formation of massive BHs, while supermassive PBHs serve as seeds of massive structures that can explain the apparent overabundance of massive galaxies in recent observations.

What carries the argument

The competing effects of PBH-driven acceleration of structure formation and gas heating from BH accretion feedback, evaluated through semi-analytical analysis and cosmological simulations.

If this is right

  • Stellar-mass PBHs change the density and temperature profiles inside the first star-forming halos and clouds.
  • Stellar-mass PBHs can trigger the formation of additional massive black holes in the early universe.
  • Supermassive PBHs provide seeds that allow massive galactic structures to assemble earlier than in standard models.
  • Improved modeling of PBH, dark-matter, and baryon interactions is required to refine predictions for high-redshift observables.

Where Pith is reading between the lines

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

  • If the minor effect on star formation is confirmed, gravitational-wave signals from early black-hole mergers would need separate explanations beyond PBH-driven channels.
  • The same PBH populations that leave star formation largely unchanged could still leave distinct imprints in the 21-cm signal from the cosmic dawn epoch.
  • Future simulations that resolve individual PBH orbits inside minihalos could reveal whether rare close encounters produce observable star-formation bursts not captured in the averaged treatment.

Load-bearing premise

The semi-analytical analysis and cosmological simulations accurately capture the competing effects of structure acceleration and gas heating by BH accretion feedback without missing dominant interactions between PBHs, particle DM, and baryons.

What would settle it

High-redshift observations that measure the number density and star-formation rates of the earliest galaxies and compare them directly against simulation outputs run with and without the allowed PBH populations would test whether the minor-impact conclusion holds.

read the original abstract

Recent gravitational wave (GW) observations of binary black hole (BH) mergers and the stochastic GW background have triggered renewed interest in primordial black holes (PBHs) in the stellar-mass ($\sim 10 - 100\ \rm M_\odot$) and supermassive regimes ($\sim 10^7 - 10^{11}\ \rm M_\odot$). Although only a small fraction ($\lesssim 1\%$) of dark matter (DM) in the form of PBHs is required to explain such observations, these PBHs may play important roles in early structure/star/galaxy formation. In this chapter, we combine semi-analytical analysis and cosmological simulations to explore the possible impact of PBHs on the formation of the first stars and galaxies, taking into account two (competing) effects of PBHs: acceleration of structure formation and gas heating by BH accretion feedback. We find that the impact of stellar-mass PBHs (allowed by existing observational constraints) on primordial star formation is likely minor, although they do alter the properties of the first star-forming halos/clouds and can potentially trigger the formation of massive BHs, while supermassive PBHs serve as seeds of massive structures that can explain the apparent overabundance of massive galaxies in recent observations. Our tentative models and results call for future studies with improved modeling of the interactions between PBHs, particle DM, and baryons to better understand the impact of PBHs on early star/galaxy/structure formation and their imprints in high-redshift observations.

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 combines semi-analytical analysis and cosmological simulations to study the effects of primordial black holes (PBHs) on early star and galaxy formation. It accounts for two competing processes—acceleration of structure formation by PBHs and gas heating via BH accretion feedback—and concludes that stellar-mass PBHs (within observational bounds) have a minor overall impact on primordial star formation while altering the properties of the first halos/clouds and potentially triggering massive BH formation; supermassive PBHs are argued to act as seeds for massive structures that may explain the apparent excess of massive galaxies seen in recent observations. The models are presented as tentative and call for improved treatments of PBH–particle DM–baryon interactions.

Significance. If the quantitative results hold under improved modeling, the work provides a useful bridge between GW-motivated PBH scenarios and high-redshift structure formation, offering a possible resolution to tensions with JWST observations of early massive galaxies. The dual-method approach (semi-analytical plus simulations) is a positive feature, though the acknowledged need for future refinements limits immediate impact.

major comments (2)
  1. [Abstract] Abstract: the central claim that stellar-mass PBH impact on primordial star formation is 'likely minor' rests on the semi-analytical and simulation results accurately balancing structure acceleration against accretion feedback; however, the abstract itself states that the models are tentative and require 'improved modeling of the interactions between PBHs, particle DM, and baryons,' which directly affects whether the minor-impact conclusion is robust.
  2. [Abstract / Results summary] The manuscript does not provide quantitative error estimates or sensitivity tests showing how the 'minor' classification changes when additional PBH–DM–baryon coupling channels (explicitly flagged as missing) are included; without such tests the load-bearing distinction between 'minor' and 'significant' alteration of star-formation efficiency remains unquantified.
minor comments (2)
  1. [Abstract] The abstract refers to 'recent observations' of massive galaxies without citing specific surveys or redshift ranges; adding these references would improve traceability.
  2. [Abstract] Notation for PBH mass ranges (e.g., stellar-mass ~10–100 M_⊙) is clear, but the transition to supermassive regime (~10^7–10^11 M_⊙) would benefit from an explicit statement of the mass threshold separating the two regimes in the analysis.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive review and for recognizing the potential bridge our work provides between PBH scenarios and high-redshift observations. We address the two major comments below point by point.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that stellar-mass PBH impact on primordial star formation is 'likely minor' rests on the semi-analytical and simulation results accurately balancing structure acceleration against accretion feedback; however, the abstract itself states that the models are tentative and require 'improved modeling of the interactions between PBHs, particle DM, and baryons,' which directly affects whether the minor-impact conclusion is robust.

    Authors: The abstract is deliberately balanced: it reports the 'likely minor' net impact on star formation as the outcome of the modeled competition between accelerated structure formation and accretion feedback, while immediately qualifying the result as tentative and calling for improved PBH–DM–baryon modeling. This wording accurately reflects the scope of the present study; we do not assert robustness against every possible additional channel. The distinction between 'minor' and 'significant' therefore applies strictly within the physics we have included, consistent with the paper’s own caveats. revision: no

  2. Referee: [Abstract / Results summary] The manuscript does not provide quantitative error estimates or sensitivity tests showing how the 'minor' classification changes when additional PBH–DM–baryon coupling channels (explicitly flagged as missing) are included; without such tests the load-bearing distinction between 'minor' and 'significant' alteration of star-formation efficiency remains unquantified.

    Authors: We agree that explicit sensitivity tests for the missing coupling channels would strengthen the quantitative claim. Our current results quantify the balance only for the two processes we modeled (structure acceleration and accretion feedback). The manuscript already flags the need for future work on additional interactions; we can expand the discussion of associated uncertainties in a revised version. Full sensitivity tests, however, would require new simulations beyond the scope of this study. revision: partial

Circularity Check

0 steps flagged

No circularity in derivation chain

full rationale

The paper uses semi-analytical analysis and cosmological simulations to model two competing effects (structure acceleration and BH accretion feedback) on early star/galaxy formation. The conclusion that stellar-mass PBH impact is likely minor follows from these independent physical modeling steps rather than any self-definition, fitted parameter renamed as prediction, or load-bearing self-citation. No equations or steps in the abstract reduce outputs to inputs by construction, and the provided text shows no uniqueness theorems or ansatzes imported from prior author work. The derivation is self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Based solely on the abstract, the central claims rest on domain assumptions about PBH-DM-baryon interactions and the dominance of the two listed effects; no explicit free parameters or invented entities are named.

free parameters (1)
  • PBH mass and abundance fractions
    Different regimes (stellar-mass ~10-100 Msun and supermassive ~10^7-10^11 Msun) with abundance ≲1% of DM are used to explore impacts; values are constrained by observations but enter the models directly.
axioms (1)
  • domain assumption PBHs accelerate structure formation and heat gas via accretion feedback as the two competing dominant effects
    Explicitly stated in the abstract as the basis for the analysis.

pith-pipeline@v0.9.0 · 5806 in / 1489 out tokens · 24650 ms · 2026-05-24T04:53:40.641003+00:00 · methodology

discussion (0)

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Forward citations

Cited by 2 Pith papers

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  1. Possible evidence for a pair-instability supernova nature of ultra-early JWST sources

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    A pair-instability supernova from a 250-260 solar mass Population III star at z≈15 matches the brightness, variability, photometry, and spectrum of the JWST source Capotauro.

  2. Impact of Primordial Black Hole population on 21 cm observables at high redshift

    astro-ph.CO 2026-04 unverdicted novelty 5.0

    X-ray heating from primordial black holes assumed to seed high-redshift AGNs shallows the global 21-cm absorption signal and suppresses its power amplitude at cosmic dawn, with strong dependence on the PBH mass function.

Reference graph

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