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Signatures of black hole seeding in the local Universe: Predictions from the BRAHMA cosmological simulations

T0 review · 3 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read The imprint of black hole seeding survives in local low-mass black holes inside dwarf galaxies, according to five simulations that differ only in how the seeds form.

desk verdict Controlled BRAHMA seeding comparison makes a plausible but dynamics-dependent case that local dwarf BHs can discriminate seed models. read the letter →

arxiv 2411.19332 v1 pith:BNMCNE5G submitted 2024-11-28 astro-ph.GA

Aklant K Bhowmick , Laura Blecha , Paul Torrey , Rachel S Somerville , Luke Zoltan Kelley , Rainer Weinberger , Mark Vogelsberger , Lars Hernquist
show 3 more authors
Priyamvada Natarajan Jonathan Kho Tiziana Di Matteo
This is my paper · ORCID
classification astro-ph.GA
keywords blackholeseedingintermediate-massholesdwarfgalaxiescosmologicalsimulationsmergersoccupationfractionmassfunctiondirectcollapse
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper tries to establish that the very first seeds of supermassive black holes leave measurable traces in the present-day Universe, specifically in black holes of roughly $10^5$ to $10^6\,M_\odot$ hosted by dwarf galaxies with stellar masses below $10^9\,M_\odot$. Five simulations of an $18\,\mathrm{Mpc}$ cube, identical except for the black hole seeding prescription, produce a local population of low-mass black holes that are either ungrown relics of seeds formed at $z\sim5$–$10$ or systems whose growth to $\sim10^6\,M_\odot$ is dominated by mergers all the way to $z=0$. Because gas accretion, which erases seed-model differences, only becomes the main growth channel above $\sim10^7\,M_\odot$, the seeding signatures survive exactly in the mass range that local dwarf-galaxy surveys can target. If the prediction holds, counting these black holes and measuring how often dwarf galaxies host them can discriminate between competing seeding models.

What carries the argument

The carrying mechanism is the split between two growth channels: black hole mergers versus gas accretion. The paper isolates this split by comparing five simulation boxes that share every aspect of the galaxy formation model except seeding: four 'direct heavy seed' models, which plant $1.5\times10^5\,M_\odot$ black holes in gas that is dense and metal-poor and then progressively add conditions (Lyman-Werner radiation, low gas spin, rich environment), and one 'extrapolated seed descendant' model, which plants the same initial mass as a stand-in for the higher-mass descendants of unresolved $\sim10^3\,M_\odot$ seeds. The merging fraction of the accumulated mass stays near unity for $10^5$–$10^6\,M_\odot$ black holes down to $z=0$, and a substantial population of seeds formed at $z\sim5$–$10$ never grows at all; those two facts are what keep seeding differences visible in the local low-mass population.

What would settle it

A complete local census of dwarf galaxies that measures the occupation fraction of $\gtrsim10^6\,M_\odot$ black holes in $M_*\sim10^9\,M_\odot$ galaxies would settle it: if the measured fraction falls below the lowest predicted value of about $20\%$ and the local black hole mass function shows no steepening at $10^5$–$10^6\,M_\odot$, the predicted population of ungrown relics and merger-grown low-mass black holes would be absent.

Watch

Extended reading notes

Core claim

On the paper's own terms, strong signatures of seeding survive in local $\sim10^5$–$10^6\,M_\odot$ black holes found in $M_*\lesssim10^9\,M_\odot$ dwarf galaxies. Two effects preserve the signal: many of the smallest local black holes are seeds from $z\sim5$–$10$ that have grown by less than about ten percent, and growth from $10^5$ to $10^6\,M_\odot$ is driven by black hole mergers rather than gas accretion all the way down to $z=0$. The seed models predict number densities of $\gtrsim10^5\,M_\odot$ black holes spanning $0.02$–$0.4\,\mathrm{Mpc}^{-3}$, number densities of $\gtrsim10^6\,M_\odot$ black holes of $0.01$–$0.05\,\mathrm{Mpc}^{-3}$, and occupation fractions of $\sim20$–$100\%$ in $M_*\sim10^9\,M_\odot$ galaxies. The variations weaken for more massive black holes and disappear above $\sim10^7\,M_\odot$, where accretion dominates; at $z\gtrsim5$, by contrast, the signatures persist up to $\sim10^8\,M_\odot$ because growth there is fully merger-dominated.

Load-bearing premise

The prediction assumes that low-mass black holes that grow by mergers actually meet and merge: the simulations park every black hole at the bottom of its galaxy's gravitational potential well and merge black holes as soon as they come close, so if wandering, slow dynamical friction, or gravitational recoil keeps many of them apart, the predicted low-mass populations and occupation fractions would be smaller and the seeding signatures weaker.

Editorial extensions

If this is right

  • Number densities of $\gtrsim10^5\,M_\odot$ local black holes are predicted to span $0.02$–$0.4\,\mathrm{Mpc}^{-3}$ across seed models, so a census at the low-mass end can discriminate seeding scenarios.
  • Occupation fractions in $M_*\sim10^9\,M_\odot$ galaxies range from $\sim40$–$100\%$ for $\gtrsim10^5\,M_\odot$ black holes and $\sim20$–$100\%$ for $\gtrsim10^6\,M_\odot$ black holes, giving a direct observable test.
  • The $z=0$ black hole mass function should be steeper at $10^5$–$10^6\,M_\odot$ than a Schechter extrapolation from higher masses; surveys that assume such an extrapolation will underestimate low-mass black hole abundances.
  • Faint local AGN with $L_{2-10\,\mathrm{keV}}\lesssim10^{39}\,\mathrm{erg\,s^{-1}}$, accessible to proposed X-ray instruments, are predicted to show strong seed-model variations, unlike high-redshift AGN luminosity functions.
  • The models that match observed high-redshift overmassive black hole scaling relations also match local black hole mass functions and dwarf-galaxy scaling relations, bracketing the viable range of seed formation efficiencies.

Reading between the lines

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

  • If the simulations' merger assumption overstates how often low-mass black holes coalesce, the predicted occupation fractions are upper limits, so a null detection in dwarf galaxies would tighten models of black hole dynamics as much as seeding.
  • The predicted steepening below $10^6\,M_\odot$ implies that extrapolating scaling-relation-based black hole mass functions into the dwarf regime could miss an entire population; targeted dwarf-galaxy surveys are the direct test.
  • Because the seed models differ most in the number of low-mass black holes available to merge, gravitational-wave event rates from $\sim10^5$–$10^6\,M_\odot$ black hole mergers should differ across models, providing an accretion-independent probe of seeding.
  • Both the low-mass-seed model and the intermediate heavy-seed models fit current data, so distinguishing them will likely require combining local occupation measurements with high-redshift number densities rather than relying on either epoch alone.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. This paper uses five [18 Mpc]^3 BRAHMA cosmological simulations run to z=0 with identical galaxy formation physics but different BH seeding models to predict local BH abundances, mass functions, AGN luminosity functions, scaling relations, and occupation fractions. The four 'DHS' models occupy heavy seeds with progressively stacked formation criteria, while the 'ESD' model initializes 1.5e5 M_sun BHs as extrapolated descendants of ~1e3 M_sun seeds using a stochastic model calibrated to high-resolution simulations. The central claim is that strong seeding signatures survive in ~1e5-1e6 M_sun local BHs hosted in M* < 1e9 M_sun dwarf galaxies, because these BHs are either ungrown relics of z~5-10 seeds or grow mainly by mergers to z=0. The predictions are compared with independent observational constraints from Shen et al. (2020), Merloni & Heinz (2008), Schutte et al. (2019), Greene et al. (2020), and others.

Significance. If the central claim survives scrutiny, the paper is a valuable contribution: it makes falsifiable, quantitative predictions for a local dwarf-galaxy BH population that upcoming facilities (AXIS, Athena) can test, and its five-box design isolates seeding from other galaxy-formation physics. The comparisons use published constraints rather than fitting to local BH data, and the paper is transparent about many caveats. The main limitation is that the size of the predicted signatures is controlled by an optimistic BH dynamics treatment, and the single realization per model leaves unknown cosmic variance; these issues currently limit how strongly the paper can claim to discriminate seed models.

major comments (3)
  1. [Section 2 (BH dynamics) and Section 4.2 (Caveats)] The claim that growth from ~1e5 to ~1e6 M_sun is merger-dominated to z=0 (Figure 6) is directly controlled by the repositioning/prompt-merging prescription, which the paper itself calls the 'most optimistic scenario' and acknowledges suppresses wandering and recoil. Because wandering or delayed mergers would shift growth to accretion (erasing seed signatures) or reduce the 1e6 M_sun abundance and occupation fractions, the z=0 merger fraction and the ~1e6 M_sun predictions (0.01-0.05 Mpc^-3; 20-100% occupation in Figure 9) are upper limits, not robust predictions. Please run or cite a sensitivity test with a sub-grid dynamical friction treatment, or explicitly re-frame the abstract's two-pillar claim as contingent on optimistic BH dynamics.
  2. [Sections 3.2-3.3 and start of Section 3] All quantitative predictions come from a single 18 Mpc box per model, so the quoted abundance ranges and occupation fractions carry no error bars. The paper's argument that the limited volume is not important uses agreement with TNG100 at >1e7 M_sun, but the low-mass dwarf regime that is the focus of the paper could be more sensitive to cosmic variance. Please provide quantitative estimates of sample variance (e.g., bootstrap sub-boxes, multiple realizations, or analytic cosmic-variance calculations) and state uncertainties on the z=0 BHMFs and occupation fractions.
  3. [Section 2.1.2 (ESD stochastic seed model)] The ESD model is calibrated using the high-resolution BRAHMA simulations of Bhowmick et al. (2024b), but the paper does not state whether those calibration runs employ the same BH repositioning and prompt-merger treatment as the present boxes. If they do, the ESD predictions inherit the same optimistic-dynamics assumption, and the 'broad agreement' of the ESD model with local observations (Section 4.1) cannot by itself establish the viability of ~1e3 M_sun seeds independent of BH dynamics. Please clarify this and, if the same treatment is used, soften the viability claim accordingly.
minor comments (5)
  1. [Section 4.1] The model name 'SM_LW10_LOWSPIN_SPIN' appears to be a typo; the intended model is likely SM5_LW10_LOWSPIN or SM5_LW10_LOWSPIN_RICH depending on the argument.
  2. [Section 3.6.1] The sentence 'Greene et al. (2020) inferred > 50% occupation fractions for ≳ 109 galaxies' is missing the stellar-mass unit; it should read 'for M* ≳ 10^9 M_sun galaxies'.
  3. [Section 1 (Introduction)] The phrase 'the subsequent the complex mass assembly history' contains a duplicated article and should be corrected to 'the subsequent complex mass assembly history'.
  4. [Figure 6] The artificial y-axis offsets used for the z=3 and z=5 curves are not quantified in the caption; please state the offsets or label the axes so that the reader can compare the curves across redshifts.
  5. [Section 2.1.1] The phrase 'a lenient threshold of 5 Mseed' is ambiguous because Mseed is a mass; please clarify explicitly that this means 5 times the seed mass (7.5e5 M_sun) of dense metal-poor gas.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the local BH predictions are self-consistent simulation outputs compared against independent observational constraints, and the main modeling assumptions are openly stated as caveats.

full rationale

The paper's central claim is that different BH seeding models produce distinguishable z=0 signatures in ~1e5-1e6 Msun BHs. This is a simulation result, not a fit to local observations: the BRAHMA boxes are evolved to z=0 with different seed prescriptions, and the predicted number densities, mass functions, scaling relations, and occupation fractions emerge from the simulations' accretion and merger dynamics. Comparisons are made against independent external data sets (Shen et al. 2020; Merloni & Heinz 2008; Schutte et al. 2019; Greene et al. 2020; Burke et al. 2024), so the predictions are not calibrated to the quantities they are used to interpret. The ESD stochastic seed model is calibrated to the authors' own higher-resolution simulations (Bhowmick et al. 2024a,b), including the 4x ESD mass addition for unresolved minor mergers, but this is a standard multi-scale subgrid calibration and is not fit to the local observables being predicted; moreover, the merger-dominated growth signature is also present in the DHS models that do not use this factor, so the central claim does not reduce to the ESD calibration. The most significant assumption, the repositioning/prompt-merging treatment of BH dynamics, is explicitly labeled in Section 4.2 as 'the most optimistic scenario for merger-driven BH growth' and is presented as a limitation rather than disguised as a prediction. No equation or fitted parameter is renamed as a prediction; the quoted 'predictions' are simulation outputs, and the paper's caveats about accretion, feedback, and dynamics acknowledge the model-dependence of the results. Therefore no circular step can be identified, and the appropriate score is 0.

Assumptions & free parameters 5 free parameters · 5 assumptions · 0 invented entities

All five models share the TNG galaxy formation backbone; the free parameters are seed thresholds and stochastic calibration constants, chosen or calibrated in earlier BRAHMA papers. There are no invented physical entities; ESDs are a numerical proxy rather than a new physical object. The main external anchors are published observational constraints, not fits.

free parameters (5)
  • Initial BH seed mass = 1.5e5 M_sun
    Chosen as the gas mass resolution scale for all five boxes; it sets the low-mass end of the BH mass function and the normalization of seed abundances. Not derived from first principles in this paper.
  • Dense metal-poor gas threshold = 5 M_seed
    Chosen leniently in Section 2.1.1 so that additional criteria still leave a usable seed population; variations across 5-150 M_seed change seed abundances by factors of roughly 10 in prior work.
  • Critical Lyman-Werner flux = 10 J21
    Adopted for SM5_LW10 and stricter models; canonical DCBH scenarios often require fluxes above 1000 J21, so this is a hand-picked model choice rather than an observed value.
  • Gas spin and environment criterion parameters = Toomre threshold; neighbor within 5 virial radii
    Restrict seeding in the third and fourth DHS boxes; motivated by Lodato & Natarajan 2006 and Wise et al. 2019 but not uniquely determined.
  • Stochastic ESD model calibration inputs = galaxy mass distribution, neighbor probability, 4x ESD mass per unresolved minor merger
    Calibrated to the authors' high-resolution BRAHMA-9-D3 simulations in Bhowmick et al. 2024a,b; these inputs control where and how often ESDs are placed.
assumptions (5)
  • domain assumption The IllustrisTNG galaxy formation model, inherited by BRAHMA, adequately captures star formation, metal enrichment, and feedback in dwarf galaxies.
    Invoked throughout Section 2; if stellar feedback or metal mixing is wrong, seed formation rates and accretion suppression change.
  • domain assumption Eddington-limited Bondi-Hoyle accretion with radiative efficiency 0.2 is a sufficient model for BH growth in these regimes.
    Eqs. 1-3; the paper notes magnetic fields can suppress Bondi rates by factors of about 100 (Cho et al. 2023), so this is a nontrivial assumption.
  • domain assumption Repositioning BHs to potential minima and merging when within the neighbor radius approximates unresolved BH dynamics.
    Section 2 and Section 4.2; this is the most optimistic merger scenario and directly supports the merger-dominated growth mechanism.
  • ad hoc to paper The seeding criteria map onto real Pop III, NSC, and DCBH formation channels.
    Section 2.1; these are modeling prescriptions rather than validated physical rate calculations.
  • domain assumption Missing large-scale modes and cosmic variance do not dominate the z=0 quantities of interest.
    Section 2 near the end; argued via agreement with TNG100 for >1e7 Msun BHs, but no formal error budget is provided.

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Pith. "Pith review of Signatures of black hole seeding in the local Universe: Predictions from the BRAHMA cosmological simulations." pith.science (2026). https://pith.science/paper/BNMCNE5G

@misc{pith2026241119332,
  author       = {Pith},
  title        = {Pith review of: Signatures of black hole seeding in the local Universe: Predictions from the BRAHMA cosmological simulations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/BNMCNE5G}},
  note         = {Machine review of arXiv:2411.19332}
}
abstract

The first "seeds" of supermassive black holes (BHs) continue to be an outstanding puzzle, and it is currently unclear whether the imprints of early seed formation survive today. Here we examine the signatures of seeding in the local Universe using five $[18~\mathrm{Mpc}]^3$ BRAHMA simulation boxes run to $z=0$. They initialize $1.5\times10^5~M_{\odot}$ BHs using different seeding models. The first four boxes initialize BHs as heavy seeds using criteria that depend on dense & metal-poor gas, Lyman-Werner radiation, gas spin, and environmental richness. The fifth box initializes BHs as descendants of lower mass seeds ($\sim10^3~M_{\odot}$) using a new stochastic seed model built in our previous work. We find that strong signatures of seeding survive in $\sim10^5-10^6~M_{\odot}$ local BHs hosted in $M_*\lesssim10^{9}~M_{\odot}$ dwarf galaxies. The signatures survive due to two reasons: 1) there is a substantial population of local $\sim10^5~M_{\odot}$ BHs that are ungrown relics of early seeds from $z\sim5-10$; 2) BH growth up to $\sim10^6~M_{\odot}$ is dominated by mergers all the way down to $z\sim0$. As the contribution from gas accretion increases, the signatures of seeding start to weaken in more massive $\gtrsim10^6~M_{\odot}$ BHs, and they eventually disappear for $\gtrsim10^7~M_{\odot}$ BHs. This is in contrast to high-z ($z\gtrsim5$) BH populations wherein the BH growth is fully merger dominated, which causes the seeding signatures to persist at least up to $\sim10^8~M_{\odot}$. The different seed models predict abundances of local $\sim10^6~M_{\odot}$ BHs ranging from $\sim0.01-0.05~\mathrm{Mpc}^{-3}$ with occupation fractions of $\sim20-100\%$ in $M_*\sim10^{9}~M_{\odot}$ galaxies. Our results highlight the potential for local $\sim10^5-10^6~M_{\odot}$ BH populations in dwarf galaxies to serve as a promising probe for BH seeding models.

Figures

Figures reproduced from arXiv: 2411.19332 by the authors.

Figure 1
Figure 1. Visualizations of the z = 0 universe in our [18 Mpc]3 simulation boxes that use the different seed models with an initial mass of 1.5 × 105 M⊙. The left side of the boxes shows the gas density profiles and the right side shows the gas metallicity profiles at z = 0, averaged over a 200 kpc thick slice along the line of sight coordinate. The top four boxes (SM5, SM5_LW10, SM5_LW10_LOWSPIN and SM5_LW10_LOWSPIN_RICH) sh… view at source ↗
Figure 3
Figure 3. For our four DHS models, we show the distribu￾tion (number density per unit redshift bin) of the formation red￾shifts of seeds that did not undergo any significant growth via accretion or mergers all the way down to z = 0. Specifically, we select seeds that only grew by ≲ 10 % of their initial mass. We find that in all four DHS models, most of these ungrown seeds were formed in the Universe between z ∼ 5 − 10. The c… view at source ↗
Figure 4
Figure 4. Comoving number density evolution of ≳ 105 and ≳ 106 M⊙ BHs are shown in the left and right panels respectively. Black data points show the local observational constraints from Merloni & Heinz (2008), Cao (2010) and Shen et al. (2020). The grey line shows the prediction from the TNG100 simulation. The z = 0 number densities exhibit significant seed model variations for both ≳ 105 and ≳ 106 M⊙ BHs [PITH_FULL_IMAGE:f… view at source ↗
Figures from the paper (5 more)
Figure 5
Figure 5. Figure 5: BH mass functions (solid lines) at z = 0 (left) and z = 5 (right) for the different seed models as compared to local observa￾tions (black data points) from Merloni & Heinz (2008), Cao (2010), Shen et al. (2020). At z = 5, we show the recent constraints from JWST BL-AGN…
Figure 6
Figure 6. Figure 6: The fraction of the accumulated BH mass that is contributed via mergers (rather than gas accretion) is plotted as a function of BH mass. The different colors show BH populations at z = 0, 3 & 5 snapshots. We added artificial y-axis offsets for z = 3 & 5 for clarity. At…
Figure 7
Figure 7. Figure 7: The top and bottom rows show the AGN bolometric and hard X-ray luminosity functions respectively, for the different seed models. The left three columns show different redshifts in the nearby Universe whereas the rightmost column shows the z = 5 prediction. The thin gre…
Figure 8
Figure 8. Figure 8: M∗ vs. Mbh relation predictions for our different BH seed models compared against different observational measurements. Specifically, we plot the total stellar mass of the subhalos versus the mass of central (most massive) BH. The four left panels show the DHS models. …
Figure 9
Figure 9. Figure 9: z = 0 occupation fractions predicted by the different seed models. The different panels correspond to BH samples with different mass thresholds. Seed model variations are substantial for ≳ 105 M⊙ and ≳ 106 M⊙ BHs. We compare our predictions with observational constrain…

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Forward citations

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