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REVIEW 2 major objections 7 minor 109 references

A black hole’s place in the mass and accretion planes is a fossil record of how it grew and what its host did.

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2026-07-10 17:58 UTC pith:XVP362FK

load-bearing objection Clean evolutionary map of massive BHs by tracking the BHs themselves; the four-channel picture is solid and useful, with only the usual sub-grid caveats. the 2 major comments →

arxiv 2607.07793 v1 pith:XVP362FK submitted 2026-07-08 astro-ph.GA

Tracing black hole and galaxy growth across environments since cosmic noon

Emma Jane Weller , Priyamvada Natarajan , Colin J. Burke , Shashank Dattathri This is my paper
classification astro-ph.GA
keywords supermassive black holesgalaxy evolutionscaling relationshydrodynamical simulationswandering black holesAGN feedbackM_BH-M_star relation
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper tracks massive black holes themselves—not just their original host galaxies—from cosmic noon (z=2) to z=0.5 in two large cosmological simulations. Central black holes stick to a tight, nearly unchanging relation between black-hole mass and host stellar mass that already looks like the local empirical relation and matches variable AGN at similar redshifts. Systems that leave that relation do so for identifiable reasons: major mergers that build the heaviest black holes and then quench their galaxies via kinetic feedback; tidal stripping that leaves overmassive black holes in gas-poor satellites; and, in one simulation, inefficient dynamical friction that leaves undermassive wandering black holes with almost no further growth. Those same populations also sit in characteristic corners of the specific black-hole accretion rate versus specific star-formation rate plane. The result is a practical claim: where a black hole sits in these two planes today tells you which dynamical, accretion, and feedback path it followed.

Core claim

Central black holes in both ASTRID and TNG300 evolve along a relatively tight, nearly redshift-invariant black-hole mass–stellar mass relation that is broadly consistent with local empirical constraints and with variable AGN at comparable redshifts. Departures from that relation map onto distinct evolutionary channels—merger-built high-mass centrals that quench their hosts, tidally stripped overmassive satellites, and (in ASTRID) undermassive wanderers—so that a black hole’s location in the mass and specific-accretion planes is a fossil record of its history.

What carries the argument

Tracking individual black holes (rather than fixed host galaxies) through the M_BH–M_★ and sBHAR–sSFR planes across 5.3 Gyr, which isolates centrals, stripped satellites, and wanderers and links each population to a concrete growth and feedback channel.

Load-bearing premise

The result rests on the simulations’ sub-grid choices for seeding, black-hole dynamics (or repositioning), accretion, and the switch into kinetic AGN feedback being realistic enough that the tight relation and the distinct off-relation channels are not artifacts of those recipes.

What would settle it

A statistically complete census of black-hole mass, host stellar mass, and accretion state at intermediate redshifts that finds either a strongly evolving central M_BH–M_★ relation or no overmassive stripped and undermassive wandering populations where the simulations predict them.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 7 minor

Summary. The paper tracks massive black holes (rather than their original host galaxies) from z=2 to z=0.5 in the ASTRID and TNG300 cosmological simulations, spanning 5.3 Gyr. By following the BHs themselves, the authors capture central BHs, BHs in satellites, and (in ASTRID) off-nuclear wanderers. They report that central BHs in both simulations evolve along a relatively tight, nearly redshift-invariant M_BH–M_⋆ relation that is broadly consistent with the local KH13 relation and with variable-AGN samples at comparable redshifts (Burke+24; Liu+25). Departures from this relation map distinct channels: merger-built high-mass centrals that quench via AGN kinetic feedback; tidally stripped satellites that become overmassive at fixed M_BH; and ASTRID wanderers that are undermassive relative to their new hosts and accrete little. These populations occupy characteristic regions of both the M_BH–M_⋆ and sBHAR–sSFR planes, which the authors interpret as a fossil record of dynamical, accretion, and feedback history.

Significance. If the evolutionary-map interpretation holds, the work provides a useful organizing framework for reading BH–galaxy scaling relations at intermediate redshift: location in the M_BH–M_⋆ and sBHAR–sSFR planes encodes not only integrated growth but also environment and dynamical history. The dual-simulation design is a genuine strength—ASTRID and TNG differ in seeding, BH dynamics (subgrid dynamical friction vs. repositioning), and kinetic-feedback thresholds, yet both produce a tight central relation and a high-mass quenching channel, while wanderers and stripped satellites appear only where the dynamics allow them. External anchors (KH13; Burke+24; Liu+25) and the explicit side-by-side comparison of known model choices strengthen the claim relative to single-simulation studies. The approach of following BHs rather than host galaxies is a clear methodological contribution for late-time assembly studies.

major comments (2)
  1. [Section 3 / Figure 3] Sec. 3 and Fig. 3: The authors correctly note that TNG merger catalogs are incomplete and that merger-driven mass growth for TNG BHs may be underestimated. However, the quantitative claims that high-mass TNG BHs grow almost entirely via mergers (mean fractions 89% at 1<z<2 and 82% at 0.5<z<1 for M_BH>10^9 M_⊙) are load-bearing for the “high-mass centrals” channel in TNG. The paper should either quantify the incompleteness (e.g., fraction of untraceable BHs as a function of mass, or a lower-limit vs. upper-limit estimate) or demonstrate that the qualitative conclusion—merger dominance at the high-mass end relative to accretion—survives plausible missing-merger corrections. Without that, the TNG side of Fig. 3 remains hard to interpret at face value.
  2. [Section 5 / Figure 7] Sec. 4.1 and Sec. 5 / Fig. 7: The comparison to the KH13 local relation is central to the claim of consistency with empirical constraints, yet KH13 uses bulge stellar mass while the simulations use stellar mass within twice the stellar half-mass radius. The manuscript notes this once but does not assess the systematic offset. Because bulge-to-total ratios vary with mass and morphology, this choice can shift the simulated relation relative to KH13 by amounts comparable to the reported residual offsets (especially at the low-mass end where ASTRID already differs). A brief estimate of the expected bias, or a restricted comparison at high mass where bulges dominate, would make the “broadly consistent” claim more secure.
minor comments (7)
  1. [Section 3] Sec. 3: The TNG sample drops from 10 000 to 4146 BHs by z=0.5, largely due to merger-catalog incompleteness and the isolation/zero-stellar-mass cuts. A short table or sentence giving the breakdown of attrition reasons (untraceable, merged duplicates dropped, isolated, M_⋆=0) would help readers judge residual selection bias.
  2. [Section 4.1] Sec. 4.1: The operational definition of “centrals” vs. “wanderers” shifts between the 3σ contour of the typical z=0.5 relation (used in Sec. 4) and the stricter R_BH < 3 h^{-1} ckpc cut (used in Sec. 5). Stating both cuts once in a single paragraph and noting how many objects change classification would reduce ambiguity.
  3. [Figure 1] Fig. 1 and related maps: The color scale is normalized jointly across both simulations and all redshifts. That choice aids comparison but can compress dynamic range within a single panel. Consider noting in the caption when a panel’s median values sit near the floor or ceiling of the shared scale.
  4. [Figure 4] Fig. 4 vs. Terrazas+17: The comparison mixes z=0.5 primaries+satellites with z∼0 central galaxies. The text already flags this; a one-sentence reminder in the figure caption would help casual readers.
  5. [Section 2] Sec. 2.1–2.2: The kinetic-feedback parameter differences (M_crit, χ_cap, redshift cut, coupling efficiencies) are listed but not tabulated. A compact parameter table would make the cross-code comparison easier to follow.
  6. [Abstract / Section 6] Abstract and Sec. 6: The phrase “fossil record” is effective but slightly strong given that the mapping is demonstrated only within these two subgrid models. Softening to “encodes” or “retains memory of” (as already used elsewhere) would better match the evidence presented.
  7. [Appendix A] Appendix A / Fig. 9: Halo mass distributions are useful context; a brief note on why ASTRID hosts sit in more massive halos at fixed galaxy M_⋆ (more galaxies per halo) is already in the text—consider moving one sentence of that explanation into the figure caption.

Circularity Check

0 steps flagged

No significant circularity: M_BH–M_⋆ tracks and fossil-record interpretation are measured simulation outputs, externally benchmarked.

full rationale

The paper’s central claims are empirical measurements from ASTRID and TNG300: central BHs track a tight, nearly redshift-invariant M_BH–M_⋆ relation (Figs. 1, 7), high-mass centrals grow by mergers then quench via kinetic feedback (Figs. 3–4), tidal stripping produces overmassive satellites, and ASTRID wanderers are undermassive with low accretion (Figs. 1–2, 5–6). These are direct outputs of the sub-grid models, not quantities fitted to the target relation or defined in terms of it. External anchors (KH13 local relation; Burke+24 and Liu+25 variable AGN) supply independent benchmarks. Self-citations (simulation method papers, Dattathri+25 for sBHAR–sSFR quadrants) define the codes or supply interpretive scaffolding; they do not force the measured tracks or the fossil-record claim by construction. Incomplete TNG merger trees are acknowledged and do not close a circular loop. No self-definitional step, fitted-input-as-prediction, uniqueness import, or renaming of a known result is present.

Axiom & Free-Parameter Ledger

3 free parameters · 3 axioms · 0 invented entities

The central claim rests on the fidelity of two existing cosmological simulations whose sub-grid parameters were fixed in earlier papers; no new free parameters are fitted here. Domain assumptions are standard ΛCDM plus the usual SUBFIND/FOF halo finders. No new physical entities are postulated.

free parameters (3)
  • ASTRID BH seed mass power-law index and range
    n = −1, 3×10^4–3×10^5 h^−1 M_⊙ (Sec. 2.1); fixed by prior ASTRID papers, not re-tuned here, but the low-mass end of the relation is sensitive to it.
  • TNG BH seed mass
    Fixed at 8×10^5 h^−1 M_⊙ (Sec. 2.2); higher than ASTRID and affects the low-mass comparison.
  • Kinetic-feedback thresholds (M_crit, χ_cap, redshift cut)
    Different values in ASTRID vs TNG control when high-mass BHs quench; the paper treats them as given model choices.
axioms (3)
  • domain assumption Bondi-like accretion plus the thermal/kinetic feedback switch correctly captures the net growth and quenching of massive BHs after z=2.
    Invoked throughout Secs. 2 and 4; the fossil-record claim collapses if the feedback modes are badly mis-calibrated.
  • domain assumption SUBFIND subhalos and the twice-half-mass-radius aperture give a meaningful stellar mass for both centrals and satellites.
    Used for every M_⋆ measurement (Sec. 3); tidal-stripping tracks depend on this definition.
  • ad hoc to paper Gaussian KDE contours of the z=0.5 ‘typical’ relation correctly separate centrals from wanderers.
    The 3σ contour is adopted as the operational boundary (Sec. 4.1); a different density estimator would move a few objects between categories.

pith-pipeline@v1.1.0-grok45 · 26675 in / 2824 out tokens · 29586 ms · 2026-07-10T17:58:50.180650+00:00 · methodology

0 comments
read the original abstract

The distribution of systems in the black hole mass-stellar mass ($M_\mathrm{BH}-M_\star$) plane encodes not only the integrated growth of galaxies and their central black holes (BHs), but also the processes that shape their evolution. Using the ASTRID and TNG300 cosmological simulations, we track massive BHs from cosmic noon ($z=2$) to $z=0.5$, spanning 5.3 Gyr of assembly. Unlike most previous studies, we follow the BHs themselves rather than their original host galaxies, thereby capturing central BHs, BHs in satellites, and off-nuclear wandering BHs. We find that central BHs in both simulations evolve along a relatively tight, nearly redshift-invariant $M_\mathrm{BH}-M_\star$ relation that is broadly consistent with local empirical constraints and with measurements from variable active galactic nuclei (AGN) at comparable redshifts. Departures from this relation trace distinct evolutionary channels. High-mass central BHs grow substantially through mergers and subsequently quench their hosts through AGN kinetic feedback. Tidal stripping moves satellites to lower $M_\star$ at nearly fixed $M_\mathrm{BH}$, producing weakly accreting, overmassive central BHs in gas-poor systems. In ASTRID, satellite accretion and inefficient dynamical friction generate wandering BHs that are undermassive relative to their new hosts and experience minimal accretion or merger-driven growth. These populations occupy characteristic regions in both the $M_\mathrm{BH}-M_\star$ and the specific BH accretion rate-specific star formation rate planes, demonstrating that a BH's location in these planes is a fossil record of its dynamical, accretion, and feedback history.

Figures

Figures reproduced from arXiv: 2607.07793 by Colin J. Burke, Emma Jane Weller, Priyamvada Natarajan, Shashank Dattathri.

Figure 1
Figure 1. Figure 1: Binned MBH − M⋆ maps for our BH sample, with each bin colored by the median value of log10 (RBH/R⋆), where RBH is a BH’s distance from the center of its host galaxy and R⋆ is the galaxy’s stellar half-mass radius. Panels are separated by simulation, redshift, and host galaxy type. We also plot 1σ, 2σ, and 3σ contours of the typical z = 0.5 MBH − M⋆ relation in the simulations. For comparison, we add the lo… view at source ↗
Figure 2
Figure 2. Figure 2: MBH vs. M⋆ evolution of subsets of our BH sample. In each simulation, we randomly select 100 BHs that begin in a primary galaxy at z = 2 and remain in a primary at z = 0.5, 100 that begin in a primary and end up in a satellite, and so on. We locate each BH at z = 2, 1, 0.5 and plot its track between these three snapshots. Most central BHs move upwards along the typical MBH − M⋆ relation. Interactions and e… view at source ↗
Figure 3
Figure 3. Figure 3: Binned MBH − M⋆ maps for our BH sample at z = 1 and z = 0.5, with each bin colored by the median value of log10 (∆MBH,m/∆MBH,tot), where ∆MBH,tot is a BH’s total mass gain since the previous snapshot (z = 2 or z = 1), and ∆MBH,m is the amount that came from mergers. BHs with ∆MBH,m = 0 are set to ∆MBH,m/∆MBH,tot = 10−5 for visualization. In TNG, the higher-mass BHs grow almost entirely via mergers, and the… view at source ↗
Figure 4
Figure 4. Figure 4: Binned MBH − M⋆ maps for our BH sample, with each bin colored by the median value of log10 (sSFR/yr−1 ), where sSFR = SFR/M⋆ is the specific star formation rate of a BH’s host galaxy. Galaxies with sSFR = 0 are set to sSFR = 10−15 yr−1 for visualization. Panels are separated by simulation and redshift. The most massive galaxies and the stripped satellites have minimal star formation due to loss of cold gas… view at source ↗
Figure 5
Figure 5. Figure 5: sBHAR vs. sSFR scatterplots for our BH sample, with each point colored according to the BH’s mass. Panels are separated by simulation, redshift, and host galaxy type. The orange dashed lines roughly divide the plane into four quadrants: active+quiescent, active+star-forming, inactive+star-forming, and inactive+quiescent. Galaxies with sSFR = 0 are set to sSFR = 10−14.5 yr−1 for visualization. Most points b… view at source ↗
Figure 6
Figure 6. Figure 6: Evolution in the sBHAR−sSFR plane for the same subsets of our BH sample used in [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Schematic showing four regions of MBH − M⋆ space and the distinct evolutionary paths that build them, as summarized in Sec. 6. their host halos or galaxies, and trace individual BHs through cosmic time as they accrete, merge, and inter￾act with their changing environments. In addition to central BHs in primary galaxies, we follow wanderers and BHs in satellites. This approach provides a more comprehensive … view at source ↗
Figure 7
Figure 7. Figure 7: Median MBH − M⋆ relation for the central BHs in our sample, separated by simulation, redshift, and host galaxy type. The local (z ∼ 0) empirical relation from KH13 is shown for comparison. Both simulations match KH13 rea￾sonably well, especially at higher masses. TNG is closer at the low-mass end. The median relation in the simulations shows minimal redshift evolution, and is relatively close to the empiri… view at source ↗
Figure 9
Figure 9. Figure 9: Mass distributions for the halos containing the host galaxies of our BH sample, separated by simulation, redshift, and host galaxy type. The halo masses are generally lower for primaries than for satellites, and lower in TNG than in ASTRID. B. SUPPLEMENTAL MBH − M⋆ MAPS Figs. 10 and 11 are binned MBH − M⋆ maps like those shown in Figs. 1, 3, and 4. They provide further support for the findings discussed in… view at source ↗
Figure 10
Figure 10. Figure 10: Binned MBH − M⋆ maps at z = 1 and z = 0.5, with each bin colored by the fraction of its BHs that were hosted by a primary galaxy at the previous snapshot (z = 2 or z = 1, respectively). Most stripped satellites have been satellites since z = 2, and most wanderers originated in satellites at z = 2. The most massive central BHs in primaries tend to experience mergers with BHs from satellites. Davis, M., Efs… view at source ↗
Figure 11
Figure 11. Figure 11: Binned MBH − M⋆ maps for our BH sample, with each bin colored by the median value of log10 (fEdd), where fEdd = M˙ BH/M˙ Edd is a BH’s Eddington ratio. Panels are separated by simulation and redshift. The most massive galaxies and the stripped satellites have low BH accretion rates due to the removal of gas by AGN feedback and tidal stripping, respectively. The wandering BHs have minimal accretion due to … view at source ↗

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